Jump to content

Supernova

From Wikipedia, the free encyclopedia

SN 1994D (bright spot on the lower left), a type Ia supernova within its host galaxy, NGC 4526

A supernova (pl.: supernovae or supernovas) is a powerful and luminous explosion of a star. A supernova occurs during the last evolutionary stages of a massive star, or when a white dwarf is triggered into runaway nuclear fusion. The original object, called the progenitor, either collapses to a neutron star or black hole, or is completely destroyed to form a diffuse nebula. The peak optical luminosity of a supernova can be comparable to that of an entire galaxy before fading over several weeks or months.

The last supernova directly observed in the Milky Way was Kepler's Supernova in 1604, appearing not long after Tycho's Supernova in 1572, both of which were visible to the naked eye. The remnants of more recent supernovae have been found, and observations of supernovae in other galaxies suggest they occur in the Milky Way on average about three times every century. A supernova in the Milky Way would almost certainly be observable through modern astronomical telescopes. The most recent naked-eye supernova was SN 1987A, which was the explosion of a blue supergiant star in the Large Magellanic Cloud, a satellite galaxy of the Milky Way.

Theoretical studies indicate that most supernovae are triggered by one of two basic mechanisms: the sudden re-ignition of nuclear fusion in a white dwarf, or the sudden gravitational collapse of a massive star's core.

  • In the re-ignition of a white dwarf, the object's temperature is raised enough to trigger runaway nuclear fusion, completely disrupting the star. Possible causes are an accumulation of material from a binary companion through accretion, or by a stellar merger.
  • In the case of a massive star's sudden implosion, the core of a massive star will undergo sudden collapse once it is unable to produce sufficient energy from fusion to counteract the star's own gravity, which must happen once the star begins fusing iron, but may happen during an earlier stage of metal fusion.

Supernovae can expel several solar masses of material at speeds up to several percent of the speed of light. This drives an expanding shock wave into the surrounding interstellar medium, sweeping up an expanding shell of gas and dust observed as a supernova remnant. Supernovae are a major source of elements in the interstellar medium from oxygen to rubidium. The expanding shock waves of supernovae can trigger the formation of new stars. Supernovae are a major source of cosmic rays. They might also produce gravitational waves.

Etymology

[edit]

The word supernova has the plural form supernovae (/-v/) or supernovas and is often abbreviated as SN or SNe. It is derived from the Latin word nova, meaning 'new', which refers to what appears to be a temporary new bright star. Adding the prefix "super-" distinguishes supernovae from ordinary novae, which are far less luminous. The word supernova was coined by Walter Baade and Fritz Zwicky, who began using it in astrophysics lectures in 1931.[1][2] Its first use in a journal article came the following year in a publication by Knut Lundmark, who may have coined it independently.[2][3]

Observation history

[edit]

Compared to a star's entire history, the visual appearance of a supernova is very brief, sometimes spanning several months, so that the chances of observing one with the naked eye are roughly once in a lifetime. Only a tiny fraction of the 100 billion stars in a typical galaxy have the capacity to become a supernova, the ability being restricted to those having high mass and those in rare kinds of binary star systems with at least one white dwarf.[4]

Early discoveries

[edit]

The earliest record of a possible supernova, known as HB9, was likely viewed by an unknown prehistoric people of the Indian subcontinent and recorded on a rock carving in the Burzahama region of Kashmir, dated to 4500±1000 BC.[5] Later, SN 185 was documented by Chinese astronomers in 185 AD. The brightest recorded supernova was SN 1006, which was observed in AD 1006 in the constellation of Lupus. This event was described by observers in China, Japan, Iraq, Egypt and Europe.[6][7][8] The widely observed supernova SN 1054 produced the Crab Nebula.[9]

Supernovae SN 1572 and SN 1604, the latest Milky Way supernovae to be observed with the naked eye, had a notable influence on the development of astronomy in Europe because they were used to argue against the Aristotelian idea that the universe beyond the Moon and planets was static and unchanging.[10] Johannes Kepler began observing SN 1604 at its peak on 17 October 1604, and continued to make estimates of its brightness until it faded from naked eye view a year later.[11] It was the second supernova to be observed in a generation, after Tycho Brahe observed SN 1572 in Cassiopeia.[12]

There is some evidence that the youngest known supernova in our galaxy, G1.9+0.3, occurred in the late 19th century, considerably more recently than Cassiopeia A from around 1680.[13] Neither was noted at the time. In the case of G1.9+0.3, high extinction from dust along the plane of the galactic disk could have dimmed the event sufficiently for it to go unnoticed. The situation for Cassiopeia A is less clear; infrared light echoes have been detected showing that it was not in a region of especially high extinction.[14]

The Crab Nebula is a pulsar wind nebula associated with the 1054 supernova.
A 1414 text cites a 1055 report: since "the baleful star appeared, a full year has passed and until now its brilliance has not faded".[15]
Historical supernovae in the Local Group
year observed in maximum apparent brightness certainty[16] of the

SN's identification

185 constellation of Centaurus −6m possible SN, but may be a comet[17][18]
386 constellation of Sagittarius +1.5m[19] uncertain whether SN or classical nova[20]
393 constellation of Scorpius −3m possible SN[20]
1006 constellation of Lupus −7.5±0.4m[21] certain: SNR known
1054 constellation of Taurus −6m certain: SNR and pulsar known
1181 constellation of Cassiopeia −2m likely type Iax SN associated with the remnant Pa30[22]
1572 constellation of Cassiopeia −4m certain: SNR known
1604 constellation of Ophiuchus −2m certain: SNR known
1680? constellation of Cassiopeia +6m SNR known, unclear whether the SN was observed
1800–1900 constellation of Sagittarius ?m SNR known, but not observed
1885 Andromeda Galaxy +6m certain
1987 Large Magellanic Cloud +3m certain

Telescope findings

[edit]

With the development of the astronomical telescope, observation and discovery of fainter and more distant supernovae became possible. The first such observation was of SN 1885A in the Andromeda Galaxy. A second supernova, SN 1895B, was discovered in NGC 5253 a decade later.[23] Early work on what was originally believed to be simply a new category of novae was performed during the 1920s. These were variously called "upper-class Novae", "Hauptnovae", or "giant novae".[24] The name "supernovae" is thought to have been coined by Walter Baade and Zwicky in lectures at Caltech in 1931. It was used, as "super-Novae", in a journal paper published by Knut Lundmark in 1933,[25] and in a 1934 paper by Baade and Zwicky.[26] By 1938, the hyphen was no longer used and the modern name was in use.[27]

American astronomers Rudolph Minkowski and Fritz Zwicky developed the modern supernova classification scheme beginning in 1941.[28] During the 1960s, astronomers found that the maximum intensities of supernovae could be used as standard candles, hence indicators of astronomical distances.[29] Some of the most distant supernovae observed in 2003 appeared dimmer than expected. This supports the view that the expansion of the universe is accelerating.[30] Techniques were developed for reconstructing supernovae events that have no written records of being observed. The date of the Cassiopeia A supernova event was determined from light echoes off nebulae,[31] while the age of supernova remnant RX J0852.0-4622 was estimated from temperature measurements[32] and the gamma ray emissions from the radioactive decay of titanium-44.[33]

Jades Deep Field. A team of astronomers studying JADES data identified about 80 objects (circled in green) that changed in brightness over time. Most of these objects, known as transients, are the result of exploding stars or supernovae.[34]

The most luminous supernova ever recorded is ASASSN-15lh, at a distance of 3.82 gigalight-years. It was first detected in June 2015 and peaked at 570 billion L, which is twice the bolometric luminosity of any other known supernova.[35] The nature of this supernova is debated and several alternative explanations, such as tidal disruption of a star by a black hole, have been suggested.[36]

SN 2013fs was recorded three hours after the supernova event on 6 October 2013, by the Intermediate Palomar Transient Factory. This is among the earliest supernovae caught after detonation, and it is the earliest for which spectra have been obtained, beginning six hours after the actual explosion. The star is located in a spiral galaxy named NGC 7610, 160 million light-years away in the constellation of Pegasus.[37][38]

The supernova SN 2016gkg was detected by amateur astronomer Victor Buso from Rosario, Argentina, on 20 September 2016.[39][40] It was the first time that the initial "shock breakout" from an optical supernova had been observed.[39] The progenitor star has been identified in Hubble Space Telescope images from before its collapse. Astronomer Alex Filippenko noted: "Observations of stars in the first moments they begin exploding provide information that cannot be directly obtained in any other way."[39]

The James Webb Space Telescope (JWST) has significantly advanced our understanding of supernovae[41] by identifying around 80 new instances through its JWST Advanced Deep Extragalactic Survey (JADES) program. This includes the most distant spectroscopically confirmed supernova at a redshift of 3.6, indicating its explosion occurred when the universe was merely 1.8 billion years old. These findings[42] offer crucial insights into the early universe's stellar evolution and the frequency of supernovae during its formative years.

Discovery programs

[edit]
Supernova remnant SNR E0519-69.0 in the Large Magellanic Cloud

Because supernovae are relatively rare events within a galaxy, occurring about three times a century in the Milky Way,[43] obtaining a good sample of supernovae to study requires regular monitoring of many galaxies. Today, amateur and professional astronomers are finding several hundred every year, some when near maximum brightness, others on old astronomical photographs or plates. Supernovae in other galaxies cannot be predicted with any meaningful accuracy. Normally, when they are discovered, they are already in progress.[44] To use supernovae as standard candles for measuring distance, observation of their peak luminosity is required. It is therefore important to discover them well before they reach their maximum. Amateur astronomers, who greatly outnumber professional astronomers, have played an important role in finding supernovae, typically by looking at some of the closer galaxies through an optical telescope and comparing them to earlier photographs.[45]

Toward the end of the 20th century, astronomers increasingly turned to computer-controlled telescopes and CCDs for hunting supernovae. While such systems are popular with amateurs, there are also professional installations such as the Katzman Automatic Imaging Telescope.[46] The Supernova Early Warning System (SNEWS) project uses a network of neutrino detectors to give early warning of a supernova in the Milky Way galaxy.[47][48] Neutrinos are subatomic particles that are produced in great quantities by a supernova, and they are not significantly absorbed by the interstellar gas and dust of the galactic disk.[49]

"A star set to explode", the SBW1 nebula surrounds a massive blue supergiant in the Carina Nebula.

Supernova searches fall into two classes: those focused on relatively nearby events and those looking farther away. Because of the expansion of the universe, the distance to a remote object with a known emission spectrum can be estimated by measuring its Doppler shift (or redshift); on average, more-distant objects recede with greater velocity than those nearby, and so have a higher redshift. Thus the search is split between high redshift and low redshift, with the boundary falling around a redshift range of z=0.1–0.3, where z is a dimensionless measure of the spectrum's frequency shift.[50]

High redshift searches for supernovae usually involve the observation of supernova light curves. These are useful for standard or calibrated candles to generate Hubble diagrams and make cosmological predictions. Supernova spectroscopy, used to study the physics and environments of supernovae, is more practical at low than at high redshift.[51][52] Low redshift observations also anchor the low-distance end of the Hubble curve, which is a plot of distance versus redshift for visible galaxies.[53][54]

As survey programmes rapidly increase the number of detected supernovae, collated collections of observations (light decay curves, astrometry, pre-supernova observations, spectroscopy) have been assembled. The Pantheon data set, assembled in 2018, detailed 1048 supernovae.[55] In 2021, this data set was expanded to 1701 light curves for 1550 supernovae taken from 18 different surveys, a 50% increase in under 3 years.[56]

Naming convention

[edit]
Multi-wavelength X-ray, infrared, and optical compilation image of Kepler's supernova remnant, SN 1604

Supernova discoveries are reported to the International Astronomical Union's Central Bureau for Astronomical Telegrams, which sends out a circular with the name it assigns to that supernova.[57] The name is formed from the prefix SN, followed by the year of discovery, suffixed with a one or two-letter designation. The first 26 supernovae of the year are designated with a capital letter from A to Z. Next, pairs of lower-case letters are used: aa, ab, and so on. Hence, for example, SN 2003C designates the third supernova reported in the year 2003.[58] The last supernova of 2005, SN 2005nc, was the 367th (14 × 26 + 3 = 367). Since 2000, professional and amateur astronomers have been finding several hundred supernovae each year (572 in 2007, 261 in 2008, 390 in 2009; 231 in 2013).[59][60]

Historical supernovae are known simply by the year they occurred: SN 185, SN 1006, SN 1054, SN 1572 (called Tycho's Nova) and SN 1604 (Kepler's Star).[61] Since 1885 the additional letter notation has been used, even if there was only one supernova discovered that year (for example, SN 1885A, SN 1907A, etc.); this last happened with SN 1947A. SN, for SuperNova, is a standard prefix. Until 1987, two-letter designations were rarely needed; since 1988, they have been needed every year. Since 2016, the increasing number of discoveries has regularly led to the additional use of three-letter designations.[62] After zz comes aaa, then aab, aac, and so on. For example, the last supernova retained in the Asiago Supernova Catalogue  when it was terminated on 31 December 2017 bears the designation SN 2017jzp.[63]

Classification

[edit]

Astronomers classify supernovae according to their light curves and the absorption lines of different chemical elements that appear in their spectra. If a supernova's spectrum contains lines of hydrogen (known as the Balmer series in the visual portion of the spectrum) it is classified Type II; otherwise it is Type I. In each of these two types there are subdivisions according to the presence of lines from other elements or the shape of the light curve (a graph of the supernova's apparent magnitude as a function of time).[64][65]

Supernova taxonomy[64][65]
Type I
No hydrogen
Type Ia
Presents a singly ionised silicon (Si II) line at 615.0 nm (nanometers), near peak light
Thermal runaway
Type Ib/c
Weak or no silicon absorption feature
Type Ib
Shows a non-ionised helium (He I) line at 587.6 nm
Core collapse
Type Ic
Weak or no helium
Type II
Shows hydrogen
Type II-P/-L/n
Type II spectrum throughout
Type II-P/L
No narrow lines
Type II-P
Reaches a "plateau" in its light curve
Type II-L
Displays a "linear" decrease in its light curve (linear in magnitude versus time)[66]
Type IIn
Some narrow lines
Type IIb
Spectrum changes to become like Type Ib

Type I

[edit]
Light curve for type Ia SN 2018gv

Type I supernovae are subdivided on the basis of their spectra, with type Ia showing a strong ionised silicon absorption line. Type I supernovae without this strong line are classified as type Ib and Ic, with type Ib showing strong neutral helium lines and type Ic lacking them. Historically, the light curves of type I supernovae were seen as all broadly similar, too much so to make useful distinctions.[66] While variations in light curves have been studied, classification continues to be made on spectral grounds rather than light-curve shape.[65]

A small number of type Ia supernovae exhibit unusual features, such as non-standard luminosity or broadened light curves, and these are typically categorised by referring to the earliest example showing similar features. For example, the sub-luminous SN 2008ha is often referred to as SN 2002cx-like or class Ia-2002cx.[67]

A small proportion of type Ic supernovae show highly broadened and blended emission lines which are taken to indicate very high expansion velocities for the ejecta. These have been classified as type Ic-BL or Ic-bl.[68]

Calcium-rich supernovae are a rare type of very fast supernova with unusually strong calcium lines in their spectra.[69][70] Models suggest they occur when material is accreted from a helium-rich companion rather than a hydrogen-rich star. Because of helium lines in their spectra, they can resemble type Ib supernovae, but are thought to have very different progenitors.[71]

Type II

[edit]
Light curves are used to classify type II-P and type II-L supernovae.[65][72]

The supernovae of type II can also be sub-divided based on their spectra. While most type II supernovae show very broad emission lines which indicate expansion velocities of many thousands of kilometres per second, some, such as SN 2005gl, have relatively narrow features in their spectra. These are called type IIn, where the "n" stands for "narrow".[65]

A few supernovae, such as SN 1987K[73] and SN 1993J, appear to change types: they show lines of hydrogen at early times, but, over a period of weeks to months, become dominated by lines of helium. The term "type IIb" is used to describe the combination of features normally associated with types II and Ib.[65]

Type II supernovae with normal spectra dominated by broad hydrogen lines that remain for the life of the decline are classified on the basis of their light curves. The most common type shows a distinctive "plateau" in the light curve shortly after peak brightness where the visual luminosity stays relatively constant for several months before the decline resumes. These are called type II-P referring to the plateau. Less common are type II-L supernovae that lack a distinct plateau. The "L" signifies "linear" although the light curve is not actually a straight line.[65]

Supernovae that do not fit into the normal classifications are designated peculiar, or "pec".[65]

Types III, IV and V

[edit]

Zwicky defined additional supernovae types based on a very few examples that did not cleanly fit the parameters for type I or type II supernovae. SN 1961i in NGC 4303 was the prototype and only member of the type III supernova class, noted for its broad light curve maximum and broad hydrogen Balmer lines that were slow to develop in the spectrum.[66] SN 1961f in NGC 3003 was the prototype and only member of the type IV class, with a light curve similar to a type II-P supernova, with hydrogen absorption lines but weak hydrogen emission lines.[66] The type V class was coined for SN 1961V in NGC 1058, an unusual faint supernova or supernova impostor with a slow rise to brightness, a maximum lasting many months, and an unusual emission spectrum. The similarity of SN 1961V to the Eta Carinae Great Outburst was noted.[74] Supernovae in M101 (1909) and M83 (1923 and 1957) were also suggested as possible type IV or type V supernovae.[75]

These types would now all be treated as peculiar type II supernovae (IIpec), of which many more examples have been discovered, although it is still debated whether SN 1961V was a true supernova following an LBV outburst or an impostor.[66][76]

Current models

[edit]
In the galaxy NGC 1365 a supernova (the bright dot slightly above the galactic center) rapidly brightens, then fades more slowly.[77]

Supernova type codes, as summarised in the table above, are taxonomic: the type number is based on the light observed from the supernova, not necessarily its cause. For example, type Ia supernovae are produced by runaway fusion ignited on degenerate white dwarf progenitors, while the spectrally similar type Ib/c are produced from massive stripped progenitor stars by core collapse.

Thermal runaway

[edit]
Formation of a type Ia supernova

A white dwarf star may accumulate sufficient material from a stellar companion to raise its core temperature enough to ignite carbon fusion, at which point it undergoes runaway nuclear fusion, completely disrupting it. There are three avenues by which this detonation is theorised to happen: stable accretion of material from a companion, the collision of two white dwarfs, or accretion that causes ignition in a shell that then ignites the core. The dominant mechanism by which type Ia supernovae are produced remains unclear.[78] Despite this uncertainty in how type Ia supernovae are produced, type Ia supernovae have very uniform properties and are useful standard candles over intergalactic distances. Some calibrations are required to compensate for the gradual change in properties or different frequencies of abnormal luminosity supernovae at high redshift, and for small variations in brightness identified by light curve shape or spectrum.[79][80]

Normal type Ia

[edit]

There are several means by which a supernova of this type can form, but they share a common underlying mechanism. If a carbon-oxygen white dwarf accreted enough matter to reach the Chandrasekhar limit of about 1.44 solar masses[81] (for a non-rotating star), it would no longer be able to support the bulk of its mass through electron degeneracy pressure[82][83] and would begin to collapse. However, the current view is that this limit is not normally attained; increasing temperature and density inside the core ignite carbon fusion as the star approaches the limit (to within about 1%)[84] before collapse is initiated.[81] In contrast, for a core primarily composed of oxygen, neon and magnesium, the collapsing white dwarf will typically form a neutron star. In this case, only a fraction of the star's mass will be ejected during the collapse.[83]

The blue spot at the centre of the red ring is an isolated neutron star in the Small Magellanic Cloud.

Within a few seconds of the collapse process, a substantial fraction of the matter in the white dwarf undergoes nuclear fusion, releasing enough energy (1–2×1044 J)[85] to unbind the star in a supernova.[86] An outwardly expanding shock wave is generated, with matter reaching velocities on the order of 5,000–20,000 km/s, or roughly 3% of the speed of light. There is also a significant increase in luminosity, reaching an absolute magnitude of −19.3 (or 5 billion times brighter than the Sun), with little variation.[87]

The model for the formation of this category of supernova is a close binary star system. The larger of the two stars is the first to evolve off the main sequence, and it expands to form a red giant. The two stars now share a common envelope, causing their mutual orbit to shrink. The giant star then sheds most of its envelope, losing mass until it can no longer continue nuclear fusion. At this point, it becomes a white dwarf star, composed primarily of carbon and oxygen.[88] Eventually, the secondary star also evolves off the main sequence to form a red giant. Matter from the giant is accreted by the white dwarf, causing the latter to increase in mass. The exact details of initiation and of the heavy elements produced in the catastrophic event remain unclear.[89]

Type Ia supernovae produce a characteristic light curve—the graph of luminosity as a function of time—after the event. This luminosity is generated by the radioactive decay of nickel-56 through cobalt-56 to iron-56.[87] The peak luminosity of the light curve is extremely consistent across normal type Ia supernovae, having a maximum absolute magnitude of about −19.3. This is because typical type Ia supernovae arise from a consistent type of progenitor star by gradual mass acquisition, and explode when they acquire a consistent typical mass, giving rise to very similar supernova conditions and behaviour. This allows them to be used as a secondary[90] standard candle to measure the distance to their host galaxies.[91]

A second model for the formation of type Ia supernovae involves the merger of two white dwarf stars, with the combined mass momentarily exceeding the Chandrasekhar limit.[92] This is sometimes referred to as the double-degenerate model, as both stars are degenerate white dwarfs. Due to the possible combinations of mass and chemical composition of the pair there is much variation in this type of event,[93] and, in many cases, there may be no supernova at all, in which case they will have a less luminous light curve than the more normal SN type Ia.[94]

Non-standard type Ia

[edit]

Abnormally bright type Ia supernovae occur when the white dwarf already has a mass higher than the Chandrasekhar limit,[95] possibly enhanced further by asymmetry,[96] but the ejected material will have less than normal kinetic energy. This super-Chandrasekhar-mass scenario can occur, for example, when the extra mass is supported by differential rotation.[97]

There is no formal sub-classification for non-standard type Ia supernovae. It has been proposed that a group of sub-luminous supernovae that occur when helium accretes onto a white dwarf should be classified as type Iax.[98][99] This type of supernova may not always completely destroy the white dwarf progenitor and could leave behind a zombie star.[100]

One specific type of supernova originates from exploding white dwarfs, like type Ia, but contains hydrogen lines in their spectra, possibly because the white dwarf is surrounded by an envelope of hydrogen-rich circumstellar material. These supernovae have been dubbed type Ia/IIn, type Ian, type IIa and type IIan.[101]

The quadruple star HD 74438, belonging to the open cluster IC 2391 the Vela constellation, has been predicted to become a non-standard type Ia supernova.[102][103]

Core collapse

[edit]
The layers of a massive, evolved star just before core collapse (not to scale)

Very massive stars can undergo core collapse when nuclear fusion becomes unable to sustain the core against its own gravity; passing this threshold is the cause of all types of supernova except type Ia. The collapse may cause violent expulsion of the outer layers of the star resulting in a supernova. However, if the release of gravitational potential energy is insufficient, the star may instead collapse into a black hole or neutron star with little radiated energy.[104]

Core collapse can be caused by several different mechanisms: exceeding the Chandrasekhar limit; electron capture; pair-instability; or photodisintegration.[104][105][106]

  • When a massive star develops an iron core larger than the Chandrasekhar mass it will no longer be able to support itself by electron degeneracy pressure and will collapse further to a neutron star or black hole.
  • Electron capture by magnesium in a degenerate O/Ne/Mg core (8–10 solar mass progenitor star) removes support and causes gravitational collapse followed by explosive oxygen fusion, with very similar results.
  • Electron-positron pair production in a large post-helium burning core removes thermodynamic support and causes initial collapse followed by runaway fusion, resulting in a pair-instability supernova.
  • A sufficiently large and hot stellar core may generate gamma-rays energetic enough to initiate photodisintegration directly, which will cause a complete collapse of the core.

The table below lists the known reasons for core collapse in massive stars, the types of stars in which they occur, their associated supernova type, and the remnant produced. The metallicity is the proportion of elements other than hydrogen or helium, as compared to the Sun. The initial mass is the mass of the star prior to the supernova event, given in multiples of the Sun's mass, although the mass at the time of the supernova may be much lower.[104]

Type IIn supernovae are not listed in the table. They can be produced by various types of core collapse in different progenitor stars, possibly even by type Ia white dwarf ignitions, although it seems that most will be from iron core collapse in luminous supergiants or hypergiants (including LBVs). The narrow spectral lines for which they are named occur because the supernova is expanding into a small dense cloud of circumstellar material.[107] It appears that a significant proportion of supposed type IIn supernovae are supernova impostors, massive eruptions of LBV-like stars similar to the Great Eruption of Eta Carinae. In these events, material previously ejected from the star creates the narrow absorption lines and causes a shock wave through interaction with the newly ejected material.[108]

Core collapse scenarios by mass and metallicity[104]
Cause of collapse Progenitor star approximate initial mass (solar masses) Supernova type Remnant
Electron capture in a degenerate O+Ne+Mg core 9–10 Faint II-P Neutron star
Iron core collapse 10–25 Faint II-P Neutron star
25–40 with low or solar metallicity Normal II-P Black hole after fallback of material onto an initial neutron star
25–40 with very high metallicity II-L or II-b Neutron star
40–90 with low metallicity None Black hole
≥ 40 with near-solar metallicity Faint Ib/c, or hypernova with gamma-ray burst (GRB) Black hole after fallback of material onto an initial neutron star
≥ 40 with very high metallicity Ib/c Neutron star
≥ 90 with low metallicity None, possible GRB Black hole
Pair instability 140–250 with low metallicity II-P, sometimes a hypernova, possible GRB No remnant
Photodisintegration ≥ 250 with low metallicity None (or luminous supernova?), possible GRB Massive black hole

Detailed process

[edit]
Within a massive, evolved star (a) the onion-layered shells of elements undergo fusion, forming an iron core (b) that reaches Chandrasekhar-mass and starts to collapse. The inner part of the core is compressed into neutrons (c), causing infalling material to bounce (d) and form an outward-propagating shock front (red). The shock starts to stall (e), but it is re-invigorated, likely by neutrino heating. The surrounding material is blasted away (f), leaving only a degenerate remnant.[109]

When a stellar core is no longer supported against gravity, it collapses in on itself with velocities reaching 70,000 km/s (0.23c),[110] resulting in a rapid increase in temperature and density. What follows depends on the mass and structure of the collapsing core, with low-mass degenerate cores forming neutron stars, higher-mass degenerate cores mostly collapsing completely to black holes, and non-degenerate cores undergoing runaway fusion.[109][111]

The initial collapse of degenerate cores is accelerated by beta decay, photodisintegration and electron capture, which causes a burst of electron neutrinos. As the density increases, neutrino emission is cut off as they become trapped in the core. The inner core eventually reaches typically 30 km in diameter[112] with a density comparable to that of an atomic nucleus, and neutron degeneracy pressure tries to halt the collapse. If the core mass is more than about 15 solar masses then neutron degeneracy is insufficient to stop the collapse and a black hole forms directly with no supernova.[105]

In lower mass cores the collapse is stopped and the newly formed neutron core has an initial temperature of about 100 billion kelvin, 6,000 times the temperature of the Sun's core.[109] At this temperature, neutrino-antineutrino pairs of all flavours are efficiently formed by thermal emission. These thermal neutrinos are several times more abundant than the electron-capture neutrinos.[113] About 1046 joules, approximately 10% of the star's rest mass, is converted into a ten-second burst of neutrinos, which is the main output of the event.[112][114] The suddenly halted core collapse rebounds and produces a shock wave that stalls in the outer core within milliseconds[115] as energy is lost through the dissociation of heavy elements. A process that is not clearly understood is necessary to allow the outer layers of the core to reabsorb around 1044 joules[114] (1 foe) from the neutrino pulse, producing the visible brightness, although there are other theories that could power the explosion.[112]

Some material from the outer envelope falls back onto the neutron star, and, for cores beyond about 8 M, there is sufficient fallback to form a black hole. This fallback will reduce the kinetic energy created and the mass of expelled radioactive material, but in some situations, it may also generate relativistic jets that result in a gamma-ray burst or an exceptionally luminous supernova.[116]

The collapse of a massive non-degenerate core will ignite further fusion.[111] When the core collapse is initiated by pair instability (photons turning into electron-positron pairs, thereby reducing the radiation pressure) oxygen fusion begins and the collapse may be halted. For core masses of 40–60 M, the collapse halts and the star remains intact, but collapse will occur again when a larger core has formed. For cores of around 60–130 M, the fusion of oxygen and heavier elements is so energetic that the entire star is disrupted, causing a supernova. At the upper end of the mass range, the supernova is unusually luminous and extremely long-lived due to many solar masses of ejected 56Ni. For even larger core masses, the core temperature becomes high enough to allow photodisintegration and the core collapses completely into a black hole.[117][105]

Type II

[edit]
The atypical subluminous type II SN 1997D

Stars with initial masses less than about 8 M never develop a core large enough to collapse and they eventually lose their atmospheres to become white dwarfs. Stars with at least 9 M (possibly as much as 12 M[118]) evolve in a complex fashion, progressively burning heavier elements at hotter temperatures in their cores.[112][119] The star becomes layered like an onion, with the burning of more easily fused elements occurring in larger shells.[104][120] Although popularly described as an onion with an iron core, the least massive supernova progenitors only have oxygen-neon(-magnesium) cores. These super-AGB stars may form the majority of core collapse supernovae, although less luminous and so less commonly observed than those from more massive progenitors.[118]

If core collapse occurs during a supergiant phase when the star still has a hydrogen envelope, the result is a type II supernova.[121] The rate of mass loss for luminous stars depends on the metallicity and luminosity. Extremely luminous stars at near solar metallicity will lose all their hydrogen before they reach core collapse and so will not form a supernova of type II.[121] At low metallicity, all stars will reach core collapse with a hydrogen envelope but sufficiently massive stars collapse directly to a black hole without producing a visible supernova.[104]

Stars with an initial mass up to about 90 times the Sun, or a little less at high metallicity, result in a type II-P supernova, which is the most commonly observed type. At moderate to high metallicity, stars near the upper end of that mass range will have lost most of their hydrogen when core collapse occurs and the result will be a type II-L supernova.[122] At very low metallicity, stars of around 140–250 M will reach core collapse by pair instability while they still have a hydrogen atmosphere and an oxygen core and the result will be a supernova with type II characteristics but a very large mass of ejected 56Ni and high luminosity.[104][123]

Type Ib and Ic

[edit]
Type Ib SN 2008D[124] at the far upper end of the galaxy, shown in X-ray (left) and visible light (right),[125] with the brighter SN 2007uy closer to the centre

These supernovae, like those of type II, are massive stars that undergo core collapse. Unlike the progenitors of type II supernovae, the stars which become types Ib and Ic supernovae have lost most of their outer (hydrogen) envelopes due to strong stellar winds or else from interaction with a companion.[126] These stars are known as Wolf–Rayet stars, and they occur at moderate to high metallicity where continuum driven winds cause sufficiently high mass-loss rates. Observations of type Ib/c supernova do not match the observed or expected occurrence of Wolf–Rayet stars. Alternate explanations for this type of core collapse supernova involve stars stripped of their hydrogen by binary interactions. Binary models provide a better match for the observed supernovae, with the proviso that no suitable binary helium stars have ever been observed.[127]

Type Ib supernovae are the more common and result from Wolf–Rayet stars of type WC which still have helium in their atmospheres. For a narrow range of masses, stars evolve further before reaching core collapse to become WO stars with very little helium remaining, and these are the progenitors of type Ic supernovae.[128]

A few percent of the type Ic supernovae are associated with gamma-ray bursts (GRB), though it is also believed that any hydrogen-stripped type Ib or Ic supernova could produce a GRB, depending on the circumstances of the geometry.[129] The mechanism for producing this type of GRB is the jets produced by the magnetic field of the rapidly spinning magnetar formed at the collapsing core of the star. The jets would also transfer energy into the expanding outer shell, producing a super-luminous supernova.[116][130][131]

Ultra-stripped supernovae occur when the exploding star has been stripped (almost) all the way to the metal core, via mass transfer in a close binary.[132][133] As a result, very little material is ejected from the exploding star (c. 0.1 M). In the most extreme cases, ultra-stripped supernovae can occur in naked metal cores, barely above the Chandrasekhar mass limit. SN 2005ek[134] might be the first observational example of an ultra-stripped supernova, giving rise to a relatively dim and fast decaying light curve. The nature of ultra-stripped supernovae can be both iron core-collapse and electron capture supernovae, depending on the mass of the collapsing core. Ultra-stripped supernovae are believed to be associated with the second supernova explosion in a binary system, producing for example a tight double neutron star system.[135][136]

In 2022 a team of astronomers led by researchers from the Weizmann Institute of Science reported the first supernova explosion showing direct evidence for a Wolf-Rayet progenitor star. SN 2019hgp was a type Icn supernova and is also the first in which the element neon has been detected.[137][138]

Electron-capture supernovae

[edit]

In 1980, a "third type" of supernova was predicted by Ken'ichi Nomoto of the University of Tokyo, called an electron-capture supernova. It would arise when a star "in the transitional range (~8 to 10 solar masses) between white dwarf formation and iron core-collapse supernovae", and with a degenerate O+Ne+Mg core,[139] imploded after its core ran out of nuclear fuel, causing gravity to compress the electrons in the star's core into their atomic nuclei,[140][141] leading to a supernova explosion and leaving behind a neutron star.[104] In June 2021, a paper in the journal Nature Astronomy reported that the 2018 supernova SN 2018zd (in the galaxy NGC 2146, about 31 million light-years from Earth) appeared to be the first observation of an electron-capture supernova.[139][140][141] The 1054 supernova explosion that created the Crab Nebula in our galaxy had been thought to be the best candidate for an electron-capture supernova, and the 2021 paper makes it more likely that this was correct.[140][141]

Failed supernovae

[edit]

The core collapse of some massive stars may not result in a visible supernova. This happens if the initial core collapse cannot be reversed by the mechanism that produces an explosion, usually because the core is too massive. These events are difficult to detect, but large surveys have detected possible candidates.[142][143] The red supergiant N6946-BH1 in NGC 6946 underwent a modest outburst in March 2009, before fading from view. Only a faint infrared source remains at the star's location.[144]

Light curves

[edit]
Typical light curves for several types of supernovae; in practice, magnitude and duration varies within each type. See Karttunen et al. for types Ia, Ib, II-L and II-P;[145] Modjaz et al. for types Ic and IIb;[146] and Nyholm et al. for type IIn.[147]

The ejecta gases would dim quickly without some energy input to keep them hot. The source of this energy—which can maintain the optical supernova glow for months—was, at first, a puzzle. Some considered rotational energy from the central pulsar as a source.[148] Although the energy that initially powers each type of supernovae is delivered promptly, the light curves are dominated by subsequent radioactive heating of the rapidly expanding ejecta. The intensely radioactive nature of the ejecta gases was first calculated on sound nucleosynthesis grounds in the late 1960s, and this has since been demonstrated as correct for most supernovae.[149] It was not until SN 1987A that direct observation of gamma-ray lines unambiguously identified the major radioactive nuclei.[150]

It is now known by direct observation that much of the light curve (the graph of luminosity as a function of time) after the occurrence of a type II Supernova, such as SN 1987A, is explained by those predicted radioactive decays.[9] Although the luminous emission consists of optical photons, it is the radioactive power absorbed by the ejected gases that keeps the remnant hot enough to radiate light. The radioactive decay of 56Ni through its daughters 56Co to 56Fe produces gamma-ray photons, primarily with energies of 847 keV and 1,238 keV, that are absorbed and dominate the heating and thus the luminosity of the ejecta at intermediate times (several weeks) to late times (several months).[151] Energy for the peak of the light curve of SN1987A was provided by the decay of 56Ni to 56Co (half-life 6 days) while energy for the later light curve in particular fit very closely with the 77.3-day half-life of 56Co decaying to 56Fe. Later measurements by space gamma-ray telescopes of the small fraction of the 56Co and 57Co gamma rays that escaped the SN 1987A remnant without absorption confirmed earlier predictions that those two radioactive nuclei were the power sources.[150]

Messier 61 with supernova SN2020jfo, taken by an amateur astronomer in 2020

The late-time decay phase of visual light curves for different supernova types all depend on radioactive heating, but they vary in shape and amplitude because of the underlying mechanisms, the way that visible radiation is produced, the epoch of its observation, and the transparency of the ejected material.[152] The light curves can be significantly different at other wavelengths. For example, at ultraviolet wavelengths there is an early extremely luminous peak lasting only a few hours corresponding to the breakout of the shock launched by the initial event, but that breakout is hardly detectable optically.[153][154]

The light curves for type Ia are mostly very uniform, with a consistent maximum absolute magnitude and a relatively steep decline in luminosity. Their optical energy output is driven by radioactive decay of ejected nickel-56 (half-life 6 days), which then decays to radioactive cobalt-56 (half-life 77 days). These radioisotopes excite the surrounding material to incandescence.[87] Modern studies of cosmology rely on 56Ni radioactivity providing the energy for the optical brightness of supernovae of type Ia, which are the "standard candles" of cosmology but whose diagnostic 847 keV and 1,238 keV gamma rays were first detected only in 2014.[155] The initial phases of the light curve decline steeply as the effective size of the photosphere decreases and trapped electromagnetic radiation is depleted. The light curve continues to decline in the B band while it may show a small shoulder in the visual at about 40 days, but this is only a hint of a secondary maximum that occurs in the infra-red as certain ionised heavy elements recombine to produce infra-red radiation and the ejecta become transparent to it. The visual light curve continues to decline at a rate slightly greater than the decay rate of the radioactive cobalt (which has the longer half-life and controls the later curve), because the ejected material becomes more diffuse and less able to convert the high energy radiation into visual radiation. After several months, the light curve changes its decline rate again as positron emission from the remaining cobalt-56 becomes dominant, although this portion of the light curve has been little-studied.[156]

Type Ib and Ic light curves are similar to type Ia although with a lower average peak luminosity. The visual light output is again due to radioactive decay being converted into visual radiation, but there is a much lower mass of the created nickel-56. The peak luminosity varies considerably and there are even occasional type Ib/c supernovae orders of magnitude more and less luminous than the norm. The most luminous type Ic supernovae are referred to as hypernovae and tend to have broadened light curves in addition to the increased peak luminosity. The source of the extra energy is thought to be relativistic jets driven by the formation of a rotating black hole, which also produce gamma-ray bursts.[157][158]

The light curves for type II supernovae are characterised by a much slower decline than type I, on the order of 0.05 magnitudes per day,[72] excluding the plateau phase. The visual light output is dominated by kinetic energy rather than radioactive decay for several months, due primarily to the existence of hydrogen in the ejecta from the atmosphere of the supergiant progenitor star. In the initial destruction this hydrogen becomes heated and ionised. The majority of type II supernovae show a prolonged plateau in their light curves as this hydrogen recombines, emitting visible light and becoming more transparent. This is then followed by a declining light curve driven by radioactive decay although slower than in type I supernovae, due to the efficiency of conversion into light by all the hydrogen.[66]

In type II-L the plateau is absent because the progenitor had relatively little hydrogen left in its atmosphere, sufficient to appear in the spectrum but insufficient to produce a noticeable plateau in the light output. In type IIb supernovae the hydrogen atmosphere of the progenitor is so depleted (thought to be due to tidal stripping by a companion star) that the light curve is closer to a type I supernova and the hydrogen even disappears from the spectrum after several weeks.[66]

Type IIn supernovae are characterised by additional narrow spectral lines produced in a dense shell of circumstellar material. Their light curves are generally very broad and extended, occasionally also extremely luminous and referred to as a superluminous supernova. These light curves are produced by the highly efficient conversion of kinetic energy of the ejecta into electromagnetic radiation by interaction with the dense shell of material. This only occurs when the material is sufficiently dense and compact, indicating that it has been produced by the progenitor star itself only shortly before the supernova occurs.[159][160]

Large numbers of supernovae have been catalogued and classified to provide distance candles and test models.[161][162] Average characteristics vary somewhat with distance and type of host galaxy, but can broadly be specified for each supernova type.

Physical properties of supernovae by type[163][164]
Typea Average peak absolute magnitudeb Approximate energy (foe)c Days to peak luminosity Days from peak to 10% luminosity
Ia −19 1 approx. 19 around 60
Ib/c (faint) around −15 0.1 15–25 unknown
Ib around −17 1 15–25 40–100
Ic around −16 1 15–25 40–100
Ic (bright) to −22 above 5 roughly 25 roughly 100
II-b around −17 1 around 20 around 100
II-L around −17 1 around 13 around 150
II-P (faint) around −14 0.1 roughly 15 unknown
II-P around −16 1 around 15 Plateau then around 50
IInd around −17 1 12–30 or more 50–150
IIn (bright) to −22 above 5 above 50 above 100

Notes:

  1. ^ Faint types may be a distinct sub-class. Bright types may be a continuum from slightly over-luminous to hypernovae.
  2. ^ These magnitudes are measured in the R band. Measurements in V or B bands are common and will be around half a magnitude brighter for supernovae.
  3. ^ Order of magnitude kinetic energy. Total electromagnetic radiated energy is usually lower, (theoretical) neutrino energy much higher.
  4. ^ Probably a heterogeneous group, any of the other types embedded in nebulosity.

Asymmetry

[edit]
The pulsar in the Crab Nebula is travelling at 375 km/s relative to the nebula.[165]

A long-standing puzzle surrounding type II supernovae is why the remaining compact object receives a large velocity away from the epicentre;[166] pulsars, and thus neutron stars, are observed to have high peculiar velocities, and black holes presumably do as well, although they are far harder to observe in isolation. The initial impetus can be substantial, propelling an object of more than a solar mass at a velocity of 500 km/s or greater. This indicates an expansion asymmetry, but the mechanism by which momentum is transferred to the compact object remains a puzzle. Proposed explanations for this kick include convection in the collapsing star, asymmetric ejection of matter during neutron star formation, and asymmetrical neutrino emissions.[166][167]

One possible explanation for this asymmetry is large-scale convection above the core. The convection can create radial variations in density giving rise to variations in the amount of energy absorbed from neutrino outflow.[109] However analysis of this mechanism predicts only modest momentum transfer.[168] Another possible explanation is that accretion of gas onto the central neutron star can create a disk that drives highly directional jets, propelling matter at a high velocity out of the star, and driving transverse shocks that completely disrupt the star. These jets might play a crucial role in the resulting supernova.[169][170] (A similar model is used for explaining long gamma-ray bursts.) The dominant mechanism may depend upon the mass of the progenitor star.[167]

Initial asymmetries have also been confirmed in type Ia supernovae through observation. This result may mean that the initial luminosity of this type of supernova depends on the viewing angle. However, the expansion becomes more symmetrical with the passage of time. Early asymmetries are detectable by measuring the polarisation of the emitted light.[171]

Energy output

[edit]
The radioactive decays of nickel-56 and cobalt-56 that produce a supernova visible light curve[87][172]

Although supernovae are primarily known as luminous events, the electromagnetic radiation they release is almost a minor side-effect. Particularly in the case of core collapse supernovae, the emitted electromagnetic radiation is a tiny fraction of the total energy released during the event.[173]

There is a fundamental difference between the balance of energy production in the different types of supernova. In type Ia white dwarf detonations, most of the energy is directed into heavy element synthesis and the kinetic energy of the ejecta.[174] In core collapse supernovae, the vast majority of the energy is directed into neutrino emission, and while some of this apparently powers the observed destruction, 99%+ of the neutrinos escape the star in the first few minutes following the start of the collapse.[47]

Standard type Ia supernovae derive their energy from a runaway nuclear fusion of a carbon-oxygen white dwarf. The details of the energetics are still not fully understood, but the result is the ejection of the entire mass of the original star at high kinetic energy. Around half a solar mass of that mass is 56Ni generated from silicon burning. 56Ni is radioactive and decays into 56Co by beta plus decay (with a half life of six days) and gamma rays. 56Co itself decays by the beta plus (positron) path with a half life of 77 days into stable 56Fe. These two processes are responsible for the electromagnetic radiation from type Ia supernovae. In combination with the changing transparency of the ejected material, they produce the rapidly declining light curve.[172]

Core collapse supernovae are on average visually fainter than type Ia supernovae,[145][146][147] but the total energy released is far higher, as outlined in the following table.

Energetics of supernovae
Supernova Approximate total energy
x1044 joules (foe)c
Ejected Ni
(solar masses)
Neutrino energy
(foe)
Kinetic energy
(foe)
Electromagnetic radiation
(foe)
Type Ia[172][175][176] 1.5 0.4 – 0.8 0.1 1.3 – 1.4 ~0.01
Core collapse[177][178] 100 (0.01) – 1 100 1 0.001 – 0.01
Hypernova 100 ~1 1–100 1–100 ~0.1
Pair instability[117] 5–100 0.5 – 50 low? 1–100 0.01 – 0.1

In some core collapse supernovae, fallback onto a black hole drives relativistic jets which may produce a brief energetic and directional burst of gamma rays and also transfers substantial further energy into the ejected material. This is one scenario for producing high-luminosity supernovae and is thought to be the cause of type Ic hypernovae and long-duration gamma-ray bursts.[179] If the relativistic jets are too brief and fail to penetrate the stellar envelope then a low-luminosity gamma-ray burst may be produced and the supernova may be sub-luminous.[180]

When a supernova occurs inside a small dense cloud of circumstellar material, it will produce a shock wave that can efficiently convert a high fraction of the kinetic energy into electromagnetic radiation. Even though the initial energy was entirely normal the resulting supernova will have high luminosity and extended duration since it does not rely on exponential radioactive decay. This type of event may cause type IIn hypernovae.[181][182]

Although pair-instability supernovae are core collapse supernovae with spectra and light curves similar to type II-P, the nature after core collapse is more like that of a giant type Ia with runaway fusion of carbon, oxygen and silicon. The total energy released by the highest-mass events is comparable to other core collapse supernovae but neutrino production is thought to be very low, hence the kinetic and electromagnetic energy released is very high. The cores of these stars are much larger than any white dwarf and the amount of radioactive nickel and other heavy elements ejected from their cores can be orders of magnitude higher, with consequently high visual luminosity.[183]

Progenitor

[edit]
Occasional supernovae appear in this sped-up artist's impression of distant galaxies. Each exploding star briefly rivals the brightness of its host galaxy.

The supernova classification type is closely tied to the type of progenitor star at the time of the collapse. The occurrence of each type of supernova depends on the star's metallicity, since this affects the strength of the stellar wind and thereby the rate at which the star loses mass.[184]

Type Ia supernovae are produced from white dwarf stars in binary star systems and occur in all galaxy types.[185] Core collapse supernovae are only found in galaxies undergoing current or very recent star formation, since they result from short-lived massive stars. They are most commonly found in type Sc spirals, but also in the arms of other spiral galaxies and in irregular galaxies, especially starburst galaxies.[186][187][188]

Type Ib and Ic supernovae are hypothesised to have been produced by core collapse of massive stars that have lost their outer layer of hydrogen and helium, either via strong stellar winds or mass transfer to a companion.[158] They normally occur in regions of new star formation, and are extremely rare in elliptical galaxies.[71] The progenitors of type IIn supernovae also have high rates of mass loss in the period just prior to their explosions.[189] Type Ic supernovae have been observed to occur in regions that are more metal-rich and have higher star-formation rates than average for their host galaxies.[190] The table shows the progenitor for the main types of core collapse supernova, and the approximate proportions that have been observed in the local neighbourhood.

Fraction of core collapse supernovae types by progenitor[127]
Type Progenitor star Fraction
Ib WC Wolf–Rayet or helium star 9.0%
Ic WO Wolf–Rayet 17.0%
II-P Supergiant 55.5%
II-L Supergiant with a depleted hydrogen shell 3.0%
IIn Supergiant in a dense cloud of expelled material (such as LBV) 2.4%
IIb Supergiant with highly depleted hydrogen (stripped by companion?) 12.1%
IIpec Blue supergiant 1.0%
Supernova types by initial mass-metallicity
Remnants of single massive stars

There are a number of difficulties reconciling modelled and observed stellar evolution leading up to core collapse supernovae. Red supergiants are the progenitors for the vast majority of core collapse supernovae, and these have been observed but only at relatively low masses and luminosities, below about 18 M and 100,000 L, respectively. Most progenitors of type II supernovae are not detected and must be considerably fainter, and presumably less massive. This discrepancy has been referred to as the red supergiant problem.[191] It was first described in 2009 by Stephen Smartt, who also coined the term. After performing a volume-limited search for supernovae, Smartt et al. found the lower and upper mass limits for type II-P supernovae to form to be 8.5+1
−1.5
 M and 16.5±1.5 M, respectively. The former is consistent with the expected upper mass limits for white dwarf progenitors to form, but the latter is not consistent with massive star populations in the Local Group.[192] The upper limit for red supergiants that produce a visible supernova explosion has been calculated at 19+4
−2
 M
.[191]

It is thought that higher mass red supergiants do not explode as supernovae, but instead evolve back towards hotter temperatures. Several progenitors of type IIb supernovae have been confirmed, and these were K and G supergiants, plus one A supergiant.[193] Yellow hypergiants or LBVs are proposed progenitors for type IIb supernovae, and almost all type IIb supernovae near enough to observe have shown such progenitors.[194][195]

Infographic showing arrows between circles representing stellar evolution and how it varies by mass
Approximate stellar evolution pathways of supernova progenitor stars (and lower mass stars) with circle size reflecting relative size and color related to temperature

Blue supergiants form an unexpectedly high proportion of confirmed supernova progenitors, partly due to their high luminosity and easy detection, while not a single Wolf–Rayet progenitor has yet been clearly identified.[193][196] Models have had difficulty showing how blue supergiants lose enough mass to reach supernova without progressing to a different evolutionary stage. One study has shown a possible route for low-luminosity post-red supergiant luminous blue variables to collapse, most likely as a type IIn supernova.[197] Several examples of hot luminous progenitors of type IIn supernovae have been detected: SN 2005gy and SN 2010jl were both apparently massive luminous stars, but are very distant; and SN 2009ip had a highly luminous progenitor likely to have been an LBV, but is a peculiar supernova whose exact nature is disputed.[193]

The progenitors of type Ib/c supernovae are not observed at all, and constraints on their possible luminosity are often lower than those of known WC stars.[193] WO stars are extremely rare and visually relatively faint, so it is difficult to say whether such progenitors are missing or just yet to be observed. Very luminous progenitors have not been securely identified, despite numerous supernovae being observed near enough that such progenitors would have been clearly imaged.[196] Population modelling shows that the observed type Ib/c supernovae could be reproduced by a mixture of single massive stars and stripped-envelope stars from interacting binary systems.[127] The continued lack of unambiguous detection of progenitors for normal type Ib and Ic supernovae may be due to most massive stars collapsing directly to a black hole without a supernova outburst. Most of these supernovae are then produced from lower-mass low-luminosity helium stars in binary systems. A small number would be from rapidly rotating massive stars, likely corresponding to the highly energetic type Ic-BL events that are associated with long-duration gamma-ray bursts.[193]

External impact

[edit]

Supernovae events generate heavier elements that are scattered throughout the surrounding interstellar medium. The expanding shock wave from a supernova can trigger star formation. Galactic cosmic rays are generated by supernova explosions.

Source of heavy elements

[edit]
Periodic table showing the source of each element in the interstellar medium

Supernovae are a major source of elements in the interstellar medium from oxygen through to rubidium,[198][199][200] though the theoretical abundances of the elements produced or seen in the spectra varies significantly depending on the various supernova types.[200] Type Ia supernovae produce mainly silicon and iron-peak elements, metals such as nickel and iron.[201][202] Core collapse supernovae eject much smaller quantities of the iron-peak elements than type Ia supernovae, but larger masses of light alpha elements such as oxygen and neon, and elements heavier than zinc. The latter is especially true with electron capture supernovae.[203] The bulk of the material ejected by type II supernovae is hydrogen and helium.[204] The heavy elements are produced by: nuclear fusion for nuclei up to 34S; silicon photodisintegration rearrangement and quasiequilibrium during silicon burning for nuclei between 36Ar and 56Ni; and rapid capture of neutrons (r-process) during the supernova's collapse for elements heavier than iron. The r-process produces highly unstable nuclei that are rich in neutrons and that rapidly beta decay into more stable forms. In supernovae, r-process reactions are responsible for about half of all the isotopes of elements beyond iron,[205] although neutron star mergers may be the main astrophysical source for many of these elements.[198][206]

In the modern universe, old asymptotic giant branch (AGB) stars are the dominant source of dust from oxides, carbon and s-process elements.[198][207] However, in the early universe, before AGB stars formed, supernovae may have been the main source of dust.[208]

Role in stellar evolution

[edit]

Remnants of many supernovae consist of a compact object and a rapidly expanding shock wave of material. This cloud of material sweeps up surrounding interstellar medium during a free expansion phase, which can last for up to two centuries. The wave then gradually undergoes a period of adiabatic expansion, and will slowly cool and mix with the surrounding interstellar medium over a period of about 10,000 years.[209]

Supernova remnant N 63A lies within a clumpy region of gas and dust in the Large Magellanic Cloud.

The Big Bang produced hydrogen, helium and traces of lithium, while all heavier elements are synthesised in stars, supernovae, and collisions between neutron stars (thus being indirectly due to supernovae). Supernovae tend to enrich the surrounding interstellar medium with elements other than hydrogen and helium, which usually astronomers refer to as "metals".[210] These ejected elements ultimately enrich the molecular clouds that are the sites of star formation.[211] Thus, each stellar generation has a slightly different composition, going from an almost pure mixture of hydrogen and helium to a more metal-rich composition. Supernovae are the dominant mechanism for distributing these heavier elements, which are formed in a star during its period of nuclear fusion. The different abundances of elements in the material that forms a star have important influences on the star's life,[210][212] and may influence the possibility of having planets orbiting it: more giant planets form around stars of higher metallicity.[213][214]

The kinetic energy of an expanding supernova remnant can trigger star formation by compressing nearby, dense molecular clouds in space.[215] The increase in turbulent pressure can also prevent star formation if the cloud is unable to lose the excess energy.[216]

Evidence from daughter products of short-lived radioactive isotopes shows that a nearby supernova helped determine the composition of the Solar System 4.5 billion years ago, and may even have triggered the formation of this system.[217]

Fast radio bursts (FRBs) are intense, transient pulses of radio waves that typically last no more than milliseconds. Many explanations for these events have been proposed; magnetars produced by core-collapse supernovae are leading candidates.[218][219][220][221]

Cosmic rays

[edit]

Supernova remnants are thought to accelerate a large fraction of galactic primary cosmic rays, but direct evidence for cosmic ray production has only been found in a small number of remnants. Gamma rays from pion-decay have been detected from the supernova remnants IC 443 and W44. These are produced when accelerated protons from the remnant impact on interstellar material.[222]

Gravitational waves

[edit]

Supernovae are potentially strong galactic sources of gravitational waves,[223] but none have so far been detected. The only gravitational wave events so far detected are from mergers of black holes and neutron stars, probable remnants of supernovae.[224] Like the neutrino emissions, the gravitational waves produced by a core-collapse supernova are expected to arrive without the delay that affects light. Consequently, they may provide information about the core-collapse process that is unavailable by other means. Most gravitational-wave signals predicted by supernova models are short in duration, lasting less than a second, and thus difficult to detect. Using the arrival of a neutrino signal may provide a trigger that can identify the time window in which to seek the gravitational wave, helping to distinguish the latter from background noise.[225]

Effect on Earth

[edit]

A near-Earth supernova is a supernova close enough to the Earth to have noticeable effects on its biosphere. Depending upon the type and energy of the supernova, it could be as far as 3,000 light-years away. In 1996 it was theorised that traces of past supernovae might be detectable on Earth in the form of metal isotope signatures in rock strata. Iron-60 enrichment was later reported in deep-sea rock of the Pacific Ocean.[226][227][228] In 2009, elevated levels of nitrate ions were found in Antarctic ice, which coincided with the 1006 and 1054 supernovae. Gamma rays from these supernovae could have boosted atmospheric levels of nitrogen oxides, which became trapped in the ice.[229]

Historically, nearby supernovae may have influenced the biodiversity of life on the planet. Geological records suggest that nearby supernova events have led to an increase in cosmic rays, which in turn produced a cooler climate. A greater temperature difference between the poles and the equator created stronger winds, increased ocean mixing, and resulted in the transport of nutrients to shallow waters along the continental shelves. This led to greater biodiversity.[230][231]

Type Ia supernovae are thought to be potentially the most dangerous if they occur close enough to the Earth. Because these supernovae arise from dim, common white dwarf stars in binary systems, it is likely that a supernova that can affect the Earth will occur unpredictably and in a star system that is not well studied. The closest-known candidate is IK Pegasi (HR 8210), about 150 light-years away,[232][233] but observations suggest it could be as long as 1.9 billion years before the white dwarf can accrete the critical mass required to become a type Ia supernova.[234]

According to a 2003 estimate, a type II supernova would have to be closer than eight parsecs (26 light-years) to destroy half of the Earth's ozone layer, and there are no such candidates closer than about 500 light-years.[235]

Milky Way candidates

[edit]
The nebula around Wolf–Rayet star WR124, which is located at a distance of about 21,000 light-years[236]

The next supernova in the Milky Way will likely be detectable even if it occurs on the far side of the galaxy. It is likely to be produced by the collapse of an unremarkable red supergiant, and it is very probable that it will already have been catalogued in infrared surveys such as 2MASS. There is a smaller chance that the next core collapse supernova will be produced by a different type of massive star such as a yellow hypergiant, luminous blue variable, or Wolf–Rayet. The chances of the next supernova being a type Ia produced by a white dwarf are calculated to be about a third of those for a core collapse supernova. Again it should be observable wherever it occurs, but it is less likely that the progenitor will ever have been observed. It is not even known exactly what a type Ia progenitor system looks like, and it is difficult to detect them beyond a few parsecs. The total supernova rate in the Milky Way is estimated to be between 2 and 12 per century, although one has not actually been observed for several centuries.[144]

Statistically, the most common variety of core-collapse supernova is type II-P, and the progenitors of this type are red supergiants.[237] It is difficult to identify which of those supergiants are in the final stages of heavy element fusion in their cores and which have millions of years left. The most-massive red supergiants shed their atmospheres and evolve to Wolf–Rayet stars before their cores collapse. All Wolf–Rayet stars end their lives from the Wolf–Rayet phase within a million years or so, but again it is difficult to identify those that are closest to core collapse. One class that is expected to have no more than a few thousand years before exploding are the WO Wolf–Rayet stars, which are known to have exhausted their core helium.[238] Only eight of them are known, and only four of those are in the Milky Way.[239]

A number of close or well-known stars have been identified as possible core collapse supernova candidates: the high-mass blue stars Spica and Rigel,[240] the red supergiants Betelgeuse, Antares, and VV Cephei A;[241][242][243] the yellow hypergiant Rho Cassiopeiae;[244] the luminous blue variable Eta Carinae that has already produced a supernova impostor;[245] and both components, a blue supergiant and a Wolf–Rayet star, of the Regor or Gamma Velorum system.[246][247] Mimosa and Acrux, two bright star systems in the southern constellation of Crux, each contain blue stars with sufficient masses to explode as supernovae.[248][249] Others have gained notoriety as possible, although not very likely, progenitors for a gamma-ray burst; for example WR 104.[250]

Identification of candidates for a type Ia supernova is much more speculative. Any binary with an accreting white dwarf might produce a supernova although the exact mechanism and timescale is still debated. These systems are faint and difficult to identify, but the novae and recurrent novae are such systems that conveniently advertise themselves. One example is U Scorpii.[251]

Map showing some of the closest core-collapse supernova candidates to Earth within one kiloparsec, most of which are K-type red supergiants.[243]

See also

[edit]

References

[edit]
  1. ^ Zwicky, Fritz (1 January 1940). "Types of Novae". Reviews of Modern Physics. 12 (1): 66–85. Bibcode:1940RvMP...12...66Z. doi:10.1103/RevModPhys.12.66. ISSN 0034-6861.
  2. ^ a b Osterbrock, D. E. (1 December 2001). "Who Really Coined the Word Supernova? Who First Predicted Neutron Stars?". American Astronomical Society Meeting Abstracts. 199: 15.01. Bibcode:2001AAS...199.1501O.
  3. ^ "supernova". Oxford English Dictionary (Online ed.). Oxford University Press. (Subscription or participating institution membership required.)
  4. ^ Murdin, P.; Murdin, L. (1978). Supernovae. New York, New York: Press Syndicate of the University of Cambridge. pp. 1–3. ISBN 978-0521300384.
  5. ^ Joglekar, H.; Vahia, M. N.; Sule, A. (2011). "Oldest sky-chart with Supernova record (in Kashmir)" (PDF). Purātattva: Journal of the Indian Archaeological Society (41): 207–211. Archived (PDF) from the original on 10 May 2019. Retrieved 29 May 2019.
  6. ^ Murdin, Paul; Murdin, Lesley (1985). Supernovae. Cambridge University Press. pp. 14–16. ISBN 978-0521300384.
  7. ^ Burnham, Robert Jr. (1978). The Celestial handbook. Dover. pp. 1117–1122.
  8. ^ Winkler, P. F.; Gupta, G.; Long, K. S. (2003). "The SN 1006 Remnant: Optical Proper Motions, Deep Imaging, Distance, and Brightness at Maximum". Astrophysical Journal. 585 (1): 324–335. arXiv:astro-ph/0208415. Bibcode:2003ApJ...585..324W. doi:10.1086/345985. S2CID 1626564.
  9. ^ a b Fraknoi, Andrew; et al. (2022). Astronomy 2e. OpenStax. p. 767. ISBN 978-1-951-69350-3.
  10. ^ Clark, D. H.; Stephenson, F. R. (1982). "The Historical Supernovae". Supernovae: A survey of current research; Proceedings of the Advanced Study Institute, Cambridge, England, 29 June – 10 July 1981. Dordrecht: D. Reidel. pp. 355–370. Bibcode:1982ASIC...90..355C.
  11. ^ Baade, W. (1943). "No. 675. Nova Ophiuchi of 1604 as a supernova". Contributions from the Mount Wilson Observatory / Carnegie Institution of Washington. 675: 1–9. Bibcode:1943CMWCI.675....1B.
  12. ^ Motz, L.; Weaver, J. H. (2001). The Story of Astronomy. Basic Books. p. 76. ISBN 978-0-7382-0586-1.
  13. ^ Chakraborti, S.; Childs, F.; Soderberg, A. (25 February 2016). "Young Remnants of type Ia Supernovae and Their Progenitors: A Study Of SNR G1.9+0.3". The Astrophysical Journal. 819 (1): 37. arXiv:1510.08851. Bibcode:2016ApJ...819...37C. doi:10.3847/0004-637X/819/1/37. S2CID 119246128.
  14. ^ Krause, O. (2008). "The Cassiopeia A Supernova was of type IIb". Science. 320 (5880): 1195–1197. arXiv:0805.4557. Bibcode:2008Sci...320.1195K. doi:10.1126/science.1155788. PMID 18511684. S2CID 40884513.
  15. ^ Pankenier, David W. (2006). "Notes on translations of the East Asian records relating to the supernova of AD 1054". Journal of Astronomical History and Heritage. 9 (1): 77. Bibcode:2006JAHH....9...77P. doi:10.3724/SP.J.1440-2807.2006.01.06. S2CID 54914821.
  16. ^ "SNRcat – High Energy Observations of Galactic Supernova Remnants". University of Manitoba. Retrieved 16 October 2020.
  17. ^ Chin, Y.-N.; Huang, Y.-L. (September 1994). "Identification of the guest star of AD 185 as a comet rather than a supernova". Nature (in German). 371 (6496): 398–399. Bibcode:1994Natur.371..398C. doi:10.1038/371398a0. ISSN 0028-0836. S2CID 4240119. Retrieved 8 November 2021.
  18. ^ Zhao, Fu-Yuan; Strom, R. G.; Jiang, Shi-Yang (October 2006). "The Guest Star of AD185 must have been a Supernova". Chinese Journal of Astronomy and Astrophysics (in German). 6 (5): 635–640. Bibcode:2006ChJAA...6..635Z. doi:10.1088/1009-9271/6/5/17. ISSN 1009-9271.
  19. ^ Moore, Patrick (2000). The Data Book of Astronomy. CRC Press. pp. 295–296. ISBN 978-1-4200-3344-1.
  20. ^ a b Hoffmann, Susanne M.; Vogt, Nikolaus (1 July 2020). "A search for the modern counterparts of the Far Eastern guest stars 369 CE, 386 CE and 393 CE". Monthly Notices of the Royal Astronomical Society (in German). 497 (2): 1419–1433. arXiv:2007.01013. Bibcode:2020MNRAS.497.1419H. doi:10.1093/mnras/staa1970.
  21. ^ Winkler, P. Frank; Gupta, G. (2003), "The SN 1006 Reminant: Optical Proper Motions, Deep Imaging, Distance, and Brightness at Maximum", The Astrophysical Journal (in German), 585 (1): 324–335, arXiv:astro-ph/0208415, Bibcode:2003ApJ...585..324W, doi:10.1086/345985, S2CID 1626564
  22. ^ Ritter, Andreas; Parker, Quentin A.; Lykou, Foteini; Zijlstra, Albert A.; Guerrero, Martín A. (1 September 2021), "The Remnant and Origin of the Historical Supernova 1181 AD", The Astrophysical Journal Letters (in German), 918 (2): L33, arXiv:2105.12384, Bibcode:2021ApJ...918L..33R, doi:10.3847/2041-8213/ac2253, hdl:10261/255617, ISSN 2041-8205, S2CID 235195784
  23. ^ Schaefer, Bradley E. (July 1995). "The Peak Brightness of SN 1895B in NGC 5253 and the Hubble Constant". Astrophysical Journal Letters. 447: L13. Bibcode:1995ApJ...447L..13S. doi:10.1086/309549. S2CID 227285055.
  24. ^ Dick, Steven J. (2019). Classifying the Cosmos: How We Can Make Sense of the Celestial Landscape. Springer International Publishing. p. 191. ISBN 9783030103804.
  25. ^ Osterbrock, D. E. (2001). "Who Coined the Word Supernova? Who First Predicted Neutron Stars?". Bulletin of the American Astronomical Society. 33: 1330. Bibcode:2001AAS...199.1501O.
  26. ^ Baade, Walter; Zwicky, Fritz (1934). "On Super-novae". Proceedings of the National Academy of Sciences. 20 (5): 254–259. Bibcode:1934PNAS...20..254B. doi:10.1073/pnas.20.5.254. PMC 1076395. PMID 16587881.
  27. ^ Murdin, P.; Murdin, L. (1985). Supernovae (2nd ed.). Cambridge University Press. p. 42. ISBN 978-0-521-30038-4.
  28. ^ da Silva, L. A. L. (1993). "The Classification of Supernovae". Astrophysics and Space Science. 202 (2): 215–236. Bibcode:1993Ap&SS.202..215D. doi:10.1007/BF00626878. S2CID 122727067.
  29. ^ Kowal, C. T. (1968). "Absolute magnitudes of supernovae". Astronomical Journal. 73: 1021–1024. Bibcode:1968AJ.....73.1021K. doi:10.1086/110763.
  30. ^ Leibundgut, B. (2003). "A cosmological surprise: The universe accelerates". Europhysics News. 32 (4): 121–125. Bibcode:2001ENews..32..121L. doi:10.1051/epn:2001401.
  31. ^ Fabian, A. C. (2008). "A Blast from the Past". Science. 320 (5880): 1167–1168. doi:10.1126/science.1158538. PMID 18511676. S2CID 206513073.
  32. ^ Aschenbach, B. (1998). "Discovery of a young nearby supernova remnant". Nature. 396 (6707): 141–142. Bibcode:1998Natur.396..141A. doi:10.1038/24103. S2CID 4426317.
  33. ^ Iyudin, A. F.; Schönfelder, V.; Bennett, K.; Bloemen, H.; Diehl, R.; Hermsen, W.; Lichti, G. G.; Van Der Meulen, R. D.; Ryan, J.; Winkler, C. (1998). "Emission from 44Ti associated with a previously unknown Galactic supernova". Nature. 396 (6707): 142–144. Bibcode:1998Natur.396..142I. doi:10.1038/24106. S2CID 4430526.
  34. ^ "NASA's Webb Opens New Window on Supernova Science - NASA Science". science.nasa.gov. Retrieved 11 June 2024.
  35. ^ Dong, Subo; Shappee, B. J.; Prieto, J. L.; Jha, S. W.; Stanek, K. Z.; Holoien, T. W. -S.; Kochanek, C. S.; Thompson, T. A.; Morrell, N.; Thompson, I. B.; Basu, U.; Beacom, J. F.; Bersier, D.; Brimacombe, J.; Brown, J. S.; Bufano, F.; Chen, Ping; Conseil, E.; Danilet, A. B.; Falco, E.; Grupe, D.; Kiyota, S.; Masi, G.; Nicholls, B.; Olivares E., F.; Pignata, G.; Pojmanski, G.; Simonian, G. V.; Szczygiel, D. M.; Woźniak, P. R. (2016). "ASASSN-15lh: A highly super-luminous supernova". Science. 351 (6270): 257–260. arXiv:1507.03010. Bibcode:2016Sci...351..257D. doi:10.1126/science.aac9613. PMID 26816375. S2CID 31444274.
  36. ^ Leloudas, G.; et al. (2016). "The superluminous transient ASASSN-15lh as a tidal disruption event from a Kerr black hole". Nature Astronomy. 1 (2): 0002. arXiv:1609.02927. Bibcode:2016NatAs...1E...2L. doi:10.1038/s41550-016-0002. S2CID 73645264.
  37. ^ Sample, I. (13 February 2017). "Massive supernova visible millions of light-years from Earth". The Guardian. Archived from the original on 13 February 2017. Retrieved 13 February 2017.
  38. ^ Yaron, O.; Perley, D. A.; Gal-Yam, A.; Groh, J. H.; Horesh, A.; Ofek, E. O.; Kulkarni, S. R.; Sollerman, J.; Fransson, C. (13 February 2017). "Confined dense circumstellar material surrounding a regular type II supernova". Nature Physics. 13 (5): 510–517. arXiv:1701.02596. Bibcode:2017NatPh..13..510Y. doi:10.1038/nphys4025. S2CID 29600801.
  39. ^ a b c Astronomy Now journalist (23 February 2018). "Amateur astronomer makes once-in-lifetime discovery". Astronomy Now. Archived from the original on 16 May 2018. Retrieved 15 May 2018.
  40. ^ Bersten, M. C.; Folatelli, G.; García, F.; Van Dyk, S. D.; Benvenuto, O. G.; Orellana, M.; Buso, V.; Sánchez, J. L.; Tanaka, M.; Maeda, K.; Filippenko, A. V.; Zheng, W.; Brink, T. G.; Cenko, S. B.; De Jaeger, T.; Kumar, S.; Moriya, T. J.; Nomoto, K.; Perley, D. A.; Shivvers, I.; Smith, N. (21 February 2018). "A surge of light at the birth of a supernova". Nature. 554 (7693): 497–499. arXiv:1802.09360. Bibcode:2018Natur.554..497B. doi:10.1038/nature25151. PMID 29469097. S2CID 4383303.
  41. ^ "James Webb Telescope Revolutionizes Supernova Research". www.jameswebbdiscovery.com. Retrieved 11 June 2024.
  42. ^ "NASA's Webb Opens New Window on Supernova Science - NASA Science". science.nasa.gov. Retrieved 11 June 2024.
  43. ^ Reynolds, S. P.; Borkowski, K. J.; Green, D. A.; Hwang, U.; Harrus, I. M.; Petre, R. (2008). "The Youngest Galactic Supernova Remnant: G1.9+0.3". The Astrophysical Journal Letters. 680 (1): L41–L44. arXiv:0803.1487. Bibcode:2008ApJ...680L..41R. doi:10.1086/589570. S2CID 67766657.
  44. ^ Colgate, S. A.; McKee, C. (1969). "Early Supernova Luminosity". The Astrophysical Journal. 157: 623. Bibcode:1969ApJ...157..623C. doi:10.1086/150102.
  45. ^ Zuckerman, B.; Malkan, M. A. (1996). The Origin and Evolution of the Universe. Jones & Bartlett Learning. p. 68. ISBN 978-0-7637-0030-0. Archived from the original on 20 August 2016.
  46. ^ Filippenko, A. V.; Li, W.-D.; Treffers, R. R.; Modjaz, M. (2001). "The Lick Observatory Supernova Search with the Katzman Automatic Imaging Telescope". In Paczynski, B.; Chen, W.-P.; Lemme, C. (eds.). Small Telescope Astronomy on Global Scale. ASP Conference Series. Vol. 246. San Francisco: Astronomical Society of the Pacific. p. 121. Bibcode:2001ASPC..246..121F. ISBN 978-1-58381-084-2.
  47. ^ a b Antonioli, P.; Fienberg, R. T.; Fleurot, F.; Fukuda, Y.; Fulgione, W.; Habig, A.; Heise, J.; McDonald, A. B.; Mills, C.; Namba, T.; Robinson, L. J.; Scholberg, K.; Schwendener, M.; Sinnott, R. W.; Stacey, B.; Suzuki, Y.; Tafirout, R.; Vigorito, C.; Viren, B.; Virtue, C.; Zichichi, A. (2004). "SNEWS: The SuperNova Early Warning System". New Journal of Physics. 6: 114. arXiv:astro-ph/0406214. Bibcode:2004NJPh....6..114A. doi:10.1088/1367-2630/6/1/114. S2CID 119431247.
  48. ^ Scholberg, K. (2000). "SNEWS: The supernova early warning system". AIP Conference Proceedings. 523: 355–361. arXiv:astro-ph/9911359. Bibcode:2000AIPC..523..355S. CiteSeerX 10.1.1.314.8663. doi:10.1063/1.1291879. S2CID 5803494.
  49. ^ Beacom, J. F. (1999). "Supernova neutrinos and the neutrino masses". Revista Mexicana de Fisica. 45 (2): 36. arXiv:hep-ph/9901300. Bibcode:1999RMxF...45...36B.
  50. ^ Frieman, J. A.; et al. (2008). "The Sloan Digital Sky Survey-Ii Supernova Survey: Technical Summary". The Astronomical Journal. 135 (1): 338–347. arXiv:0708.2749. Bibcode:2008AJ....135..338F. doi:10.1088/0004-6256/135/1/338. S2CID 53135988.
  51. ^ Perlmutter, S. A. (1997). "Scheduled discovery of 7+ high-redshift SNe: First cosmology results and bounds on q0". In Ruiz-Lapuente, P.; Canal, R.; Isern, J. (eds.). Thermonuclear Supernovae, Proceedings of the NATO Advanced Study Institute. NATO Advanced Science Institutes Series C. Vol. 486. Dordrecth: Kluwer Academic Publishers. p. 749. arXiv:astro-ph/9602122. Bibcode:1997ASIC..486..749P. doi:10.1007/978-94-011-5710-0_46.
  52. ^ Linder, E. V.; Huterer, D. (2003). "Importance of supernovae at z > 1.5 to probe dark energy". Physical Review D. 67 (8): 081303. arXiv:astro-ph/0208138. Bibcode:2003PhRvD..67h1303L. doi:10.1103/PhysRevD.67.081303. S2CID 8894913.
  53. ^ Perlmutter, S. A.; Gabi, S.; Goldhaber, G.; Goobar, A.; Groom, D. E.; Hook, I. M.; Kim, A. G.; Kim, M. Y.; Lee, J. C.; Pain, R.; Pennypacker, C. R.; Small, I. A.; Ellis, R. S.; McMahon, R. G.; Boyle, B. J.; Bunclark, P. S.; Carter, D.; Irwin, M. J.; Glazebrook, K.; Newberg, H. J. M.; Filippenko, A. V.; Matheson, T.; Dopita, M.; Couch, W. J. (1997). "Measurements of the Cosmological Parameters Ω and Λ from the First Seven Supernovae at z ≥ 0.35". The Astrophysical Journal. 483 (2): 565. arXiv:astro-ph/9608192. Bibcode:1997ApJ...483..565P. doi:10.1086/304265. S2CID 118187050.
  54. ^ Copin, Y.; Blanc, N.; Bongard, S.; Gangler, E.; Saugé, L.; Smadja, G.; Antilogus, P.; Garavini, G.; Gilles, S.; Pain, R.; Aldering, G.; Bailey, S.; Lee, B.C.; Loken, S.; Nugent, P. E.; Perlmutter, S. A.; Scalzo, R.; Thomas, R.C.; Wang, L.; Weaver, B.A.; Pécontal, E.; Kessler, R.; Baltay, C.; Rabinowitz, D.; Bauer, A. (2006). "The Nearby Supernova Factory" (PDF). New Astronomy Reviews. 50 (4–5): 637–640. arXiv:astro-ph/0401513. Bibcode:2006NewAR..50..436C. CiteSeerX 10.1.1.316.4895. doi:10.1016/j.newar.2006.02.035. Archived (PDF) from the original on 22 September 2017. Retrieved 25 October 2017.
  55. ^ Scolnic, D. M.; Jones, D. O.; Rest, A. (2018). "The Complete Light-curve Sample of Spectroscopically Confirmed SNe Ia from Pan-STARRS1 and Cosmological Constraints from the Combined Pantheon Sample". The Astrophysical Journal. 859 (2): 101. arXiv:1710.00845. Bibcode:2018ApJ...859..101S. doi:10.3847/1538-4357/aab9bb. S2CID 54676349.
  56. ^ Scolnic, D. M.; Brout, D.; Carr, A. (2021). "The Pantheon+ Analysis: The Full Dataset and Light-Curve Release". Astrophysical Journal Letters. 938 (2): 113. arXiv:2112.03863. Bibcode:2022ApJ...938..113S. doi:10.3847/1538-4357/ac8b7a. S2CID 246652657.
  57. ^ "What Kinds of Discovered Objects to Report for IAUC Publication". cbat.eps.harvard.edu. Retrieved 8 March 2023.
  58. ^ Kirshner, R. P. (1980). "Type I supernovae: An observer's view" (PDF). AIP Conference Proceedings. 63: 33–37. Bibcode:1980AIPC...63...33K. doi:10.1063/1.32212. hdl:2027.42/87614. Archived (PDF) from the original on 7 August 2020. Retrieved 20 March 2020.
  59. ^ "List of Supernovae". IAU Central Bureau for Astronomical Telegrams. Archived from the original on 12 November 2010. Retrieved 25 October 2010.
  60. ^ "The Padova-Asiago supernova catalogue". Osservatorio Astronomico di Padova. Archived from the original on 10 January 2014. Retrieved 10 January 2014.
  61. ^ Stephenson, F. Richard; Green, David A. (2002). Historical Supernovae and Their Remnants. Oxford: Clarendon Press. pp. 1–5, 60, 82. ISBN 0-19-850766-6. OCLC 50403827.
  62. ^ "Open Supernova Catalog". Archived from the original on 3 March 2016. Retrieved 5 February 2020.
  63. ^ Padova-Asiago Supernova Group, Asiago Supernova Catalogue, accessed 2023-12-27
  64. ^ a b Cappellaro, E.; Turatto, M. (2001). "The Influence of Binaries on Stellar Population Studies". Influence of Binaries on Stellar Population Studies. Astrophysics and Space Science Library. Vol. 264. Dordrecht: Kluwer Academic Publishers. p. 199. arXiv:astro-ph/0012455. Bibcode:2001ASSL..264..199C. doi:10.1007/978-94-015-9723-4_16. ISBN 978-0-7923-7104-5.
  65. ^ a b c d e f g h Turatto, M. (2003). "Classification of Supernovae". Supernovae and Gamma-Ray Bursters. Lecture Notes in Physics. Vol. 598. pp. 21–36. arXiv:astro-ph/0301107. CiteSeerX 10.1.1.256.2965. doi:10.1007/3-540-45863-8_3. ISBN 978-3-540-44053-6. S2CID 15171296.
  66. ^ a b c d e f g Doggett, J. B.; Branch, D. (1985). "A comparative study of supernova light curves". The Astronomical Journal. 90: 2303. Bibcode:1985AJ.....90.2303D. doi:10.1086/113934.
  67. ^ Foley, Ryan J.; Chornock, Ryan; Filippenko, Alexei V.; Ganeshalingam, Mohan; Kirshner, Robert P.; Li, Weidong; Cenko, S. Bradley; Challis, Peter J.; Friedman, Andrew S.; Modjaz, Maryam; Silverman, Jeffrey M.; Wood-Vasey, W. Michael (2009). "SN 2008ha: an extremely low luminosity and exceptionally low energy supernova". The Astronomical Journal. 138 (2): 376. arXiv:0902.2794. Bibcode:2009AJ....138..376F. doi:10.1088/0004-6256/138/2/376. S2CID 13855329.
  68. ^ Bianco, F. B.; Modjaz, M.; Hicken, M.; Friedman, A.; Kirshner, R. P.; Bloom, J. S.; Challis, P.; Marion, G. H.; Wood-Vasey, W. M.; Rest, A. (2014). "Multi-color Optical and Near-infrared Light Curves of 64 Stripped-envelope Core-Collapse Supernovae". The Astrophysical Journal Supplement. 213 (2): 19. arXiv:1405.1428. Bibcode:2014ApJS..213...19B. doi:10.1088/0067-0049/213/2/19. S2CID 119243970.
  69. ^ Lyman, J. D.; Levan, A. J.; James, P. A.; Angus, C. R.; Church, R. P.; Davies, M. B.; Tanvir, N. R. (11 May 2016). "Hubble Space Telescope observations of the host galaxies and environments of calcium-rich supernovae". Monthly Notices of the Royal Astronomical Society. 458 (2): 1768–1777. arXiv:1602.08098. doi:10.1093/mnras/stw477. ISSN 0035-8711.
  70. ^ Nugent, Peter (2 June 2017). "Supernovae: The explosion in a bubble". Nature Astronomy. 1 (6): 0140. Bibcode:2017NatAs...1E.140N. doi:10.1038/s41550-017-0140. ISSN 2397-3366. OSTI 1456969. S2CID 125998037.
  71. ^ a b Perets, H. B.; Gal-Yam, A.; Mazzali, P. A.; Arnett, D.; Kagan, D.; Filippenko, A. V.; Li, W.; Arcavi, I.; Cenko, S. B.; Fox, D. B.; Leonard, D. C.; Moon, D.-S.; Sand, D. J.; Soderberg, A. M.; Anderson, J. P.; James, P. A.; Foley, R. J.; Ganeshalingam, M.; Ofek, E. O.; Bildsten, L.; Nelemans, G.; Shen, K. J.; Weinberg, N. N.; Metzger, B. D.; Piro, A. L.; Quataert, E.; Kiewe, M.; Poznanski, D. (2010). "A faint type of supernova from a white dwarf with a helium-rich companion". Nature. 465 (7296): 322–325. arXiv:0906.2003. Bibcode:2010Natur.465..322P. doi:10.1038/nature09056. PMID 20485429. S2CID 4368207.
  72. ^ a b Barbon, R.; Ciatti, F.; Rosino, L. (1979). "Photometric properties of type II supernovae". Astronomy and Astrophysics. 72: 287. Bibcode:1979A&A....72..287B.
  73. ^ Filippenko, A. V. (1988). "Supernova 1987K: Type II in Youth, Type Ib in Old Age". The Astronomical Journal. 96: 1941. Bibcode:1988AJ.....96.1941F. doi:10.1086/114940.
  74. ^ Zwicky, F. (1964). "NGC 1058 and its Supernova 1961". The Astrophysical Journal. 139: 514. Bibcode:1964ApJ...139..514Z. doi:10.1086/147779.
  75. ^ Zwicky, F. (1962). "New Observations of Importance to Cosmology". In McVittie, G. C. (ed.). Problems of Extra-Galactic Research, Proceedings from IAU Symposium. Vol. 15. New York: Macmillan Press. p. 347. Bibcode:1962IAUS...15..347Z.
  76. ^ Filippenko, Alexei V. (September 1997). "Optical Spectra of Supernovae". Annual Review of Astronomy and Astrophysics. 35 (1): 309–355. Bibcode:1997ARA&A..35..309F. doi:10.1146/annurev.astro.35.1.309. ISSN 0066-4146. SN 1961V in NGC 1058 (Type V) had the most bizarre light curve ever recorded.
  77. ^ "The Rise and Fall of a Supernova". ESO Picture of the Week. Archived from the original on 2 July 2013. Retrieved 14 June 2013.
  78. ^ Piro, A. L.; Thompson, T. A.; Kochanek, C. S. (2014). "Reconciling 56Ni production in Type Ia supernovae with double degenerate scenarios". Monthly Notices of the Royal Astronomical Society. 438 (4): 3456. arXiv:1308.0334. Bibcode:2014MNRAS.438.3456P. doi:10.1093/mnras/stt2451. S2CID 27316605.
  79. ^ Chen, W.-C.; Li, X.-D. (2009). "On the Progenitors of Super-Chandrasekhar Mass Type Ia Supernovae". The Astrophysical Journal. 702 (1): 686–691. arXiv:0907.0057. Bibcode:2009ApJ...702..686C. doi:10.1088/0004-637X/702/1/686. S2CID 14301164.
  80. ^ Howell, D. A.; Sullivan, M.; Conley, A. J.; Carlberg, R. G. (2007). "Predicted and Observed Evolution in the Mean Properties of Type Ia Supernovae with Redshift". Astrophysical Journal Letters. 667 (1): L37–L40. arXiv:astro-ph/0701912. Bibcode:2007ApJ...667L..37H. doi:10.1086/522030. S2CID 16667595.
  81. ^ a b Mazzali, P. A.; Röpke, F. K.; Benetti, S.; Hillebrandt, W. (2007). "A Common Explosion Mechanism for Type Ia Supernovae". Science. 315 (5813): 825–828. arXiv:astro-ph/0702351. Bibcode:2007Sci...315..825M. doi:10.1126/science.1136259. PMID 17289993. S2CID 16408991.
  82. ^ Lieb, E. H.; Yau, H.-T. (1987). "A rigorous examination of the Chandrasekhar theory of stellar collapse". The Astrophysical Journal. 323 (1): 140–144. Bibcode:1987ApJ...323..140L. doi:10.1086/165813. Archived from the original on 3 March 2020. Retrieved 20 March 2020.
  83. ^ a b Canal, R.; Gutiérrez, J. L. (1997). "The possible white dwarf-neutron star connection". In Isern, J.; Hernanz, M.; Gracia-Berro, E. (eds.). White Dwarfs: Proceedings of the 10th European Workshop on White Dwarfs. Astrophysics and Space Science Library. Vol. 214. Dordrecht: Kluwer Academic Publishers. p. 49. arXiv:astro-ph/9701225. Bibcode:1997ASSL..214...49C. doi:10.1007/978-94-011-5542-7_7. ISBN 978-0-7923-4585-5. S2CID 9288287.
  84. ^ Wheeler, J. C. (2000). Cosmic Catastrophes: Supernovae, Gamma-Ray Bursts, and Adventures in Hyperspace. Cambridge University Press. p. 96. ISBN 978-0-521-65195-0. Archived from the original on 10 September 2015.
  85. ^ Khokhlov, A. M.; Mueller, E.; Höflich, P. A. (1993). "Light curves of Type IA supernova models with different explosion mechanisms". Astronomy and Astrophysics. 270 (1–2): 223–248. Bibcode:1993A&A...270..223K.
  86. ^ Röpke, F. K.; Hillebrandt, W. (2004). "The case against the progenitor's carbon-to-oxygen ratio as a source of peak luminosity variations in type Ia supernovae". Astronomy and Astrophysics Letters. 420 (1): L1–L4. arXiv:astro-ph/0403509. Bibcode:2004A&A...420L...1R. doi:10.1051/0004-6361:20040135. S2CID 2849060.
  87. ^ a b c d Hillebrandt, W.; Niemeyer, J. C. (2000). "Type IA Supernova Explosion Models". Annual Review of Astronomy and Astrophysics. 38 (1): 191–230. arXiv:astro-ph/0006305. Bibcode:2000ARA&A..38..191H. doi:10.1146/annurev.astro.38.1.191. S2CID 10210550.
  88. ^ Paczyński, B. (1976). "Common Envelope Binaries". In Eggleton, P.; Mitton, S.; Whelan, J. (eds.). Structure and Evolution of Close Binary Systems. IAU Symposium No. 73. Dordrecht: D. Reidel. pp. 75–80. Bibcode:1976IAUS...73...75P.
  89. ^ Poludnenko, Alexei Y.; Chambers, Jessica; Ahmed, Kareem; Gamezo, Vadim N.; Taylor, Brian D. (November 2019). "A unified mechanism for unconfined deflagration-to-detonation transition in terrestrial chemical systems and type Ia supernovae". Science. 366 (6465): eaau7365. arXiv:1911.00050. Bibcode:2019Sci...366.7365P. doi:10.1126/science.aau7365. ISSN 0036-8075. PMID 31672866. S2CID 207817150. Theoretical models of SNIa have remained limited because of uncertainties in the explosion mechanisms. [...] SNIa explosions are driven by fast thermonuclear burning in 12C/16O white dwarf (WD) stars with a mass close to, or below, the Chandrasekhar mass limit of ≈1.4 solar masses [...] Beyond this general statement, however, the exact mechanisms of SNIa remain unclear, with a number of possible scenarios.
  90. ^ Macri, L. M.; Stanek, K. Z.; Bersier, D.; Greenhill, L. J.; Reid, M. J. (2006). "A New Cepheid Distance to the Maser-Host Galaxy NGC 4258 and Its Implications for the Hubble Constant". The Astrophysical Journal. 652 (2): 1133–1149. arXiv:astro-ph/0608211. Bibcode:2006ApJ...652.1133M. doi:10.1086/508530. S2CID 15728812.
  91. ^ Colgate, S. A. (1979). "Supernovae as a standard candle for cosmology". The Astrophysical Journal. 232 (1): 404–408. Bibcode:1979ApJ...232..404C. doi:10.1086/157300.
  92. ^ Ruiz-Lapuente, P.; Blinnikov, S.; Canal, R.; Mendez, J.; Sorokina, E.; Visco, A.; Walton, N. (2000). "Type IA supernova progenitors". Memorie della Societa Astronomica Italiana. 71: 435. Bibcode:2000MmSAI..71..435R.
  93. ^ Dan, M.; Rosswog, S.; Guillochon, J.; Ramirez-Ruiz, E. (2012). "How the merger of two white dwarfs depends on their mass ratio: Orbital stability and detonations at contact". Monthly Notices of the Royal Astronomical Society. 422 (3): 2417. arXiv:1201.2406. Bibcode:2012MNRAS.422.2417D. doi:10.1111/j.1365-2966.2012.20794.x. S2CID 119159904.
  94. ^ Maoz, Dan; Mannucci, Filippo; Nelemans, Gijs (18 August 2014). "Observational Clues to the Progenitors of Type Ia Supernovae". Annual Review of Astronomy and Astrophysics. 52 (1): 107–170. arXiv:1312.0628. Bibcode:2014ARA&A..52..107M. doi:10.1146/annurev-astro-082812-141031. ISSN 0066-4146. S2CID 55533680.
  95. ^ Howell, D. A.; Sullivan, M.; Nugent, P. E.; Ellis, R. S.; Conley, A. J.; Le Borgne, D.; Carlberg, R. G.; Guy, J.; Balam, D.; Basa, S.; Fouchez, D.; Hook, I. M.; Hsiao, E. Y.; Neill, J. D.; Pain, R.; Perrett, K. M.; Pritchet, C. J. (2006). "The type Ia supernova SNLS-03D3bb from a super-Chandrasekhar-mass white dwarf star". Nature. 443 (7109): 308–311. arXiv:astro-ph/0609616. Bibcode:2006Natur.443..308H. doi:10.1038/nature05103. PMID 16988705. S2CID 4419069.
  96. ^ Tanaka, M.; Kawabata, K. S.; Yamanaka, M.; Maeda, K.; Hattori, T.; Aoki, K.; Nomoto, K. I.; Iye, M.; Sasaki, T.; Mazzali, P. A.; Pian, E. (2010). "Spectropolarimetry of Extremely Luminous Type Ia Supernova 2009dc: Nearly Spherical Explosion of Super-Chandrasekhar Mass White Dwarf". The Astrophysical Journal. 714 (2): 1209. arXiv:0908.2057. Bibcode:2010ApJ...714.1209T. doi:10.1088/0004-637X/714/2/1209. S2CID 13990681.
  97. ^ Fink, M.; Kromer, M.; Hillebrandt, W.; Röpke, F. K.; Pakmor, R.; Seitenzahl, I. R.; Sim, S. A. (October 2018). "Thermonuclear explosions of rapidly differentially rotating white dwarfs: Candidates for superluminous Type Ia supernovae?". Astronomy & Astrophysics. 618: A124. arXiv:1807.10199. Bibcode:2018A&A...618A.124F. doi:10.1051/0004-6361/201833475. S2CID 118965737. A124.
  98. ^ Wang, B.; Liu, D.; Jia, S.; Han, Z. (2014). "Helium double-detonation explosions for the progenitors of type Ia supernovae". Proceedings of the International Astronomical Union. 9 (S298): 442. arXiv:1301.1047. Bibcode:2014IAUS..298..442W. doi:10.1017/S1743921313007072. S2CID 118612081.
  99. ^ Foley, R. J.; Challis, P. J.; Chornock, R.; Ganeshalingam, M.; Li, W.; Marion, G. H.; Morrell, N. I.; Pignata, G.; Stritzinger, M. D.; Silverman, J. M.; Wang, X.; Anderson, J. P.; Filippenko, A. V.; Freedman, W. L.; Hamuy, M.; Jha, S. W.; Kirshner, R. P.; McCully, C.; Persson, S. E.; Phillips, M. M.; Reichart, D. E.; Soderberg, A. M. (2013). "Type Iax Supernovae: A New Class of Stellar Explosion". The Astrophysical Journal. 767 (1): 57. arXiv:1212.2209. Bibcode:2013ApJ...767...57F. doi:10.1088/0004-637X/767/1/57. S2CID 118603977.
  100. ^ McCully, C.; Jha, S. W.; Foley, R. J.; Bildsten, L.; Fong, W.-F.; Kirshner, R. P.; Marion, G. H.; Riess, A. G.; Stritzinger, M. D. (2014). "A luminous, blue progenitor system for the type Iax supernova 2012Z". Nature. 512 (7512): 54–56. arXiv:1408.1089. Bibcode:2014Natur.512...54M. doi:10.1038/nature13615. PMID 25100479. S2CID 4464556.
  101. ^ Silverman, J. M.; Nugent, P. E.; Gal-Yam, A.; Sullivan, M.; Howell, D. A.; Filippenko, A. V.; Arcavi, I.; Ben-Ami, S.; Bloom, J. S.; Cenko, S. B.; Cao, Y.; Chornock, R.; Clubb, K. I.; Coil, A. L.; Foley, R. J.; Graham, M. L.; Griffith, C. V.; Horesh, A.; Kasliwal, M. M.; Kulkarni, S. R.; Leonard, D. C.; Li, W.; Matheson, T.; Miller, A. A.; Modjaz, M.; Ofek, E. O.; Pan, Y.-C.; Perley, D. A.; Poznanski, D.; Quimby, R. M. (2013). "Type Ia Supernovae strongly interaction with their circumstellar medium". The Astrophysical Journal Supplement Series. 207 (1): 3. arXiv:1304.0763. Bibcode:2013ApJS..207....3S. doi:10.1088/0067-0049/207/1/3. S2CID 51415846.
  102. ^ Gilmore, Gerry; Randich, Sofia (March 2012). "The Gaia-ESO Public Spectroscopic Survey". The Messenger. 147 (147). Garching, Germany: European Southern Observatory: 25–31. Bibcode:2012Msngr.147...25G.
  103. ^ Merle, Thibault; Hamers, Adrian S.; Van Eck, Sophie; Jorissen, Alain; Van der Swaelmen, Mathieu; Pollard, Karen; Smiljanic, Rodolfo; Pourbaix, Dimitri; Zwitter, Tomaž; Traven, Gregor; Gilmore, Gerry; Randich, Sofia; Gonneau, Anaïs; Hourihane, Anna; Sacco, Germano; Worley, C. Clare (12 May 2022). "A spectroscopic quadruple as a possible progenitor of sub-Chandrasekhar type Ia supernovae". Nature Astronomy. 6 (6): 681–688. arXiv:2205.05045. Bibcode:2022NatAs...6..681M. doi:10.1038/s41550-022-01664-5. S2CID 248665714.
  104. ^ a b c d e f g h Heger, A.; Fryer, C. L.; Woosley, S. E.; Langer, N.; Hartmann, D. H. (2003). "How Massive Single Stars End Their Life". Astrophysical Journal. 591 (1): 288–300. arXiv:astro-ph/0212469. Bibcode:2003ApJ...591..288H. doi:10.1086/375341. S2CID 59065632.
  105. ^ a b c Renzo, M.; Farmer, R.; Justham, S.; Götberg, Y.; De Mink, S. E.; Zapartas, E.; Marchant, P.; Smith, N. (2020). "Predictions for the hydrogen-free ejecta of pulsational pair-instability supernovae". Astronomy and Astrophysics. 640: A56. arXiv:2002.05077. Bibcode:2020A&A...640A..56R. doi:10.1051/0004-6361/202037710. S2CID 211082844.
  106. ^ Nomoto, K.; Tanaka, M.; Tominaga, N.; Maeda, K. (2010). "Hypernovae, gamma-ray bursts, and first stars". New Astronomy Reviews. 54 (3–6): 191. Bibcode:2010NewAR..54..191N. doi:10.1016/j.newar.2010.09.022.
  107. ^ Moriya, T. J. (2012). "Progenitors of Recombining Supernova Remnants". The Astrophysical Journal. 750 (1): L13. arXiv:1203.5799. Bibcode:2012ApJ...750L..13M. doi:10.1088/2041-8205/750/1/L13. S2CID 119209527.
  108. ^ Smith, N.; Ganeshalingam, M.; Chornock, R.; Filippenko, A. V.; Li, W.; Silverman, J. M.; Steele, T. N.; Griffith, C. V.; Joubert, N.; Lee, N. Y.; Lowe, T. B.; Mobberley, M. P.; Winslow, D. M. (2009). "Sn 2008S: A Cool Super-Eddington Wind in a Supernova Impostor". The Astrophysical Journal. 697 (1): L49. arXiv:0811.3929. Bibcode:2009ApJ...697L..49S. doi:10.1088/0004-637X/697/1/L49. S2CID 17627678.
  109. ^ a b c d Janka, H.-T.; Langanke, K.; Marek, A.; Martínez-Pinedo, G.; Müller, B. (2007). "Theory of core-collapse supernovae". Physics Reports. 442 (1–6): 38–74. arXiv:astro-ph/0612072. Bibcode:2007PhR...442...38J. doi:10.1016/j.physrep.2007.02.002. S2CID 15819376.
  110. ^ Fryer, C. L.; New, K. C. B. (2003). "Gravitational Waves from Gravitational Collapse". Living Reviews in Relativity. 6 (1): 2. arXiv:gr-qc/0206041. Bibcode:2003LRR.....6....2F. doi:10.12942/lrr-2003-2. PMC 5253977. PMID 28163639.
  111. ^ a b Hurley, J. R.; Pols, O. R.; Tout, C. A. (1 July 2000). "Comprehensive analytic formulae for stellar evolution as a function of mass and metallicity". Monthly Notices of the Royal Astronomical Society. 315 (3): 543–569. arXiv:astro-ph/0001295. Bibcode:2000MNRAS.315..543H. doi:10.1046/j.1365-8711.2000.03426.x. ISSN 0035-8711.
  112. ^ a b c d Woosley, S. E.; Janka, H.-T. (2005). "The Physics of Core-Collapse Supernovae". Nature Physics. 1 (3): 147–154. arXiv:astro-ph/0601261. Bibcode:2005NatPh...1..147W. CiteSeerX 10.1.1.336.2176. doi:10.1038/nphys172. S2CID 118974639.
  113. ^ Gribbin, J. R.; Gribbin, M. (2000). Stardust: Supernovae and Life – The Cosmic Connection. Yale University Press. p. 173. Bibcode:2000sslc.book.....G. ISBN 978-0-300-09097-0.
  114. ^ a b Barwick, S. W; Beacom, J. F; Cianciolo, V.; Dodelson, S.; Feng, J. L; Fuller, G. M; Kaplinghat, M.; McKay, D. W; Meszaros, P.; Mezzacappa, A.; Murayama, H.; Olive, K. A; Stanev, T.; Walker, T. P (2004). "APS Neutrino Study: Report of the Neutrino Astrophysics and Cosmology Working Group". arXiv:astro-ph/0412544.
  115. ^ Myra, E. S.; Burrows, A. (1990). "Neutrinos from type II supernovae- The first 100 milliseconds". Astrophysical Journal. 364: 222–231. Bibcode:1990ApJ...364..222M. doi:10.1086/169405.
  116. ^ a b Piran, Tsvi; Nakar, Ehud; Mazzali, Paolo; Pian, Elena (2019). "Relativistic Jets in Core-collapse Supernovae". The Astrophysical Journal. 871 (2): L25. arXiv:1704.08298. Bibcode:2019ApJ...871L..25P. doi:10.3847/2041-8213/aaffce. S2CID 19266567.
  117. ^ a b Kasen, D.; Woosley, S. E.; Heger, A. (2011). "Pair Instability Supernovae: Light Curves, Spectra, and Shock Breakout". The Astrophysical Journal. 734 (2): 102. arXiv:1101.3336. Bibcode:2011ApJ...734..102K. doi:10.1088/0004-637X/734/2/102. S2CID 118508934.
  118. ^ a b Poelarends, A. J. T.; Herwig, F.; Langer, N.; Heger, A. (2008). "The Supernova Channel of Super-AGB Stars". The Astrophysical Journal. 675 (1): 614–625. arXiv:0705.4643. Bibcode:2008ApJ...675..614P. doi:10.1086/520872. S2CID 18334243.
  119. ^ Gilmore, G. (2004). "The Short Spectacular Life of a Superstar". Science. 304 (5679): 1915–1916. doi:10.1126/science.1100370. PMID 15218132. S2CID 116987470.
  120. ^ Faure, G.; Mensing, T. M. (2007). "Life and Death of Stars". Introduction to Planetary Science. pp. 35–48. doi:10.1007/978-1-4020-5544-7_4. ISBN 978-1-4020-5233-0.
  121. ^ a b Horiuchi, S.; Nakamura, K.; Takiwaki, T.; Kotake, K.; Tanaka, M. (2014). "The red supergiant and supernova rate problems: Implications for core-collapse supernova physics". Monthly Notices of the Royal Astronomical Society: Letters. 445: L99–L103. arXiv:1409.0006. Bibcode:2014MNRAS.445L..99H. doi:10.1093/mnrasl/slu146.
  122. ^ Faran, T.; Poznanski, D.; Filippenko, A. V.; Chornock, R.; Foley, R. J.; Ganeshalingam, M.; Leonard, D. C.; Li, W.; Modjaz, M.; Serduke, F. J. D.; Silverman, J. M. (2014). "A sample of Type II-L supernovae". Monthly Notices of the Royal Astronomical Society. 445 (1): 554–569. arXiv:1409.1536. Bibcode:2014MNRAS.445..554F. doi:10.1093/mnras/stu1760.
  123. ^ Farmer, R.; Renzo, M.; de Mink, S. E.; Marchant, P.; Justham, S. (2019). "Mind the Gap: The Location of the Lower Edge of the Pair-instability Supernova Black Hole Mass Gap". The Astrophysical Journal. 887 (1): 53. arXiv:1910.12874. Bibcode:2019ApJ...887...53F. doi:10.3847/1538-4357/ab518b.
  124. ^ Malesani, D.; Fynbo, J. P. U.; Hjorth, J.; Leloudas, G.; Sollerman, J.; Stritzinger, M. D.; Vreeswijk, P. M.; Watson, D. J.; Gorosabel, J.; Michałowski, M. J.; Thöne, C. C.; Augusteijn, T.; Bersier, D.; Jakobsson, P.; Jaunsen, A. O.; Ledoux, C.; Levan, A. J.; Milvang-Jensen, B.; Rol, E.; Tanvir, N. R.; Wiersema, K.; Xu, D.; Albert, L.; Bayliss, M. B.; Gall, C.; Grove, L. F.; Koester, B. P.; Leitet, E.; Pursimo, T.; Skillen, I. (2009). "Early Spectroscopic Identification of SN 2008D". The Astrophysical Journal Letters. 692 (2): L84. arXiv:0805.1188. Bibcode:2009ApJ...692L..84M. doi:10.1088/0004-637X/692/2/L84. S2CID 1435322.
  125. ^ Svirski, G.; Nakar, E. (2014). "Sn 2008D: A Wolf-Rayet Explosion Through a Thick Wind". The Astrophysical Journal. 788 (1): L14. arXiv:1403.3400. Bibcode:2014ApJ...788L..14S. doi:10.1088/2041-8205/788/1/L14. S2CID 118395580.
  126. ^ Pols, O. (1997). "Close Binary Progenitors of Type Ib/Ic and IIb/II-L Supernovae". In Leung, K.-C. (ed.). Proceedings of the Third Pacific Rim Conference on Recent Development on Binary Star Research. ASP Conference Series. Vol. 130. pp. 153–158. Bibcode:1997ASPC..130..153P.
  127. ^ a b c Eldridge, J. J.; Fraser, M.; Smartt, S. J.; Maund, J. R.; Crockett, R. Mark (2013). "The death of massive stars – II. Observational constraints on the progenitors of Type Ibc supernovae". Monthly Notices of the Royal Astronomical Society. 436 (1): 774. arXiv:1301.1975. Bibcode:2013MNRAS.436..774E. doi:10.1093/mnras/stt1612. S2CID 118535155.
  128. ^ Yoon, Sung-Chul (2017). "Towards a better understanding of the evolution of Wolf–Rayet stars and Type Ib/Ic supernova progenitors". Monthly Notices of the Royal Astronomical Society. 470 (4): 3970–3980. arXiv:1706.04716. Bibcode:2017MNRAS.470.3970Y. doi:10.1093/mnras/stx1496.
  129. ^ Ryder, S. D.; Sadler, E. M.; Subrahmanyan, R.; Weiler, K. W.; Panagia, N.; Stockdale, C. J. (2004). "Modulations in the radio light curve of the Type IIb supernova 2001ig: evidence for a Wolf-Rayet binary progenitor?". Monthly Notices of the Royal Astronomical Society. 349 (3): 1093–1100. arXiv:astro-ph/0401135. Bibcode:2004MNRAS.349.1093R. doi:10.1111/j.1365-2966.2004.07589.x. S2CID 18132819.
  130. ^ Inserra, C.; Smartt, S. J.; Jerkstrand, A.; Valenti, S.; Fraser, M.; Wright, D.; Smith, K.; Chen, T.-W.; Kotak, R.; Pastorello, A.; Nicholl, M.; Bresolin, S. F.; Kudritzki, R. P.; Benetti, S.; Botticella, M. T.; Burgett, W. S.; Chambers, K. C.; Ergon, M.; Flewelling, H.; Fynbo, J. P. U.; Geier, S.; Hodapp, K. W.; Howell, D. A.; Huber, M.; Kaiser, N.; Leloudas, G.; Magill, L.; Magnier, E. A.; McCrum, M. G.; Metcalfe, N.; Price, P. A.; Rest, A.; Sollerman, J.; Sweeney, W.; Taddia, F.; Taubenberger, S.; Tonry, J. L.; Wainscoat, R. J.; Waters, C.; Young, D. (2013). "Super-luminous Type Ic Supernovae: Catching a Magnetar by the Tail". The Astrophysical Journal. 770 (2): 28. arXiv:1304.3320. Bibcode:2013ApJ...770..128I. doi:10.1088/0004-637X/770/2/128. S2CID 13122542.
  131. ^ Nicholl, M.; Smartt, S. J.; Jerkstrand, A.; Inserra, C.; McCrum, M.; Kotak, R.; Fraser, M.; Wright, D.; Chen, T. W.; Smith, K.; Young, D. R.; Sim, S. A.; Valenti, S.; Howell, D. A.; Bresolin, F.; Kudritzki, R. P.; Tonry, J. L.; Huber, M. E.; Rest, A.; Pastorello, A.; Tomasella, L.; Cappellaro, E.; Benetti, S.; Mattila, S.; Kankare, E.; Kangas, T.; Leloudas, G.; Sollerman, J.; Taddia, F.; Berger, E. (2013). "Slowly fading super-luminous supernovae that are not pair-instability explosions". Nature. 502 (7471): 346–349. arXiv:1310.4446. Bibcode:2013Natur.502..346N. doi:10.1038/nature12569. PMID 24132291. S2CID 4472977.
  132. ^ Tauris, T. M.; Langer, N.; Moriya, T. J.; Podsiadlowski, P.; Yoon, S.-C.; Blinnikov, S. I. (2013). "Ultra-stripped Type Ic supernovae from close binary evolution". Astrophysical Journal Letters. 778 (2): L23. arXiv:1310.6356. Bibcode:2013ApJ...778L..23T. doi:10.1088/2041-8205/778/2/L23. S2CID 50835291.
  133. ^ Tauris, Thomas M.; Langer, Norbert; Podsiadlowski, Philipp (11 June 2015). "Ultra-stripped supernovae: progenitors and fate". Monthly Notices of the Royal Astronomical Society. 451 (2): 2123–2144. arXiv:1505.00270. Bibcode:2015MNRAS.451.2123T. doi:10.1093/mnras/stv990. eISSN 1365-2966. ISSN 0035-8711.
  134. ^ Drout, M. R.; Soderberg, A. M.; Mazzali, P. A.; Parrent, J. T.; Margutti, R.; Milisavljevic, D.; Sanders, N. E.; Chornock, R.; Foley, R. J.; Kirshner, R. P.; Filippenko, A. V.; Li, W.; Brown, P. J.; Cenko, S. B.; Chakraborti, S.; Challis, P.; Friedman, A.; Ganeshalingam, M.; Hicken, M.; Jensen, C.; Modjaz, M.; Perets, H. B.; Silverman, J. M.; Wong, D. S. (2013). "The Fast and Furious Decay of the Peculiar Type Ic Supernova 2005ek". Astrophysical Journal. 774 (58): 44. arXiv:1306.2337. Bibcode:2013ApJ...774...58D. doi:10.1088/0004-637X/774/1/58. S2CID 118690361.
  135. ^ Tauris, T. M.; Kramer, M.; Freire, P. C. C.; Wex, N.; Janka, H.-T.; Langer, N.; Podsiadlowski, Ph.; Bozzo, E.; Chaty, S.; Kruckow, M. U.; Heuvel, E. P. J. van den; Antoniadis, J.; Breton, R. P.; Champion, D. J. (13 September 2017). "Formation of Double Neutron Star Systems". The Astrophysical Journal. 846 (2): 170. arXiv:1706.09438. Bibcode:2017ApJ...846..170T. doi:10.3847/1538-4357/aa7e89. eISSN 1538-4357. S2CID 119471204.
  136. ^ De, K.; Kasliwal, M. M.; Ofek, E. O.; Moriya, T. J.; Burke, J.; Cao, Y.; Cenko, S. B.; Doran, G. B.; Duggan, G. E.; Fender, R. P.; Fransson, C.; Gal-Yam, A.; Horesh, A.; Kulkarni, S. R.; Laher, R. R.; Lunnan, R.; Manulis, I.; Masci, F.; Mazzali, P. A.; Nugent, P. E.; Perley, D. A.; Petrushevska, T.; Piro, A. L.; Rumsey, C.; Sollerman, J.; Sullivan, M.; Taddia, F. (12 October 2018). "A hot and fast ultra-stripped supernova that likely formed a compact neutron star binary". Science. 362 (6411): 201–206. arXiv:1810.05181. Bibcode:2018Sci...362..201D. doi:10.1126/science.aas8693. eISSN 1095-9203. ISSN 0036-8075. PMID 30309948. S2CID 52961306.
  137. ^ Gal-Yam, A.; Bruch, R.; Schulze, S.; Yang, Y.; Perley, D. A.; Irani, I.; Sollerman, J.; Kool, E. C.; Soumagnac, M. T.; Yaron, O.; Strotjohann, N. L.; Zimmerman, E.; Barbarino, C.; Kulkarni, S. R.; Kasliwal, M. M.; De, K.; Yao, Y.; Fremling, C.; Yan, L.; Ofek, E. O.; Fransson, C.; Filippenko, A. V.; Zheng, W.; Brink, T. G.; Copperwheat, C. M.; Foley, R. J.; Brown, J.; Siebert, M.; Leloudas, G.; Cabrera-Lavers, A. L. (2022). "A WC/WO star exploding within an expanding carbon–oxygen–neon nebula". Nature. 601 (7892): 201–204. arXiv:2111.12435. Bibcode:2022Natur.601..201G. doi:10.1038/s41586-021-04155-1. PMID 35022591. S2CID 244527654.
  138. ^ "Astronomers discover first supernova explosion of a Wolf-Rayet star". Instituto de Astrofísica de Canarias • IAC. 12 January 2022. Retrieved 9 February 2022.
  139. ^ a b Hiramatsu D; Howell D; Van S; et al. (28 June 2021). "The electron-capture origin of supernova 2018zd". Nat Astron. 5 (9): 903–910. arXiv:2011.02176. Bibcode:2021NatAs...5..903H. doi:10.1038/s41550-021-01384-2. S2CID 226246044. Archived from the original on 30 June 2021. Retrieved 1 July 2021.
  140. ^ a b c "New, Third Type Of Supernova Observed". W. M. Keck Observatory. 28 June 2021. Archived from the original on 29 June 2021. Retrieved 1 July 2021.
  141. ^ a b c "Astronomers discover new type of supernova". RTE News. PA. 28 June 2021. Archived from the original on 30 June 2021. Retrieved 1 July 2021. In 1980, Ken'ichi Nomoto of the University of Tokyo predicted a third type called an electron capture supernova. ... In an electron capture supernova, as the core runs out of fuel, gravity forces electrons in the core into their atomic nuclei, causing the star to collapse in on itself.
  142. ^ Reynolds, T. M.; Fraser, M.; Gilmore, G. (2015). "Gone without a bang: an archival HST survey for disappearing massive stars". Monthly Notices of the Royal Astronomical Society. 453 (3): 2886–2901. arXiv:1507.05823. Bibcode:2015MNRAS.453.2885R. doi:10.1093/mnras/stv1809. S2CID 119116538.
  143. ^ Gerke, J. R.; Kochanek, C. S.; Stanek, K. Z. (2015). "The search for failed supernovae with the Large Binocular Telescope: first candidates". Monthly Notices of the Royal Astronomical Society. 450 (3): 3289–3305. arXiv:1411.1761. Bibcode:2015MNRAS.450.3289G. doi:10.1093/mnras/stv776. S2CID 119212331.
  144. ^ a b Adams, S. M.; Kochanek, C. S.; Beacom, J. F.; Vagins, M. R.; Stanek, K. Z. (2013). "Observing the Next Galactic Supernova". The Astrophysical Journal. 778 (2): 164. arXiv:1306.0559. Bibcode:2013ApJ...778..164A. doi:10.1088/0004-637X/778/2/164. S2CID 119292900.
  145. ^ a b Karttunen, H.; Kröger, P.; Oja, H.; Poutanen, M.; Donner, K. J., eds. (2016). Fundamental Astronomy. Springer. p. 309. ISBN 978-3-662-53044-3.
  146. ^ a b Modjaz, M.; Gutiérrez, C. P.; Arcavi, I. (August 2019). "New regimes in the observation of core-collapse supernovae". Nature Astronomy. 3 (8): 717–724. arXiv:1908.02476. Bibcode:2019NatAs...3..717M. doi:10.1038/s41550-019-0856-2. S2CID 199472802.
  147. ^ a b Nyholm, A.; et al. (2020). "Type IIn supernova light-curve properties measured from an untargeted survey sample". Astronomy and Astrophysics. 637: A73. arXiv:1906.05812. Bibcode:2020A&A...637A..73N. doi:10.1051/0004-6361/201936097. S2CID 189762490.
  148. ^ Michel, F. Curtis; Kennel, C. F.; Fowler, William A. (13 November 1987). "When Will a Pulsar in Supernova 1987a Be Seen?". Science. 238 (4829): 938–940. Bibcode:1987Sci...238..938M. doi:10.1126/science.238.4829.938. PMID 17829358. S2CID 46408677.
  149. ^ Bodansky, D.; Clayton, D. D.; Fowler, W. A. (1968). "Nucleosynthesis During Silicon Burning". Physical Review Letters. 20 (4): 161. Bibcode:1968PhRvL..20..161B. doi:10.1103/PhysRevLett.20.161. Archived from the original on 13 February 2020. Retrieved 16 June 2019.
  150. ^ a b Matz, S. M.; Share, G. H.; Leising, M. D.; Chupp, E. L.; Vestrand, W. T.; Purcell, W.R.; Strickman, M.S.; Reppin, C. (1988). "Gamma-ray line emission from SN1987A". Nature. 331 (6155): 416. Bibcode:1988Natur.331..416M. doi:10.1038/331416a0. S2CID 4313713.
  151. ^ Kasen, D.; Woosley, S. E. (2009). "Type Ii Supernovae: Model Light Curves and Standard Candle Relationships". The Astrophysical Journal. 703 (2): 2205. arXiv:0910.1590. Bibcode:2009ApJ...703.2205K. doi:10.1088/0004-637X/703/2/2205. S2CID 42058638.
  152. ^ Nagy, A. P.; Vinkó, J. (2016). "A two-component model for fitting light curves of core-collapse supernovae". Astronomy & Astrophysics. 589: A53. arXiv:1602.04001. Bibcode:2016A&A...589A..53N. doi:10.1051/0004-6361/201527931. S2CID 53380594.
  153. ^ Tominaga, N.; Blinnikov, S.; Baklanov, P.; Morokuma, T.; Nomoto, K.; Suzuki, T. (1 November 2009). "Properties of Type II Plateau Supernova SNLS-04D2dc: Multicolor Light Curves of Shock Breakout and Plateau". The Astrophysical Journal. 705 (1): L10–L14. arXiv:0908.2162. Bibcode:2009ApJ...705L..10T. doi:10.1088/0004-637X/705/1/L10. ISSN 0004-637X.
  154. ^ de la Rosa, Janie; Roming, Pete; Pritchard, Tyler; Fryer, Chris (22 March 2016). "Characterizing Mid-Ultraviolet to Optical Light Curves of Nearby Type IIn Supernovae". The Astrophysical Journal. 820 (1): 74. Bibcode:2016ApJ...820...74D. doi:10.3847/0004-637X/820/1/74. ISSN 1538-4357.
  155. ^ Churazov, E.; Sunyaev, R.; Isern, J.; Knödlseder, J.; Jean, P.; Lebrun, F.; Chugai, N.; Grebenev, S.; Bravo, E.; Sazonov, S.; Renaud, M. (2014). "Cobalt-56 γ-ray emission lines from the Type Ia supernova 2014J". Nature. 512 (7515): 406–8. arXiv:1405.3332. Bibcode:2014Natur.512..406C. doi:10.1038/nature13672. PMID 25164750. S2CID 917374.
  156. ^ Seitenzahl, I. R.; Taubenberger, S.; Sim, S. A. (2009). "Late-time supernova light curves: The effect of internal conversion and Auger electrons". Monthly Notices of the Royal Astronomical Society. 400 (1): 531–535. arXiv:0908.0247. Bibcode:2009MNRAS.400..531S. doi:10.1111/j.1365-2966.2009.15478.x. S2CID 10283901.
  157. ^ Tsvetkov, D. Yu. (1987). "Light curves of type Ib supernova: SN 1984l in NGC 991". Soviet Astronomy Letters. 13: 376–378. Bibcode:1987SvAL...13..376T.
  158. ^ a b Filippenko, A.V. (2004). "Supernovae and Their Massive Star Progenitors". The Fate of the Most Massive Stars. 332: 34. arXiv:astro-ph/0412029. Bibcode:2005ASPC..332...33F.
  159. ^ Filippenko, A. V. (1997). "Optical Spectra of Supernovae". Annual Review of Astronomy and Astrophysics. 35: 309–355. Bibcode:1997ARA&A..35..309F. doi:10.1146/annurev.astro.35.1.309.
  160. ^ Pastorello, A.; Turatto, M.; Benetti, S.; Cappellaro, E.; Danziger, I. J.; Mazzali, P. A.; Patat, F.; Filippenko, A. V.; Schlegel, D. J.; Matheson, T. (2002). "The type IIn supernova 1995G: interaction with the circumstellar medium". Monthly Notices of the Royal Astronomical Society. 333 (1): 27–38. arXiv:astro-ph/0201483. Bibcode:2002MNRAS.333...27P. doi:10.1046/j.1365-8711.2002.05366.x. S2CID 119347211.
  161. ^ Hauret, C; Magain, P; Biernaux, J (21 September 2018). "A cosmology-independent calibration of Type Ia supernovae data". Monthly Notices of the Royal Astronomical Society. 479 (3): 3996–4003. arXiv:1806.10900. Bibcode:2018MNRAS.479.3996H. doi:10.1093/mnras/sty1715. ISSN 0035-8711.
  162. ^ de Jaeger, T.; Galbany, L.; González-Gaitán, S.; Kessler, R.; Filippenko, A. V.; Förster, F.; Hamuy, M.; Brown, P. J.; Davis, T. M.; Gutiérrez, C. P.; Inserra, C.; Lewis, G. F.; Möller, A.; Scolnic, D.; Smith, M. (11 July 2020). "Studying Type II supernovae as cosmological standard candles using the Dark Energy Survey". Monthly Notices of the Royal Astronomical Society. 495 (4): 4860–4892. arXiv:1806.10900. Bibcode:2018MNRAS.479.3996H. doi:10.1093/mnras/staa1402. ISSN 0035-8711.
  163. ^ Li, W.; Leaman, J.; Chornock, R.; Filippenko, A. V.; Poznanski, D.; Ganeshalingam, M.; Wang, X.; Modjaz, M.; Jha, S.; Foley, R. J.; Smith, N. (2011). "Nearby supernova rates from the Lick Observatory Supernova Search – II. The observed luminosity functions and fractions of supernovae in a complete sample". Monthly Notices of the Royal Astronomical Society. 412 (3): 1441. arXiv:1006.4612. Bibcode:2011MNRAS.412.1441L. doi:10.1111/j.1365-2966.2011.18160.x. S2CID 59467555.
  164. ^ Richardson, D.; Branch, D.; Casebeer, D.; Millard, J.; Thomas, R. C.; Baron, E. (2002). "A Comparative Study of the Absolute Magnitude Distributions of Supernovae". The Astronomical Journal. 123 (2): 745–752. arXiv:astro-ph/0112051. Bibcode:2002AJ....123..745R. doi:10.1086/338318. S2CID 5697964.
  165. ^ Frail, D. A.; Giacani, E. B.; Goss, W. Miller; Dubner, G. M. (1996). "The Pulsar Wind Nebula Around PSR B1853+01 in the Supernova Remnant W44". Astrophysical Journal Letters. 464 (2): L165–L168. arXiv:astro-ph/9604121. Bibcode:1996ApJ...464L.165F. doi:10.1086/310103. S2CID 119392207.
  166. ^ a b Höflich, P. A.; Kumar, P.; Wheeler, J. Craig (2004). "Neutron star kicks and supernova asymmetry". Cosmic explosions in three dimensions: Asymmetries in supernovae and gamma-ray bursts. Cambridge University Press. p. 276. arXiv:astro-ph/0312542. Bibcode:2004cetd.conf..276L. {{cite book}}: |journal= ignored (help)
  167. ^ a b Janka, Hans-Thomas; Wongwathanarat, Annop; Kramer, Michael (1 February 2022). "Supernova Fallback as Origin of Neutron Star Spins and Spin-kick Alignment". The Astrophysical Journal. 926 (1): 9. arXiv:2104.07493. Bibcode:2022ApJ...926....9J. doi:10.3847/1538-4357/ac403c. ISSN 0004-637X.
  168. ^ Fryer, C. L. (2004). "Neutron Star Kicks from Asymmetric Collapse". Astrophysical Journal. 601 (2): L175–L178. arXiv:astro-ph/0312265. Bibcode:2004ApJ...601L.175F. doi:10.1086/382044. S2CID 1473584.
  169. ^ Gilkis, A.; Soker, N. (2014). "Implications of turbulence for jets in core-collapse supernova explosions". The Astrophysical Journal. 806 (1): 28. arXiv:1412.4984. Bibcode:2015ApJ...806...28G. doi:10.1088/0004-637X/806/1/28. S2CID 119002386.
  170. ^ Khokhlov, A. M.; Höflich, P. A.; Oran, E. S.; Wheeler, J. Craig; Wang, L.; Chtchelkanova, A. Yu. (1999). "Jet-induced Explosions of Core Collapse Supernovae". The Astrophysical Journal. 524 (2): L107. arXiv:astro-ph/9904419. Bibcode:1999ApJ...524L.107K. doi:10.1086/312305. S2CID 37572204.
  171. ^ Wang, L.; Baade, D.; Höflich, P. A.; Khokhlov, A. M.; Wheeler, J. C.; Kasen, D.; Nugent, P. E.; Perlmutter, S. A.; Fransson, C.; Lundqvist, P. (2003). "Spectropolarimetry of SN 2001el in NGC 1448: Asphericity of a Normal Type Ia Supernova". The Astrophysical Journal. 591 (2): 1110–1128. arXiv:astro-ph/0303397. Bibcode:2003ApJ...591.1110W. doi:10.1086/375444. S2CID 2923640.
  172. ^ a b c Mazzali, P. A.; Nomoto, K. I.; Cappellaro, E.; Nakamura, T.; Umeda, H.; Iwamoto, K. (2001). "Can Differences in the Nickel Abundance in Chandrasekhar-Mass Models Explain the Relation between the Brightness and Decline Rate of Normal Type Ia Supernovae?". The Astrophysical Journal. 547 (2): 988. arXiv:astro-ph/0009490. Bibcode:2001ApJ...547..988M. doi:10.1086/318428. S2CID 9324294.
  173. ^ Janka, H.-Th. (2002). "The Secrets Behind Supernovae". Science. 297 (5584): 1134–1135. doi:10.1126/science.1075935. PMID 12183617. S2CID 34349443.
  174. ^ Nomoto, Ken'Ichi; Iwamoto, Koichi; Kishimoto, Nobuhiro (1997). "Type Ia Supernovae: Their Origin and Possible Applications in Cosmology". Science. 276 (5317): 1378–1382. arXiv:astro-ph/9706007. Bibcode:1997Sci...276.1378N. doi:10.1126/science.276.5317.1378. PMID 9190677. S2CID 2502919.
  175. ^ Iwamoto, K. (2006). "Neutrino Emission from Type Ia Supernovae". AIP Conference Proceedings. 847: 406–408. Bibcode:2006AIPC..847..406I. doi:10.1063/1.2234440.
  176. ^ Hayden, B. T.; Garnavich, P. M.; Kessler, R.; Frieman, J. A.; Jha, S. W.; Bassett, B.; Cinabro, D.; Dilday, B.; Kasen, D.; Marriner, J.; Nichol, R. C.; Riess, A. G.; Sako, M.; Schneider, D. P.; Smith, M.; Sollerman, J. (2010). "The Rise and Fall of Type Ia Supernova Light Curves in the SDSS-II Supernova Survey". The Astrophysical Journal. 712 (1): 350–366. arXiv:1001.3428. Bibcode:2010ApJ...712..350H. doi:10.1088/0004-637X/712/1/350. S2CID 118463541.
  177. ^ Janka, H.-T. (2012). "Explosion Mechanisms of Core-Collapse Supernovae". Annual Review of Nuclear and Particle Science. 62 (1): 407–451. arXiv:1206.2503. Bibcode:2012ARNPS..62..407J. doi:10.1146/annurev-nucl-102711-094901. S2CID 118417333.
  178. ^ Smartt, Stephen J.; Nomoto, Ken'ichi; Cappellaro, Enrico; Nakamura, Takayoshi; Umeda, Hideyuki; Iwamoto, Koichi (2009). "Progenitors of core-collapse supernovae". Annual Review of Astronomy and Astrophysics. 47 (1): 63–106. arXiv:0908.0700. Bibcode:2009ARA&A..47...63S. doi:10.1146/annurev-astro-082708-101737. S2CID 55900386.
  179. ^ Dessart, L.; Burrows, A.; Livne, E.; Ott, C. D. (20 January 2008). "The Proto-Neutron Star Phase of the Collapsar Model and the Route to Long-Soft Gamma-Ray Bursts and Hypernovae". The Astrophysical Journal. 673 (1): L43–L46. arXiv:0710.5789. Bibcode:2008ApJ...673L..43D. doi:10.1086/527519. ISSN 0004-637X.
  180. ^ Senno, Nicholas; Murase, Kohta; Mészáros, Peter (8 April 2016). "Choked jets and low-luminosity gamma-ray bursts as hidden neutrino sources". Physical Review D. 93 (8): 083003. arXiv:1512.08513. Bibcode:2016PhRvD..93h3003S. doi:10.1103/PhysRevD.93.083003. ISSN 2470-0010. S2CID 16452722.
  181. ^ Woosley, S. E.; Blinnikov, S.; Heger, Alexander (15 November 2007). "Pulsational pair instability as an explanation for the most luminous supernovae". Nature. 450 (7168): 390–392. arXiv:0710.3314. Bibcode:2007Natur.450..390W. doi:10.1038/nature06333. ISSN 0028-0836. PMID 18004378. S2CID 2925738.
  182. ^ Barkov, Maxim V.; Komissarov, Serguei S. (21 July 2011). "Recycling of neutron stars in common envelopes and hypernova explosions: Recycling of neutron stars and hypernovae". Monthly Notices of the Royal Astronomical Society. 415 (1): 944–958. arXiv:1012.4565. Bibcode:2011MNRAS.415..944B. doi:10.1111/j.1365-2966.2011.18762.x.
  183. ^ Wright, Warren P.; Gilmer, Matthew S.; Fröhlich, Carla; Kneller, James P. (13 November 2017). "Neutrino signal from pair-instability supernovae". Physical Review D. 96 (10): 103008. arXiv:1706.08410. Bibcode:2017PhRvD..96j3008W. doi:10.1103/PhysRevD.96.103008. ISSN 2470-0010. S2CID 119487775.
  184. ^ Ganss, R; Pledger, J L; Sansom, A E; James, P A; Puls, J; Habergham-Mawson, S M (22 March 2022). "Metallicity estimation of core-collapse Supernova H ii regions in galaxies within 30 Mpc". Monthly Notices of the Royal Astronomical Society. 512 (1): 1541–1556. arXiv:2203.03308. Bibcode:2022MNRAS.512.1541G. doi:10.1093/mnras/stac625. ISSN 0035-8711.
  185. ^ Prochaska, J. X.; Bloom, J. S.; Chen, H.-W.; Foley, R. J.; Perley, D. A.; Ramirez-Ruiz, E.; Granot, J.; Lee, W. H.; Pooley, D.; Alatalo, K.; Hurley, K.; Cooper, M. C.; Dupree, A. K.; Gerke, B. F.; Hansen, B. M. S. (10 May 2006). "The Galaxy Hosts and Large-Scale Environments of Short-Hard Gamma-Ray Bursts". The Astrophysical Journal. 642 (2): 989–994. arXiv:astro-ph/0510022. Bibcode:2006ApJ...642..989P. doi:10.1086/501160. ISSN 0004-637X.
  186. ^ Petrosian, Artashes; Navasardyan, Hripsime; Cappellaro, Enrico; McLean, Brian; Allen, Ron; Panagia, Nino; Leitherer, Claus; MacKenty, John; Turatto, Massimo (March 2005). "Active and Star-forming Galaxies and Their Supernovae". The Astronomical Journal. 129 (3): 1369–1380. Bibcode:2005AJ....129.1369P. doi:10.1086/427712. ISSN 0004-6256.
  187. ^ Shao, X.; Liang, Y. C.; Dennefeld, M.; Chen, X. Y.; Zhong, G. H.; Hammer, F.; Deng, L. C.; Flores, H.; Zhang, B.; Shi, W. B.; Zhou, L. (25 July 2014). "Comparing the Host Galaxies of Type Ia, Type II, and Type Ibc Supernovae". The Astrophysical Journal. 791 (1): 57. arXiv:1407.0483. Bibcode:2014ApJ...791...57S. doi:10.1088/0004-637X/791/1/57. ISSN 0004-637X.
  188. ^ Taggart, K; Perley, D A (5 April 2021). "Core-collapse, superluminous, and gamma-ray burst supernova host galaxy populations at low redshift: the importance of dwarf and starbursting galaxies". Monthly Notices of the Royal Astronomical Society. 503 (3): 3931–3952. arXiv:1911.09112. Bibcode:2021MNRAS.503.3931T. doi:10.1093/mnras/stab174. ISSN 0035-8711.
  189. ^ Moriya, Takashi J.; Maeda, Keiichi; Taddia, Francesco; Sollerman, Jesper; Blinnikov, Sergei I.; Sorokina, Elena I. (11 April 2014). "Mass-loss histories of Type IIn supernova progenitors within decades before their explosion". Monthly Notices of the Royal Astronomical Society. 439 (3): 2917–2926. arXiv:1401.4893. Bibcode:2014MNRAS.439.2917M. doi:10.1093/mnras/stu163. ISSN 1365-2966.
  190. ^ Galbany, L.; Anderson, J. P.; Sánchez, S. F.; Kuncarayakti, H.; Pedraz, S.; González-Gaitán, S.; Stanishev, V.; Domínguez, I.; Moreno-Raya, M. E.; Wood-Vasey, W. M.; Mourão, A. M.; Ponder, K. A.; Badenes, C.; Mollá, M.; López-Sánchez, A. R. (13 March 2018). "PISCO: The PMAS/PPak Integral-field Supernova Hosts Compilation". The Astrophysical Journal. 855 (2): 107. arXiv:1802.01589. Bibcode:2018ApJ...855..107G. doi:10.3847/1538-4357/aaaf20. ISSN 1538-4357.
  191. ^ a b Davies, Ben; Beasor, Emma R. (2020). "'On the red supergiant problem': A rebuttal, and a consensus on the upper mass cut-off for II-P progenitors". Monthly Notices of the Royal Astronomical Society: Letters. 496 (1): L142–L146. arXiv:2005.13855. Bibcode:2020MNRAS.496L.142D. doi:10.1093/mnrasl/slaa102.
  192. ^ Smartt, S. J.; Eldridge, J. J.; Crockett, R. M.; Maund, J. R. (May 2009). "The death of massive stars – I. Observational constraints on the progenitors of Type II-P supernovae". Monthly Notices of the Royal Astronomical Society. 395 (3): 1409–1437. arXiv:0809.0403. Bibcode:2009MNRAS.395.1409S. doi:10.1111/j.1365-2966.2009.14506.x. ISSN 0035-8711. S2CID 3228766.
  193. ^ a b c d e Smartt, Stephen J.; Thompson, Todd A.; Kochanek, Christopher S. (2009). "Progenitors of Core-Collapse Supernovae". Annual Review of Astronomy & Astrophysics. 47 (1): 63–106. arXiv:0908.0700. Bibcode:2009ARA&A..47...63S. doi:10.1146/annurev-astro-082708-101737. S2CID 55900386.
  194. ^ Walmswell, J. J.; Eldridge, J. J. (2012). "Circumstellar dust as a solution to the red supergiant supernova progenitor problem". Monthly Notices of the Royal Astronomical Society. 419 (3): 2054. arXiv:1109.4637. Bibcode:2012MNRAS.419.2054W. doi:10.1111/j.1365-2966.2011.19860.x. S2CID 118445879.
  195. ^ Georgy, C. (2012). "Yellow supergiants as supernova progenitors: An indication of strong mass loss for red supergiants?". Astronomy & Astrophysics. 538: L8–L2. arXiv:1111.7003. Bibcode:2012A&A...538L...8G. doi:10.1051/0004-6361/201118372. S2CID 55001976.
  196. ^ a b Yoon, S.-C.; Gräfener, G.; Vink, J. S.; Kozyreva, A.; Izzard, R. G. (2012). "On the nature and detectability of Type Ib/c supernova progenitors". Astronomy & Astrophysics. 544: L11. arXiv:1207.3683. Bibcode:2012A&A...544L..11Y. doi:10.1051/0004-6361/201219790. S2CID 118596795.
  197. ^ Groh, J. H.; Meynet, G.; Ekström, S. (2013). "Massive star evolution: Luminous blue variables as unexpected supernova progenitors". Astronomy & Astrophysics. 550: L7. arXiv:1301.1519. Bibcode:2013A&A...550L...7G. doi:10.1051/0004-6361/201220741. S2CID 119227339.
  198. ^ a b c Johnson, Jennifer A. (2019). "Populating the periodic table: Nucleosynthesis of the elements". Science. 363 (6426): 474–478. Bibcode:2019Sci...363..474J. doi:10.1126/science.aau9540. PMID 30705182. S2CID 59565697.
  199. ^ François, P.; Matteucci, F.; Cayrel, R.; Spite, M.; Spite, F.; Chiappini, C. (2004). "The evolution of the Milky Way from its earliest phases: Constraints on stellar nucleosynthesis". Astronomy & Astrophysics. 421 (2): 613–621. arXiv:astro-ph/0401499. Bibcode:2004A&A...421..613F. doi:10.1051/0004-6361:20034140. S2CID 16257700.
  200. ^ a b Truran, J. W. (1977). "Supernova Nucleosynthesis". In Schramm, D. N. (ed.). Supernovae. Astrophysics and Space Science Library. Vol. 66. Springer. pp. 145–158. Bibcode:1977ASSL...66..145T. doi:10.1007/978-94-010-1229-4_14. ISBN 978-94-010-1231-7.
  201. ^ Nomoto, Ken'Ichi; Leung, Shing-Chi (2018). "Single Degenerate Models for Type Ia Supernovae: Progenitor's Evolution and Nucleosynthesis Yields". Space Science Reviews. 214 (4): 67. arXiv:1805.10811. Bibcode:2018SSRv..214...67N. doi:10.1007/s11214-018-0499-0. S2CID 118951927.
  202. ^ Maeda, K.; Röpke, F.K.; Fink, M.; Hillebrandt, W.; Travaglio, C.; Thielemann, F.-K. (2010). "Nucleosynthesis in Two-Dimensional Delayed Detonation Models of Type Ia Supernova Explosions". The Astrophysical Journal. 712 (1): 624–638. arXiv:1002.2153. Bibcode:2010ApJ...712..624M. doi:10.1088/0004-637X/712/1/624. S2CID 119290875.
  203. ^ Wanajo, Shinya; Janka, Hans-Thomas; Müller, Bernhard (2011). "Electron-Capture Supernovae as the Origin of Elements Beyond Iron". The Astrophysical Journal. 726 (2): L15. arXiv:1009.1000. Bibcode:2011ApJ...726L..15W. doi:10.1088/2041-8205/726/2/L15. S2CID 119221889.
  204. ^ Eichler, M.; Nakamura, K.; Takiwaki, T.; Kuroda, T.; Kotake, K.; Hempel, M.; Cabezón, R.; Liebendörfer, M.; Thielemann, F-K (2018). "Nucleosynthesis in 2D core-collapse supernovae of 11.2 and 17.0 M⊙ progenitors: Implications for Mo and Ru production". Journal of Physics G: Nuclear and Particle Physics. 45 (1): 014001. arXiv:1708.08393. Bibcode:2018JPhG...45a4001E. doi:10.1088/1361-6471/aa8891. S2CID 118936429.
  205. ^ Qian, Y.-Z.; Vogel, P.; Wasserburg, G. J. (1998). "Diverse Supernova Sources for the r-Process". Astrophysical Journal. 494 (1): 285–296. arXiv:astro-ph/9706120. Bibcode:1998ApJ...494..285Q. doi:10.1086/305198. S2CID 15967473.
  206. ^ Siegel, Daniel M.; Barnes, Jennifer; Metzger, Brian D. (2019). "Collapsars as a major source of r-process elements". Nature. 569 (7755): 241–244. arXiv:1810.00098. Bibcode:2019Natur.569..241S. doi:10.1038/s41586-019-1136-0. PMID 31068724. S2CID 73612090.
  207. ^ Gonzalez, G.; Brownlee, D.; Ward, P. (2001). "The Galactic Habitable Zone: Galactic Chemical Evolution". Icarus. 152 (1): 185. arXiv:astro-ph/0103165. Bibcode:2001Icar..152..185G. doi:10.1006/icar.2001.6617. S2CID 18179704.
  208. ^ Rho, Jeonghee; Milisavljevic, Danny; Sarangi, Arkaprabha; Margutti, Raffaella; Chornock, Ryan; Rest, Armin; Graham, Melissa; Craig Wheeler, J.; DePoy, Darren; Wang, Lifan; Marshall, Jennifer; Williams, Grant; Street, Rachel; Skidmore, Warren; Haojing, Yan; Bloom, Joshua; Starrfield, Sumner; Lee, Chien-Hsiu; Cowperthwaite, Philip S.; Stringfellow, Guy S.; Coppejans, Deanne; Terreran, Giacomo; Sravan, Niharika; Geballe, Thomas R.; Evans, Aneurin; Marion, Howie (2019). "Astro2020 Science White Paper: Are Supernovae the Dust Producer in the Early Universe?". Bulletin of the American Astronomical Society. 51 (3): 351. arXiv:1904.08485. Bibcode:2019BAAS...51c.351R.
  209. ^ Cox, D. P. (1972). "Cooling and Evolution of a Supernova Remnant". Astrophysical Journal. 178: 159. Bibcode:1972ApJ...178..159C. doi:10.1086/151775.
  210. ^ a b Johnson, Jennifer A. (February 2019). "Populating the periodic table: Nucleosynthesis of the elements". Science. 363 (6426): 474–478. Bibcode:2019Sci...363..474J. doi:10.1126/science.aau9540. ISSN 0036-8075. PMID 30705182. S2CID 59565697.
  211. ^ Sandstrom, K. M.; Bolatto, A. D.; Stanimirović, S.; Van Loon, J. Th.; Smith, J. D. T. (2009). "Measuring Dust Production in the Small Magellanic Cloud Core-Collapse Supernova Remnant 1E 0102.2–7219". The Astrophysical Journal. 696 (2): 2138–2154. arXiv:0810.2803. Bibcode:2009ApJ...696.2138S. doi:10.1088/0004-637X/696/2/2138. S2CID 8703787.
  212. ^ Salaris, Maurizio; Cassisi, Santi (August 2017). "Chemical element transport in stellar evolution models". Royal Society Open Science. 4 (8): 170192. arXiv:1707.07454. Bibcode:2017RSOS....470192S. doi:10.1098/rsos.170192. ISSN 2054-5703. PMC 5579087. PMID 28878972.
  213. ^ Fischer, Debra A.; Valenti, Jeff (2005). "The planet-metallicity correlation". The Astrophysical Journal. 622 (2): 1102–1117. Bibcode:2005ApJ...622.1102F. doi:10.1086/428383. S2CID 121872365.
  214. ^ Zhu, Wei; Dong, Subo (2021). "Exoplanet Statistics and Theoretical Implications". Annual Review of Astronomy and Astrophysics. 59: 291–336. arXiv:2103.02127. Bibcode:2021ARA&A..59..291Z. doi:10.1146/annurev-astro-112420-020055. S2CID 232105177.
  215. ^ Preibisch, T.; Zinnecker, H. (2001). "Triggered Star Formation in the Scorpius-Centaurus OB Association (Sco OB2)". From Darkness to Light: Origin and Evolution of Young Stellar Clusters. 243: 791. arXiv:astro-ph/0008013. Bibcode:2001ASPC..243..791P.
  216. ^ Krebs, J.; Hillebrandt, W. (1983). "The interaction of supernova shockfronts and nearby interstellar clouds". Astronomy and Astrophysics. 128 (2): 411. Bibcode:1983A&A...128..411K.
  217. ^ Cameron, A.G.W.; Truran, J.W. (1977). "The supernova trigger for formation of the solar system". Icarus. 30 (3): 447. Bibcode:1977Icar...30..447C. doi:10.1016/0019-1035(77)90101-4.
  218. ^ Bhandan, Shivani (1 June 2020). "The Host Galaxies and Progenitors of Fast Radio Bursts Localised with the Australian Square Kilometre Array Pathfinder". The Astrophysical Journal Letters. 895 (2): L37. arXiv:2005.13160. Bibcode:2020ApJ...895L..37B. doi:10.3847/2041-8213/ab672e. S2CID 218900539.
  219. ^ Zhang, Bing (5 November 2020). "The physical mechanisms of fast radio bursts". Nature. 587 (7832): 45–53. arXiv:2011.03500. Bibcode:2020Natur.587...45Z. doi:10.1038/s41586-020-2828-1. ISSN 0028-0836. PMID 33149290. S2CID 226259246.
  220. ^ Chu, Jennifer (13 July 2022). "Astronomers detect a radio "heartbeat" billions of light-years from Earth". MIT News. Massachusetts Institute of Technology. Retrieved 19 March 2023.
  221. ^ Petroff, E.; Hessels, J. W. T.; Lorimer, D. R. (29 March 2022). "Fast radio bursts at the dawn of the 2020s". The Astronomy and Astrophysics Review. 30 (1): 2. arXiv:2107.10113. Bibcode:2022A&ARv..30....2P. doi:10.1007/s00159-022-00139-w. ISSN 1432-0754. S2CID 253690001.
  222. ^ Ackermann, M.; et al. (2013). "Detection of the Characteristic Pion-Decay Signature in Supernova Remnants". Science. 339 (6121): 807–11. arXiv:1302.3307. Bibcode:2013Sci...339..807A. doi:10.1126/science.1231160. PMID 23413352. S2CID 29815601.
  223. ^ Ott, C. D.; O'Connor, E. P.; Gossan, S. E.; Abdikamalov, E.; Gamma, U. C. T.; Drasco, S. (2012). "Core-Collapse Supernovae, Neutrinos, and Gravitational Waves". Nuclear Physics B: Proceedings Supplements. 235: 381–387. arXiv:1212.4250. Bibcode:2013NuPhS.235..381O. doi:10.1016/j.nuclphysbps.2013.04.036. S2CID 34040033.
  224. ^ Morozova, Viktoriya; Radice, David; Burrows, Adam; Vartanyan, David (2018). "The Gravitational Wave Signal from Core-collapse Supernovae". The Astrophysical Journal. 861 (1): 10. arXiv:1801.01914. Bibcode:2018ApJ...861...10M. doi:10.3847/1538-4357/aac5f1. S2CID 118997362.
  225. ^ Al Kharusi, S.; BenZvi, S. Y.; Bobowski, J. S.; Bonivento, W.; Brdar, V.; Brunner, T.; Caden, E.; Clark, M.; Coleiro, A.; Colomer-Molla, M.; Crespo-Anadón, J. I.; Depoian, A.; Dornic, D.; Fischer, V.; et al. (1 March 2021). "SNEWS 2.0: a next-generation supernova early warning system for multi-messenger astronomy". New Journal of Physics. 23 (3): 031201. arXiv:2011.00035. Bibcode:2021NJPh...23c1201A. doi:10.1088/1367-2630/abde33. ISSN 1367-2630. S2CID 226227393.
  226. ^ Fields, B. D.; Hochmuth, K. A.; Ellis, J. (2005). "Deep-Ocean Crusts as Telescopes: Using Live Radioisotopes to Probe Supernova Nucleosynthesis". The Astrophysical Journal. 621 (2): 902–907. arXiv:astro-ph/0410525. Bibcode:2005ApJ...621..902F. doi:10.1086/427797. S2CID 17932224.
  227. ^ Knie, K.; Korschinek, G.; Faestermann, T.; Dorfi, E.; Rugel, G.; Wallner, A. (2004). "60Fe Anomaly in a Deep-Sea Manganese Crust and Implications for a Nearby Supernova Source". Physical Review Letters. 93 (17): 171103–171106. Bibcode:2004PhRvL..93q1103K. doi:10.1103/PhysRevLett.93.171103. PMID 15525065. S2CID 23162505.
  228. ^ Fields, B. D.; Ellis, J. (1999). "On Deep-Ocean Fe-60 as a Fossil of a Near-Earth Supernova". New Astronomy. 4 (6): 419–430. arXiv:astro-ph/9811457. Bibcode:1999NewA....4..419F. doi:10.1016/S1384-1076(99)00034-2. S2CID 2786806.
  229. ^ "In Brief". Scientific American. 300 (5): 28. 2009. Bibcode:2009SciAm.300e..28.. doi:10.1038/scientificamerican0509-28a.
  230. ^ Petersen, Carolyn Collins (22 March 2023). "Did Supernovae Help Push Life to Become More Diverse?". Universe Today. Retrieved 23 March 2023.
  231. ^ Svensmark, Henrik (16 March 2023). "A persistent influence of supernovae on biodiversity over the Phanerozoic". Ecology and Evolution. 13 (3). Wiley Online Library: e9898. Bibcode:2023EcoEv..13E9898S. doi:10.1002/ece3.9898. PMC 10019915. PMID 36937070. e9898.
  232. ^ Gorelick, M. (2007). "The Supernova Menace". Sky & Telescope. 113 (3): 26. Bibcode:2007S&T...113c..26G.
  233. ^ Landsman, W.; Simon, T.; Bergeron, P. (1999). "The hot white-dwarf companions of HR 1608, HR 8210, and HD 15638". Publications of the Astronomical Society of the Pacific. 105 (690): 841–847. Bibcode:1993PASP..105..841L. doi:10.1086/133242.
  234. ^ Beech, Martin (December 2011). "The past, present and future supernova threat to Earth's biosphere". Astrophysics and Space Science. 336 (2): 287–302. Bibcode:2011Ap&SS.336..287B. doi:10.1007/s10509-011-0873-9. ISSN 0004-640X. S2CID 119803426.
  235. ^ Gehrels, N.; Laird, C. M.; Jackman, C. H.; Cannizzo, J. K.; Mattson, B. J.; Chen, W. (2003). "Ozone Depletion from Nearby Supernovae". Astrophysical Journal. 585 (2): 1169–1176. arXiv:astro-ph/0211361. Bibcode:2003ApJ...585.1169G. doi:10.1086/346127. S2CID 15078077.
  236. ^ Van Der Sluys, M. V.; Lamers, H. J. G. L. M. (2003). "The dynamics of the nebula M1-67 around the run-away Wolf-Rayet star WR 124". Astronomy and Astrophysics. 398: 181–194. arXiv:astro-ph/0211326. Bibcode:2003A&A...398..181V. doi:10.1051/0004-6361:20021634. S2CID 6142859.
  237. ^ Cristofari, P; Marcowith, A; Renaud, M; Dwarkadas, V V; Tatischeff, V; Giacinti, G; Peretti, E; Sol, H (18 February 2022). "The first days of Type II-P core collapse supernovae in the gamma-ray range". Monthly Notices of the Royal Astronomical Society. 511 (3): 3321–3329. arXiv:2201.09583. doi:10.1093/mnras/stac217. ISSN 0035-8711.
  238. ^ Tramper, F.; Straal, S. M.; Sanyal, D.; Sana, H.; De Koter, A.; Gräfener, G.; Langer, N.; Vink, J. S.; De Mink, S. E.; Kaper, L. (2015). "Massive stars on the verge of exploding: The properties of oxygen sequence Wolf-Rayet stars". Astronomy & Astrophysics. 581: A110. arXiv:1507.00839. Bibcode:2015A&A...581A.110T. doi:10.1051/0004-6361/201425390. S2CID 56093231.
  239. ^ Tramper, F.; Gräfener, G.; Hartoog, O. E.; Sana, H.; De Koter, A.; Vink, J. S.; Ellerbroek, L. E.; Langer, N.; Garcia, M.; Kaper, L.; De Mink, S. E. (2013). "On the nature of WO stars: A quantitative analysis of the WO3 star DR1 in IC 1613". Astronomy & Astrophysics. 559: A72. arXiv:1310.2849. Bibcode:2013A&A...559A..72T. doi:10.1051/0004-6361/201322155. S2CID 216079684.
  240. ^ Firestone, R. B. (June 2014). "Observation of 23 Supernovae That Exploded". The Astrophysical Journal. 789 (1): 29. Bibcode:2014ApJ...789...29F. doi:10.1088/0004-637X/789/1/29. ISSN 0004-637X.
  241. ^ Inglis, M. (2015). "Star Death: Supernovae, Neutron Stars & Black Holes". Astrophysics is Easy!. The Patrick Moore Practical Astronomy Series. pp. 203–223. doi:10.1007/978-3-319-11644-0_12. ISBN 978-3-319-11643-3.
  242. ^ "VV Cephei". stars.astro.illinois.edu. Retrieved 14 April 2024.
  243. ^ a b Mukhopadhyay, Mainak; Lunardini, Cecilia; Timmes, F. X.; Zuber, Kai (1 August 2020). "Presupernova neutrinos: directional sensitivity and prospects for progenitor identification". The Astrophysical Journal. 899 (2): 153. arXiv:2004.02045. Bibcode:2020ApJ...899..153M. doi:10.3847/1538-4357/ab99a6. ISSN 0004-637X.
  244. ^ Lobel, A.; Stefanik, R. P.; Torres, G.; Davis, R. J.; Ilyin, I.; Rosenbush, A. E. (2004). "Spectroscopy of the Millennium Outburst and Recent Variability of the Yellow Hypergiant Rho Cassiopeiae". Stars as Suns: Activity. 219: 903. arXiv:astro-ph/0312074. Bibcode:2004IAUS..219..903L.
  245. ^ Van Boekel, R.; Kervella, P.; Schöller, M.; Herbst, T.; Brandner, W.; De Koter, A.; Waters, L. B. F. M.; Hillier, D. J.; Paresce, F.; Lenzen, R.; Lagrange, A.-M. (2003). "Direct measurement of the size and shape of the present-day stellar wind of eta Carinae". Astronomy and Astrophysics. 410 (3): L37. arXiv:astro-ph/0310399. Bibcode:2003A&A...410L..37V. doi:10.1051/0004-6361:20031500. S2CID 18163131.
  246. ^ Thielemann, F.-K.; Hirschi, R.; Liebendörfer, M.; Diehl, R. (2011). "Massive Stars and Their Supernovae". Astronomy with Radioactivities. Lecture Notes in Physics. Vol. 812. pp. 153–231. arXiv:1008.2144. Bibcode:2011LNP...812..153T. doi:10.1007/978-3-642-12698-7_4. ISBN 978-3-642-12697-0. S2CID 119254840.
  247. ^ "Regor". stars.astro.illinois.edu. Retrieved 18 August 2024.
  248. ^ "Acrux". stars.astro.illinois.edu. Retrieved 15 August 2024.
  249. ^ "Mimosa". stars.astro.illinois.edu. Retrieved 15 August 2024.
  250. ^ Tuthill, P. G.; Monnier, J. D.; Lawrance, N.; Danchi, W. C.; Owocki, S. P.; Gayley, K. G. (2008). "The Prototype Colliding-Wind Pinwheel WR 104". The Astrophysical Journal. 675 (1): 698–710. arXiv:0712.2111. Bibcode:2008ApJ...675..698T. doi:10.1086/527286. S2CID 119293391.
  251. ^ Thoroughgood, T. D.; Dhillon, V. S.; Littlefair, S. P.; Marsh, T. R.; Smith, D. A. (2002). "The recurrent nova U Scorpii – A type Ia supernova progenitor". The Physics of Cataclysmic Variables and Related Objects. Vol. 261. San Francisco, CA: Astronomical Society of the Pacific. arXiv:astro-ph/0109553. Bibcode:2002ASPC..261...77T.

Further reading

[edit]
[edit]