A supernova (/ˌsuːpərˈnoʊvə/ plural: supernovae /ˌsuːpərˈnoʊviː/ or supernovas, abbreviations: SN and SNe) is a powerful and luminous stellar explosion. This transient astronomical event 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. The peak optical luminosity of a supernova can be comparable to that of an entire galaxy before fading over several weeks or months.
Supernovae are more energetic than novae. In Latin, nova means "new", referring astronomically 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 in 1929.
The most recent directly observed supernova in the Milky Way was Kepler's Supernova in 1604, but the remnants of more recent supernovae have been found. Observations of supernovae in other galaxies suggest they occur in the Milky Way on average about three times every century. These supernovae would almost certainly be observable with modern astronomical telescopes. The most recent naked-eye supernova was SN 1987A, the explosion of a blue supergiant star in the Large Magellanic Cloud, a satellite 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 degenerate star such as a white dwarf, or the sudden gravitational collapse of a massive star's core. In the first class of events, 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 a stellar merger. In the massive star case, the core of a massive star may undergo sudden collapse, releasing gravitational potential energy as a supernova. While some observed supernovae are more complex than these two simplified theories, the astrophysical mechanics have been established and accepted by most astronomers for some time.[vague]
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. Supernova remnants might be a major source of cosmic rays. Supernovae might produce gravitational waves, though thus far, gravitational waves have been detected only from the mergers of black holes and neutron stars.
Observation history
Main article: History of supernova observation
The Crab Nebula is a pulsar wind nebula associated with the 1054 supernova
The highlighted passages refer to the Chinese observation of SN 1054.
Compared to a star's entire history, the visual appearance of a supernova is very brief, perhaps spanning several months, so that the chances of observing one with the naked eye is 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, restricted to either those having large mass or extraordinarily rare kinds of binary stars containing white dwarfs.[1]
The earliest possible recorded supernova, known as HB9, could have been viewed and recorded by unknown Indian observers in 4500±1000 BC.[2] Later, SN 185 was viewed by Chinese astronomers in 185 AD. The brightest recorded supernova was SN 1006, which occurred in 1006 AD in the constellation of Lupus, and was described by observers across China, Japan, Iraq, Egypt, and Europe.[3][4][5] The widely observed supernova SN 1054 produced the Crab Nebula. Supernovae SN 1572 and SN 1604, the latest to be observed with the naked eye in the Milky Way galaxy, had notable effects 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.[6] Johannes Kepler began observing SN 1604 at its peak on October 17, 1604, and continued to make estimates of its brightness until it faded from naked eye view a year later.[7] It was the second supernova to be observed in a generation (after SN 1572 seen by Tycho Brahe in Cassiopeia).[8]
There is some evidence that the youngest galactic supernova, G1.9+0.3, occurred in the late 19th century, considerably more recently than Cassiopeia A from around 1680.[9] Neither supernova was noted at the time. In the case of G1.9+0.3, high extinction along the plane of the galaxy could have dimmed the event sufficiently to go unnoticed. The situation for Cassiopeia A is less clear. Infrared light echos have been detected showing that it was a type IIb supernova and was not in a region of especially high extinction.[10]
Observation and discovery of extragalactic supernovae are now far more common. The first such observation was of SN 1885A in the Andromeda Galaxy. Today, amateur and professional astronomers are finding several hundred every year, some when near maximum brightness, others on old astronomical photographs or plates. American astronomers Rudolph Minkowski and Fritz Zwicky developed the modern supernova classification scheme beginning in 1941.[11] During the 1960s, astronomers found that the maximum intensities of supernovae could be used as standard candles, hence indicators of astronomical distances.[12] 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.[13] 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,[14] while the age of supernova remnant RX J0852.0-4622 was estimated from temperature measurements[15] and the gamma ray emissions from the radioactive decay of titanium-44.[16]
SN Antikythera in galaxy cluster RXC J0949.8+1707. SN Eleanor and SN Alexander were observed in the same galaxy in 2011.[17]
The most luminous supernova ever recorded is ASASSN-15lh. It was first detected in June 2015 and peaked at 570 billion L☉, which is twice the bolometric luminosity of any other known supernova.[18] However, the nature of this supernova continues to be debated and several alternative explanations have been suggested, e.g. tidal disruption of a star by a black hole.[19]
Among the earliest detected since time of detonation, and for which the earliest spectra have been obtained (beginning at 6 hours after the actual explosion), is the type II SN 2013fs (iPTF13dqy) which was recorded 3 hours after the supernova event on 6 October 2013 by the Intermediate Palomar Transient Factory (iPTF). The star is located in a spiral galaxy named NGC 7610, 160 million light-years away in the constellation of Pegasus.[20][21]
On 20 September 2016, amateur astronomer Victor Buso from Rosario, Argentina was testing his telescope.[22][23] When taking several photographs of galaxy NGC 613, Buso chanced upon a supernova that had just become visible on Earth. After examining the images, he contacted the Instituto de Astrofísica de La Plata. "It was the first time anyone had ever captured the initial moments of the “shock breakout” from an optical supernova, one not associated with a gamma-ray or X-ray burst."[22] The odds of capturing such an event were put between one in ten million to one in a hundred million, according to astronomer Melina Bersten from the Instituto de Astrofísica. The supernova Buso observed was a type IIb made by a star twenty times the mass of the sun.[22] Astronomer Alex Filippenko, from the University of California, remarked that professional astronomers had been searching for such an event for a long time. He stated: "Observations of stars in the first moments they begin exploding provide information that cannot be directly obtained in any other way."[22]
Discovery
Main article: History of supernova observation § Telescope observation
Supernova remnant SNR E0519-69.0 in the Large Magellanic Cloud
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 Fritz Zwicky in lectures at Caltech during 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 had been lost and the modern name was in use.[27] Because supernovae are relatively rare events within a galaxy, occurring about three times a century in the Milky Way,[28] obtaining a good sample of supernovae to study requires regular monitoring of many galaxies.
Supernovae in other galaxies cannot be predicted with any meaningful accuracy. Normally, when they are discovered, they are already in progress.[29] 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.[30]
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.[31] 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.[32][33] Neutrinos are 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.[34]
"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[35]—where z is a dimensionless measure of the spectrum's frequency shift.
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.[36][37] Low redshift observations also anchor the low-distance end of the Hubble curve, which is a plot of distance versus redshift for visible galaxies.[38][39]
Naming convention
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. 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. Afterward 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.[40] The last supernova of 2005, SN 2005nc, was the 367th (14 × 26 + 3 = 367). The suffix "nc" acts as a bijective base-26 encoding, with a = 1, b = 2, c = 3, ... z = 26. Since 2000, professional and amateur astronomers have been finding several hundreds of supernovae each year (572 in 2007, 261 in 2008, 390 in 2009; 231 in 2013).[41][42]
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). Since 1885 the additional letter notation has been used, even if there was only one supernova discovered that year (e.g. 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, however, they have been needed every year. Since 2016, the increasing number of discoveries has regularly led to the additional use of three-digit designations.[43]
Classification
Artist's impression of supernova 1993J.[44]
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).[45][46]
Supernova taxonomy[45][46] 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).[47]
Type IIn
Some narrow lines
Type IIb
Spectrum changes to become like Type Ib
Type I
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. The light curves are all similar, although type Ia are generally brighter at peak luminosity, but the light curve is not important for classification of type I supernovae.
A small number of type Ia supernovae exhibit unusual features, such as non-standard luminosity or broadened light curves, and these are typically classified 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.
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.[48]
Type II
Light curves are used to classify type II-P and type II-L supernovae.
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'.
A few supernovae, such as SN 1987K[49] 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.[46]
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.
Supernovae that do not fit into the normal classifications are designated peculiar, or 'pec'.[46]
Types III, IV, and V
Fritz 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. 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. 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.[50] Supernovae in M101 (1909) and M83 (1923 and 1957) were also suggested as possible type IV or type V supernovae.[51]
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.[47]
Current models
Sequence shows the rapid brightening and slower fading of a supernova in the galaxy NGC 1365 (the bright dot close to and slightly above the galactic center).[52]
Supernovae type codes, as described above, are taxonomic: the type number describes 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 Wolf–Rayet progenitors by core collapse. The following summarises what is currently believed to be the most plausible explanations for supernovae.
Thermal runaway
Main article: Type Ia supernova
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.[53] 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.[54][55]
Normal Type Ia
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 (M☉)[56] (for a non-rotating star), it would no longer be able to support the bulk of its mass through electron degeneracy pressure[57][58] 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%[59]) before collapse is initiated.[56] 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.[58]
Within a few seconds, a substantial fraction of the matter in the white dwarf undergoes nuclear fusion, releasing enough energy (1–2×1044 J)[60] to unbind the star in a supernova.[61] 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.[62]
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.[63] 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. Despite widespread acceptance of the basic model, the exact details of initiation and of the heavy elements produced in the catastrophic event are still unclear.
Type Ia supernovae follow 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.[62] 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 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 behavior. This allows them to be used as a secondary[64] standard candle to measure the distance to their host galaxies.[65]
Non-standard Type Ia
Another 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.[66] There is much variation in this type of event,[67] and, in many cases, there may be no supernova at all, in which case they will have a broader and less luminous light curve than the more normal SN type Ia.
Abnormally bright type Ia supernovae occur when the white dwarf already has a mass higher than the Chandrasekhar limit,[68] possibly enhanced further by asymmetry,[69] but the ejected material will have less than normal kinetic energy.
There is no formal sub-classification for the 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.[70][71] This type of supernova may not always completely destroy the white dwarf progenitor and could leave behind a zombie star.[72]
One specific type of non-standard type Ia supernova develops hydrogen, and other, emission lines and gives the appearance of mixture between a normal type Ia and a type IIn supernova. Examples are SN 2002ic and SN 2005gj. These supernovae have been dubbed type Ia/IIn, type Ian, type IIa and type IIan.[73]
Core collapse
Supernova types by initial mass-metallicity
The layers of a massive, evolved star just prior to 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, or the release of gravitational potential energy may be insufficient and the star may collapse into a black hole or neutron star with little radiated energy.
Core collapse can be caused by several different mechanisms: electron capture; exceeding the Chandrasekhar limit; pair-instability; or photodisintegration.[74][75] 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 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.
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.[76] 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.[77]
Core collapse scenarios by mass and metallicity[74] 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
Remnants of single massive stars
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 by a process that may include neutrino interaction. The surrounding material is blasted away (f), leaving only a degenerate remnant.
When a stellar core is no longer supported against gravity, it collapses in on itself with velocities reaching 70,000 km/s (0.23c),[78] resulting in a rapid increase in temperature and density. What follows next 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.
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 diameter[79] and 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 M☉ then neutron degeneracy is insufficient to stop the collapse and a black hole forms directly with no supernova.
In lower mass cores the collapse is stopped and the newly formed neutron core has an initial temperature of about 100 billion kelvin, 6000 times the temperature of the sun's core.[80] At this temperature, neutrino-antineutrino pairs of all flavors are efficiently formed by thermal emission. These thermal neutrinos are several times more abundant than the electron-capture neutrinos.[81] 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.[79][82] The suddenly halted core collapse rebounds and produces a shock wave that stalls within milliseconds[83] in the outer core 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[82] (1 foe) from the neutrino pulse, producing the visible brightness, although there are also other theories on how to power the explosion.[79]
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.
The collapse of a massive non-degenerate core will ignite further fusion. When the core collapse is initiated by pair instability, 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.[84]
Type II
Main article: Type II supernova
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☉[85]) evolve in a complex fashion, progressively burning heavier elements at hotter temperatures in their cores.[79][86] The star becomes layered like an onion, with the burning of more easily fused elements occurring in larger shells.[74][87] 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.[85]
If core collapse occurs during a supergiant phase when the star still has a hydrogen envelope, the result is a type II supernova. 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 type II supernova. 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.
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. 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.
Type Ib and Ic
Main article: Type Ib and Ic supernovae
SN 2008D, a type Ib[88] supernova, shown in X-ray (left) and visible light (right) at the far upper end of the galaxy[89]
These supernovae, like those of type II, are massive stars that undergo core collapse. However 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.[90] 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 and 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.[91] Since a supernova can occur whenever the mass of the star at the time of core collapse is low enough not to cause complete fallback to a black hole, any massive star may result in a supernova if it loses enough mass before core collapse occurs.
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.
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.[92] 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.[93][94]
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.[95] 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[96] might be an 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.
Failed supernovae
Main article: Failed supernova
The core collapse of some massive stars may not result in a visible supernova. The main model for this is a sufficiently massive core that the kinetic energy is insufficient to reverse the infall of the outer layers onto a black hole. These events are difficult to detect, but large surveys have detected possible candidates.[97][98] 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.[99]
Light curves
Comparative supernova type light curves
A historic puzzle concerned the source of energy that can maintain the optical supernova glow for months. Although the energy that disrupts each type of supernovae is delivered promptly, the light curves are dominated by subsequent radioactive heating of the rapidly expanding ejecta. Some have considered rotational energy from the central pulsar. The ejecta gases would dim quickly without some energy input to keep it hot. The intensely radioactive nature of the ejecta gases, which is now known to be correct for most supernovae, was first calculated on sound nucleosynthesis grounds in the late 1960s.[100] It was not until SN 1987A that direct observation of gamma-ray lines unambiguously identified the major radioactive nuclei.[101]
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. 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 of 847keV and 1238keV, that are absorbed and dominate the heating and thus the luminosity of the ejecta at intermediate times (several weeks) to late times (several months).[102] 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.[101]
Messier 61 with supernova SN2020jfo, taken by an amateur astronomer in 2020
The visual light curves of the different supernova types all depend at late times 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. 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.
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. Studies of cosmology today 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 847keV and 1238keV gamma rays were first detected only in 2014.[103] 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 becomes dominant from the remaining cobalt-56, although this portion of the light curve has been little-studied.
Type Ib and Ic light curves are basically 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.
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,[104] 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.[47]
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.[47]
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.
Large numbers of supernovae have been catalogued and classified to provide distance candles and test models. 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[105][106] 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:
a. ^ Faint types may be a distinct sub-class. Bright types may be a continuum from slightly over-luminous to hypernovae.
b. ^ 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.
c. ^ Order of magnitude kinetic energy. Total electromagnetic radiated energy is usually lower, (theoretical) neutrino energy much higher.
d. ^ Probably a heterogeneous group, any of the other types embedded in nebulosity.
Asymmetry
The pulsar in the Crab nebula is travelling at 375 km/s relative to the nebula.[107]
A long-standing puzzle surrounding type II supernovae is why the remaining compact object receives a large velocity away from the epicentre;[108] pulsars, and thus neutron stars, are observed to have high 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 and jet production during neutron star formation.
One possible explanation for this asymmetry is large-scale convection above the core. The convection can create variations in the local abundances of elements, resulting in uneven nuclear burning during the collapse, bounce and resulting expansion.[109]
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.[110][111] (A similar model is now favored for explaining long gamma-ray bursts.)
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 polarization of the emitted light.[112]
Energy output
The radioactive decays of nickel-56 and cobalt-56 that produce a supernova visible light curve
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.
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. 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.
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 end 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.[113]
Core collapse supernovae are on average visually fainter than type Ia supernovae, but the total energy released is far higher. In these type of supernovae, the gravitational potential energy is converted into kinetic energy that compresses and collapses the core, initially producing electron neutrinos from disintegrating nucleons, followed by all flavours of thermal neutrinos from the super-heated neutron star core. Around 1% of these neutrinos are thought to deposit sufficient energy into the outer layers of the star to drive the resulting catastrophe, but again the details cannot be reproduced exactly in current models. Kinetic energies and nickel yields are somewhat lower than type Ia supernovae, hence the lower peak visual luminosity of type II supernovae, but energy from the de-ionisation of the many solar masses of remaining hydrogen can contribute to a much slower decline in luminosity and produce the plateau phase seen in the majority of core collapse supernovae.
Energetics of supernovae Supernova Approximate total energy
1044 joules (foe)c Ejected Ni
(solar masses) Neutrino energy
(foe) Kinetic energy
(foe) Electromagnetic radiation
(foe)
Type Ia[113][114][115] 1.5 0.4 – 0.8 0.1 1.3 – 1.4 ~0.01
Core collapse[116][117] 100 (0.01) – 1 100 1 0.001 – 0.01
Hypernova 100 ~1 1–100 1–100 ~0.1
Pair instability[84] 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. 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.
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.
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.
Progenitor
File:Artist's impression time-lapse of distant supernovae.webmPlay media
Shown in this sped-up artist's impression, is a collection of distant galaxies, the occasional supernova can be seen. Each of these exploding stars briefly rivals the brightness of its host galaxy.
The supernova classification type is closely tied to the type of star at the time of the collapse. The occurrence of each type of supernova depends dramatically on the metallicity, and hence the age of the host galaxy.
Type Ia supernovae are produced from white dwarf stars in binary systems and occur in all galaxy types. 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.
Type Ib/c and II-L, and possibly most type IIn, supernovae are only thought to be produced from stars having near-solar metallicity levels that result in high mass loss from massive stars, hence they are less common in older, more-distant galaxies. 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[91] 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%
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. It is now proposed 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.[118] 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.[119][120]
Isolated neutron star in the Small Magellanic Cloud
Until just a few decades ago, hot supergiants were not considered likely to explode, but observations have shown otherwise. 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.[118][121] 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.[122] 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.[118]
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.[118] 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.[123] 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.[91] 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.[118]
Other impacts
Source of heavy elements
Main articles: Stellar nucleosynthesis and Supernova nucleosynthesis
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,[124][125][126] though the theoretical abundances of the elements produced or seen in the spectra varies significantly depending on the various supernova types.[126] Type Ia supernovae produce mainly silicon and iron-peak elements, metals such as nickel and iron.[127][128] 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. [129] The bulk of the material ejected by type II supernovae is hydrogen and helium.[130] 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,[131] although neutron star mergers may be the main astrophysical source for many of these elements.[124][132]
In the modern universe, old asymptotic giant branch (AGB) stars are the dominant source of dust from s-process elements, oxides, and carbon.[124][133] However, in the early universe, before AGB stars formed, supernovae may have been the main source of dust.[134]
Role in stellar evolution
Main article: Supernova remnant
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.[135]
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 and supernovae. Supernovae tend to enrich the surrounding interstellar medium with elements other than hydrogen and helium, which usually astronomers refer to as "metals".
These injected elements ultimately enrich the molecular clouds that are the sites of star formation.[136] 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, and may decisively influence the possibility of having planets orbiting it.
The kinetic energy of an expanding supernova remnant can trigger star formation by compressing nearby, dense molecular clouds in space.[137] The increase in turbulent pressure can also prevent star formation if the cloud is unable to lose the excess energy.[138]
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.[139]
On 1 June 2020, astronomers reported narrowing down the source of Fast Radio Bursts (FRBs), which may now plausibly include "compact-object mergers and magnetars arising from normal core collapse supernovae".[140][141]
Cosmic rays
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 SNR impact on interstellar material.[142]
Gravitational waves
Supernovae are potentially strong galactic sources of gravitational waves,[143] 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.[144]
Effect on Earth
Main article: Near-Earth supernova
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 3000 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.[145][146][147] 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 levels of nitrogen oxides, which became trapped in the ice.[148]
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 (see below).[149] Recent estimates predict that 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.[150]
Milky Way candidates
Main article: List of supernova candidates
The nebula around Wolf–Rayet star WR124, which is located at a distance of about 21,000 light-years[151]
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 isn't 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 our galaxy is estimated to be between 2 and 12 per century, although we haven't actually observed one for several centuries.[99]
Statistically, the next supernova is likely to be produced from an otherwise unremarkable red supergiant, but 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.[152] Only eight of them are known, and only four of those are in the Milky Way.[153]
A number of close or well known stars have been identified as possible core collapse supernova candidates: the red supergiants Antares and Betelgeuse;[154] the yellow hypergiant Rho Cassiopeiae;[155] the luminous blue variable Eta Carinae that has already produced a supernova impostor;[156] and the brightest component, a Wolf–Rayet star, in the Regor or Gamma Velorum system.[157] Others have gained notoriety as possible, although not very likely, progenitors for a gamma-ray burst; for example WR 104.[158]
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.[159] The nearest known Type Ia supernova candidate is IK Pegasi (HR 8210), located at a distance of 150 light-years,[160] but observations suggest it will be several million years before the white dwarf can accrete the critical mass required to become a type Ia supernova.[161]
See also
Astronomy portal iconStar portal Space portal
Kilonova – Supernova formed from a neutron star merger
List of supernovae
List of supernova remnants
Quark-nova – Hypothetical violent explosion resulting from conversion of a neutron star to a quark star
Supernovae in fiction – List of supernovae appearances in fictional works
Timeline of white dwarfs, neutron stars, and supernovae – Chronological list of developments in knowledge and records
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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.
Iwamoto, K. (2006). "Neutrino Emission from Type Ia Supernovae". AIP Conference Proceedings. 847: 406–408. Bibcode:2006AIPC..847..406I. doi:10.1063/1.2234440.
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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.
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.
Smartt, Stephen J.; Thompson, Todd A.; Kochanek, Christopher S. (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.
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.
Georgy, C. (2012). "Yellow supergiants as supernova progenitors: An indication of strong mass loss for red supergiants?". Astronomy and Astrophysics. 538: L8–L2.arXiv:1111.7003. Bibcode:2012A&A...538L...8G. doi:10.1051/0004-6361/201118372. S2CID 55001976.
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 and Astrophysics. 544: L11. arXiv:1207.3683. Bibcode:2012A&A...544L..11Y. doi:10.1051/0004-6361/201219790. S2CID 118596795.
Groh, J. H.; Meynet, G.; Ekström, S. (2013). "Massive star evolution: Luminous blue variables as unexpected supernova progenitors". Astronomy and Astrophysics. 550: L7.arXiv:1301.1519. Bibcode:2013A&A...550L...7G. doi:10.1051/0004-6361/201220741. S2CID 119227339.
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 and Astrophysics. 544: L11. arXiv:1207.3683. Bibcode:2012A&A...544L..11Y. doi:10.1051/0004-6361/201219790. S2CID 118596795.
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.
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 and Astrophysics. 421 (2): 613–621. arXiv:astro-ph/0401499. Bibcode:2004A&A...421..613F. doi:10.1051/0004-6361:20034140. S2CID 16257700.
Truran, J. W. (1977). "Supernova Nucleosynthesis". In Schramm, D. N. (ed.). Supernovae. Astrophysics and Space Science Library. 66. Springer. pp. 145–158. doi:10.1007/978-94-010-1229-4_14. ISBN 978-94-010-1231-7.
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.
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.
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.
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.
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.
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.
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.
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.
Cox, D. P. (1972). "Cooling and Evolution of a Supernova Remnant". Astrophysical Journal. 178: 159. Bibcode:1972ApJ...178..159C. doi:10.1086/151775.
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.
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.
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.
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.
Starr, Michelle (1 June 2020). "Astronomers Just Narrowed Down The Source of Those Powerful Radio Signals From Space". ScienceAlert.com. Retrieved 2 June 2020.
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.
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.
Ott, C. D.; et al. (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.
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.
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.
Knie, K.; et al. (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.
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.
"In Brief" . Scientific American. 300 (5): 28. 2009. Bibcode:2009SciAm.300e..28.. doi:10.1038/scientificamerican0509-28a.
Gorelick, M. (2007). "The Supernova Menace". Sky & Telescope. 113 (3): 26. Bibcode:2007S&T...113c..26G.
Gehrels, N.; et al. (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.
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.
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 and Astrophysics. 581: A110. arXiv:1507.00839. Bibcode:2015A&A...581A.110T. doi:10.1051/0004-6361/201425390. S2CID 56093231.
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 and Astrophysics. 559: A72. arXiv:1310.2849. Bibcode:2013A&A...559A..72T. doi:10.1051/0004-6361/201322155. S2CID 216079684.
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.
Lobel, A.; et al. (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.
Van Boekel, R.; et al. (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.
Thielemann, F.-K.; Hirschi, R.; Liebendörfer, M.; Diehl, R. (2011). "Massive Stars and Their Supernovae". Astronomy with Radioactivities. Lecture Notes in Physics. 812. p. 153.arXiv:1008.2144. doi:10.1007/978-3-642-12698-7_4. ISBN 978-3-642-12697-0. S2CID 119254840.
Tuthill, P. G.; et al. (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.
Thoroughgood, T. D.; et al. (2002). "The recurrent nova U Scorpii — A type Ia supernova progenitor". The Physics of Cataclysmic Variables and Related Objects. 261. San Francisco, CA: Astronomical Society of the Pacific.arXiv:astro-ph/0109553. Bibcode:2002ASPC..261...77T.
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.
Vennes, S.; Kawka, A. (2008). "On the empirical evidence for the existence of ultramassive white dwarfs". Monthly Notices of the Royal Astronomical Society. 389 (3): 1367. arXiv:0806.4742. Bibcode:2008MNRAS.389.1367V. doi:10.1111/j.1365-2966.2008.13652.x. S2CID 15349194.
Further reading
Branch, D.; Wheeler, J. C. (2017). Supernova Explosions. [Springer]. ISBN 978-3-662-55052-6. A research-level book, 721 pages
"Introduction to Supernova Remnants". NASA/GSFC. 2007-10-04. Retrieved 2011-03-15.
Bethe, H. A. (1990). "Supernovae". Physics Today. 43 (9): 736–739. Bibcode:1990PhT....43i..24B. doi:10.1063/1.881256.
Croswell, K. (1996). The Alchemy of the Heavens: Searching for Meaning in the Milky Way. Anchor Books. ISBN 978-0-385-47214-2. A popular-science account.
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. An article describing spectral classes of supernovae.
Takahashi, K.; Sato, K.; Burrows, A.; Thompson, T. A. (2003). "Supernova Neutrinos, Neutrino Oscillations, and the Mass of the Progenitor Star". Physical Review D. 68 (11): 77–81.arXiv:hep-ph/0306056. Bibcode:2003PhRvD..68k3009T. doi:10.1103/PhysRevD.68.113009. S2CID 119390151. A good review of supernova events.
Hillebrandt, W.; Janka, H.-T.; Müller, E. (2006). "How to Blow Up a Star" . Scientific American. 295 (4): 42–49. Bibcode:2006SciAm.295d..42H. doi:10.1038/scientificamerican1006-42. PMID 16989479.
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.
External links
"RSS news feed" (RSS). The Astronomer's Telegram. Retrieved 2006-11-28.
Tsvetkov, D. Yu.; Pavlyuk, N. N.; Bartunov, O. S.; Pskovskii, Y. P. "Sternberg Astronomical Institute Supernova Catalogue". Sternberg Astronomical Institute, Moscow University. Retrieved 2006-11-28. A searchable catalog.
"The Open Supernova Catalog". Retrieved 2016-02-02. An open-access catalog of supernova light curves and spectra.
"List of Supernovae with IAU Designations". IAU: Central Bureau for Astronomical Telegrams. Retrieved 2010-10-25.
Overbye, D. (2008-05-21). "Scientists See Supernova in Action". The New York Times. Retrieved 2008-05-21.
"How to blow up a star". Elizabeth Gibney. Nature. 2018-04-18. Retrieved 2018-04-20.
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Supernovae
Classes
Type Ia Type Ib and Ic Type II (IIP, IIL, IIn, and IIb) Hypernova Superluminous Pair-instability
Physics of
Calcium-rich Carbon detonation Foe Near-Earth Phillips relationship Nucleosynthesis
P-process R-process Neutrinos
Related
Imposter
pulsational pair-instability Failed Gamma-ray burst Kilonova Luminous red nova Nova Pulsar kick Quark-nova Symbiotic nova
Progenitors
Hypergiant
yellow Luminous blue variable Supergiant
blue red yellow White dwarf
related links Wolf–Rayet star
Remnants
Supernova remnant
Pulsar wind nebula Neutron star
pulsar magnetar related links Stellar black hole
related links Compact star
quark star exotic star Zombie star Local Bubble Superbubble
Orion–Eridanus
Discovery
Guest star History of supernova observation Timeline of white dwarfs, neutron stars, and supernovae
Lists
Candidates Notable Massive stars Most distant Remnants In fiction
Notable
Barnard's Loop Cassiopeia A Crab
Crab Nebula iPTF14hls Tycho's Kepler's SN 1987A SN 185 SN 1006 SN 2003fg Remnant G1.9+0.3 SN 2007bi SN 2011fe SN 2014J SN Refsdal Vela Remnant
Research
ASAS-SN Calán/Tololo Survey High-Z Supernova Search Team Katzman Automatic Imaging Telescope Monte Agliale Supernovae and Asteroid Survey Nearby Supernova Factory Sloan Supernova Survey Supernova/Acceleration Probe Supernova Cosmology Project SuperNova Early Warning System Supernova Legacy Survey Texas Supernova Search
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Accretion Molecular cloud Bok globule Young stellar object
Protostar Pre-main-sequence Herbig Ae/Be T Tauri FU Orionis Herbig–Haro object Hayashi track Henyey track
Main sequence Red-giant branch Horizontal branch
Red clump Asymptotic giant branch
super-AGB Blue loop Protoplanetary nebula Planetary nebula PG1159 Dredge-up OH/IR Instability strip Luminous blue variable Blue straggler Stellar population Supernova Superluminous supernova / Hypernova
Early Late Main sequence
O B A F G K M Brown dwarf WR OB Subdwarf
O B Subgiant Giant
Blue Red Yellow Bright giant Supergiant
Blue Red Yellow Hypergiant
Yellow Carbon
S CN CH White dwarf Chemically peculiar
Am Ap/Bp HgMn Helium-weak Barium Extreme helium Lambda Boötis Lead Technetium Be
Shell B[e]
White dwarf
Helium planet Black dwarf Neutron
Radio-quiet Pulsar
Binary X-ray Magnetar Stellar black hole X-ray binary
Burster
Hypothetical
Blue dwarf Green Black dwarf Exotic
Boson Electroweak Strange Preon Planck Dark Dark-energy Quark Q Black Gravastar Frozen Quasi-star Thorne–Żytkow object Iron Blitzar
Deuterium burning Lithium burning Proton–proton chain CNO cycle Helium flash Triple-alpha process Alpha process Carbon burning Neon burning Oxygen burning Silicon burning S-process R-process Fusor Nova
Symbiotic Remnant Luminous red nova
Structure
Core Convection zone
Microturbulence Oscillations Radiation zone Atmosphere
Photosphere Starspot Chromosphere Stellar corona Stellar wind
Bubble Bipolar outflow Accretion disk Asteroseismology
Helioseismology Eddington luminosity Kelvin–Helmholtz mechanism
Properties
Designation Dynamics Effective temperature Luminosity Kinematics Magnetic field Absolute magnitude Mass Metallicity Rotation Starlight Variable Photometric system Color index Hertzsprung–Russell diagram Color–color diagram
Star systems
Binary
Contact Common envelope Eclipsing Symbiotic Multiple Cluster
Open Globular Super Planetary system
Earth-centric
observations
Sun
Solar System Sunlight Pole star Circumpolar Constellation Asterism Magnitude
Apparent Extinction Photographic Radial velocity Proper motion Parallax Photometric-standard
Lists
Proper names
Arabic Chinese Extremes Most massive Highest temperature Lowest temperature Largest volume Smallest volume Brightest
Historical Most luminous Nearest
Nearest bright With exoplanets Brown dwarfs White dwarfs Milky Way novae Supernovae
Candidates Remnants Planetary nebulae Timeline of stellar astronomy
Related articles
Substellar object
Brown dwarf Sub-brown dwarf Planet Galactic year Galaxy Guest Gravity Intergalactic Planet-hosting stars Tidal disruption event
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Novae
Recurrent novae
T Coronae Borealis IM Normae RS Ophiuchi T Pyxidis U Scorpii
Classical novae
CK Vulpeculae (1670) T Scorpii (1860) T Aurigae (1891) Nova Sagittarii 1898 (1898) V606 Aquilae (1899) GK Persei (1901) DM Geminorum (1903) V604 Aquilae (1905) DI Lacertae (1910) DN Geminorum (1912) V603 Aquilae (1918) HR Lyrae (1919) V849 Ophiuchi (1919) V476 Cygni (1920) RR Pictoris (1925) XX Tauri (1927) DQ Herculis (1934) CP Lacertae (1936) BT Monocerotis (1939) CP Puppis (1942) V500 Aquilae (1943) CT Serpentis (1948) DK Lacertae (1950) RW Ursae Minoris (1956) V446 Herculis (1960) V533 Herculis (1963) HR Delphini (1967) FH Serpentis (1970) V1500 Cygni (1975) V373 Scuti (1975) NQ Vulpeculae (1976) V1668 Cygni (1978) QU Vulpeculae (1984) V842 Centauri (1986) V838 Herculis (1991) V1974 Cygni (1992) V382 Velorum (1999) V1494 Aquilae (1999) V445 Puppis (2000) V598 Puppis (2007) V1280 Scorpii (2007) KT Eridani (2009) V339 Delphini (2013) V1369 Centauri (2013) V5856 Sagittarii (2016)
See also: List of novae in the Milky Way galaxy
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Variable stars
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Black holes
Types
Schwarzschild Rotating Charged Virtual Kugelblitz Primordial Planck particle
Size
Micro
Extremal Electron Stellar
Microquasar Intermediate-mass Supermassive
Active galactic nucleus Quasar Blazar
Formation
Stellar evolution Gravitational collapse Neutron star
Related links Tolman–Oppenheimer–Volkoff limit White dwarf
Related links Supernova
Related links Hypernova Gamma-ray burst Binary black hole
Properties
Gravitational singularity
Ring singularity Theorems Event horizon Photon sphere Innermost stable circular orbit Ergosphere
Penrose process Blandford–Znajek process Accretion disk Hawking radiation Gravitational lens Bondi accretion M–sigma relation Quasi-periodic oscillation Thermodynamics
Immirzi parameter Schwarzschild radius Spaghettification
Issues
Black hole complementarity Information paradox Cosmic censorship ER=EPR Final parsec problem Firewall (physics) Holographic principle No-hair theorem
Metrics
Schwarzschild (Derivation) Kerr Reissner–Nordström Kerr–Newman Hayward
Alternatives
Nonsingular black hole models Black star Dark star Dark-energy star Gravastar Magnetospheric eternally collapsing object Planck star Q star Fuzzball
Analogs
Optical black hole Sonic black hole
Lists
Black holes Most massive Nearest Quasars Microquasars
Related
Black Hole Initiative Black hole starship Compact star Exotic star
Quark star Preon star Gamma-ray burst progenitors Gravity well Hypercompact stellar system Membrane paradigm Naked singularity Quasi-star Rossi X-ray Timing Explorer Timeline of black hole physics White hole Wormhole
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Neutron star
Types
Single pulsars
Magnetar
Soft gamma repeater Anomalous X-ray Rotating radio transient
Binary pulsars
Binary X-ray pulsar
X-ray binary X-ray burster List Millisecond Be/X-ray Spin-up
Properties
Blitzar
Fast radio burst Bondi accretion Chandrasekhar limit Gamma-ray burst Glitch Neutronium Neutron-star oscillation Optical Pulsar kick Quasi-periodic oscillation Relativistic Rp-process Starquake Timing noise Tolman–Oppenheimer–Volkoff limit Urca process
Related
Gamma-ray burst progenitors Asteroseismology Compact star
Quark star Exotic star Supernova
Supernova remnant Related links Hypernova Kilonova Neutron star merger Quark-nova White dwarf
Related links Stellar black hole
Related links Radio star Pulsar planet Pulsar wind nebula Thorne–Żytkow object
Discovery
LGM-1 Centaurus X-3 Timeline of white dwarfs, neutron stars, and supernovae
Satellite
investigation
Rossi X-ray Timing Explorer Fermi Gamma-ray Space Telescope Compton Gamma Ray Observatory Chandra X-ray Observatory
Other
X-ray pulsar-based navigation Tempo software program Astropulse The Magnificent Seven
vte
Stellar core collapse
Stars
Formation Evolution Structure Core Metallicity Stellar physics Stellar plasma Supergiant Variable star Cataclysmic variable star Binary star
X-ray binary Super soft X-ray source
Stellar processes
Nuclear fusion Surface fusion Nucleosynthesis
R-process RP-process Supernova nucleosynthesis Accretion (Bondi accretion) Electron capture Carbon detonation / deflagration Gamma-ray burst Helium flash Orbital decay
Collapse
Gravitational collapse Chandrasekhar limit Tolman–Oppenheimer–Volkoff limit
Supernovae
Type Ia Type Ib and Ic Type II Pair-instability Hypernova Quark-nova Nebula Remnant More...
Compact and exotic objects
Neutron star
Pulsar Quasar Magnetar Radio-quiet White dwarf Black hole Exotic star Quark star Electroweak star Observational timeline
Particles, forces, and interactions
Elementary particles
Proton Neutron Electron Neutrino Fundamental interactions
Strong interaction Weak interaction Gravitation
Pair production Inverse beta decay (electron capture) Degeneracy pressure Electron degeneracy pressure Pauli exclusion principle More...
Quantum theory
Quantum mechanics
Introduction Basic concepts Quantum electrodynamics Quantum hydrodynamics Quantum chromodynamics (QCD) Lattice QCD Color confinement Deconfinement
Degenerate matter
Neutron matter QCD matter Quark matter Quark–gluon plasma Preon matter Strangelet Strange matter
Related topics
Astronomy Astrophysics Nuclear astrophysics Physical cosmology Physics of shock waves
Portals
Physics Astronomy Stars Space
Portal
vte
Gravitational-wave astronomy
Gravitational wave Gravitational-wave observatory
Detectors
Resonant mass
antennas
Active
NAUTILUS (IGEC) AURIGA (IGEC) MiniGRAIL Mario Schenberg
Past
EXPLORER (IGEC) ALLEGRO (IGEC) NIOBE (IGEC) Stanford gravitational wave detector ALTAIR GEOGRAV AGATA Weber bar
Proposed
TOBA
Past proposals
GRAIL (downsized to MiniGRAIL) TIGA SFERA Graviton (downsized to Mario Schenberg)
Ground-based
Interferometers
Active
AIGO (ACIGA) CLIO Fermilab holometer GEO600 Advanced LIGO (LIGO Scientific Collaboration) KAGRA Advanced Virgo (European Gravitational Observatory)
Past
TAMA 300 TAMA 20, later known as LISM TENKO-100 Caltech 40m interferometer
Planned
INDIGO (LIGO-India)
Proposed
Cosmic Explorer Einstein Telescope
Past proposals
AIGO (LIGO-Australia)
Space-based
interferometers
Planned
LISA
Proposed
Big Bang Observer DECIGO TianQin
Pulsar timing arrays
EPTA IPTA NANOGrav PPTA
Data analysis
Einstein@Home PyCBC Zooniverse: Gravity Spy
Observations
Events
List of observations First observation (GW150914) GW151012 GW151226 GW170104 GW170608 GW170729 GW170809 GW170814 GW170817 (first neutron star merger) GW170818 GW170823 GW190412 GW190521 (first-ever light from bh-bh merger) GW190814 (first-ever "mass gap" collision)
Methods
Direct detection
Laser interferometers Resonant mass detectors Proposed: Atom interferometers Indirect detection
B-modes of CMB Pulsar timing array Binary pulsar
Theory
General relativity Tests of general relativity Metric theories Graviton
Effects / properties
Polarization Spin-flip Redshift Travel with speed of light h strain Chirp signal (chirp mass) Carried energy
Types / sources
Stochastic
Cosmic inflation-quantum fluctuation Phase transition Binary inspiral
Supermassive black holes Stellar black holes Neutron stars EMRI Continuous
Rotating neutron star Burst
Supernova or from unknown sources Hypothesis
Colliding cosmic string and other unknown sources
vte
Astronomy in the medieval Islamic world
Astronomers
by century
8th
Ahmad Nahavandi Al-Fadl ibn Naubakht Muḥammad ibn Ibrāhīm al-Fazārī Mashallah ibn Athari Yaʿqūb ibn Ṭāriq
9th
Abu Maʿshar Abu Said Gorgani Al-Farghānī Al-Kindi Al-Mahani Abu Hanifa Dinawari Al-Ḥajjāj ibn Yūsuf Al-Marwazi Ali ibn Isa al-Asturlabi Banu Musa Iranshahri Khālid ibn ʿAbd al‐Malik Al-Khwārizmī Sahl ibn Bishr Thābit ibn Qurra Yahya ibn Abi Mansur
10th
al-Sufi Ibn Al-Adami al-Khojandi al-Khazin al-Qūhī Abu al-Wafa Ahmad ibn Yusuf al-Battani Al-Qabisi Ibn al-A'lam Al-Nayrizi Al-Saghani Aṣ-Ṣaidanānī Ibn Yunus Ibrahim ibn Sinan Ma Yize al-Sijzi Mariam al-Asturlabi Nastulus Abolfadl Harawi Haseb-i Tabari al-Majriti Abu al-Hasan al-Ahwazi
11th
Abu Nasr Mansur al-Biruni Ali ibn Ridwan Al-Zarqālī Ibn al-Samh Alhazen Avicenna Ibn al-Saffar Kushyar Gilani Said al-Andalusi Ibrahim ibn Said al-Sahli Ibn Muʿādh al-Jayyānī Al-Isfizari Ali ibn Khalaf
12th
Al-Bitruji Avempace Ibn Tufail Al-Kharaqī Al-Khazini Al-Samawal al-Maghribi Abu al-Salt Averroes Ibn al-Kammad Jabir ibn Aflah Omar Khayyam Sharaf al-Dīn al-Ṭūsī
13th
Ibn al-Banna' al-Marrakushi Ibn al‐Ha'im al‐Ishbili Jamal ad-Din Alam al-Din al-Hanafi Najm al‐Din al‐Misri Muhyi al-Dīn al-Maghribī Nasir al-Din al-Tusi Qutb al-Din al-Shirazi Shams al-Dīn al-Samarqandī Zakariya al-Qazwini al-Urdi al-Abhari Muhammad ibn Abi Bakr al‐Farisi Abu Ali al-Hasan al-Marrakushi Ibn Ishaq al-Tunisi Ibn al‐Raqqam Al-Ashraf Umar II Fakhr al-Din al- Akhlati
14th
Ibn al-Shatir Al-Khalili Ibn Shuayb al-Battiwi Abū al‐ʿUqūl Al-Wabkanawi Nizam al-Din Nishapuri al-Jadiri Sadr al-Shari'a al-Asghar
15th
Ali Kuşçu ʿAbd al‐Wājid Jamshīd al-Kāshī Kadızade Rumi Ulugh Beg Sibt al-Maridini Ibn al-Majdi al-Wafa'i al-Kubunani 'Abd al-'Aziz al-Wafa'i
16th
Al-Birjandi al-Khafri Bahāʾ al-dīn al-ʿĀmilī Piri Reis Takiyüddin
17th
Yang Guangxian Ahmad Khani Al Achsasi al Mouakket Mohammed al-Rudani
Topics
Works
Arabic star names Islamic calendar ʿAjā'ib al-makhlūqāt wa gharā'ib al-mawjūdāt Encyclopedia of the Brethren of Purity Tabula Rogeriana The Book of Healing The Remaining Signs of Past Centuries
Zij
Alfonsine tables Huihui Lifa Book of Fixed Stars Toledan Tables Zij-i Ilkhani Zij-i Sultani Sullam al-sama'
Instruments
Alidade Analog computer Aperture Armillary sphere Astrolabe Astronomical clock Celestial globe Compass Compass rose Dioptra Equatorial ring Equatorium Globe Graph paper Magnifying glass Mural instrument Navigational astrolabe Nebula Octant Planisphere Quadrant Sextant Shadow square Sundial Schema for horizontal sundials Triquetrum
Concepts
Almucantar Apogee Astrology in medieval Islam Astrophysics Axial tilt Azimuth Celestial mechanics Celestial spheres Circular orbit Deferent and epicycle Earth's rotation Eccentricity Ecliptic Elliptic orbit Equant Galaxy Geocentrism Gravitational potential energy Gravity Heliocentrism Inertia Islamic cosmology Moonlight Multiverse Muwaqqit Obliquity Parallax Precession Qibla Salah times Specific gravity Spherical Earth Sublunary sphere Sunlight Supernova Temporal finitism Trepidation Triangulation Tusi couple Universe
Institutions
Al-Azhar University House of Knowledge House of Wisdom University of Al Quaraouiyine Observatories
Constantinople (Taqi al-Din) Maragheh Samarkand (Ulugh Beg)
Influences
Babylonian astronomy Egyptian astronomy Hellenistic astronomy Indian astronomy
Influenced
Byzantine science Chinese astronomy Medieval European science Indian astronomy
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