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In gamma-ray astronomy, gamma-ray bursts (GRBs) are immensely energetic events occurring in distant galaxies which represent the brightest and "most powerful class of explosion in the universe." These extreme electromagnetic events are second only to the Big Bang as the most energetic and luminous phenomenon ever known. Gamma-ray bursts can last from ten milliseconds to several hours. After the initial flash of gamma rays, a longer-lived § afterglow is emitted, usually in the longer wavelengths of X-ray, ultraviolet, optical, infrared, microwave or radio frequencies.

The intense radiation of most observed GRBs is thought to be released during a supernova or superluminous supernova as a high-mass star implodes to form a neutron star or a black hole. From gravitational wave observations, § short-duration (sGRB) events describe a subclass of GRB signals that are now known to originate from the cataclysmic merger of binary neutron stars.

The sources of most GRB are billions of light years away from Earth, implying that the explosions are both extremely energetic (a typical burst releases as much energy in a few seconds as the Sun will in its entire 10-billion-year lifetime) and extremely rare (a few per galaxy per million years). All GRBs in recorded history have originated from outside the Milky Way galaxy, although a related class of phenomena, soft gamma repeaters, are associated with magnetars within our galaxy. This may be self-evident, since a gamma-ray burst in the Milky Way pointed directly at Earth would likely sterilize the planet or effect a mass extinction. The Late Ordovician mass extinction has been hypothesised by some researchers to have occurred as a result of such a gamma-ray burst.

GRB signals were first detected in 1967 by the Vela satellites, which were designed to detect covert nuclear weapons tests; after an "exhaustive" period of analysis, this was published as academic research in 1973. Following their discovery, hundreds of theoretical models were proposed to explain these bursts, such as collisions between comets and neutron stars. Little information was available to verify these models until the 1997 detection of the first X-ray and optical afterglows and direct measurement of their redshifts using optical spectroscopy, and thus their distances and energy outputs. These discoveries—and subsequent studies of the galaxies and supernovae associated with the bursts—clarified the distance and luminosity of GRBs, definitively placing them in distant galaxies.

History

Gamma-ray bursts were first observed in the late 1960s by the U.S. Vela satellites, which were built to detect gamma radiation pulses emitted by nuclear weapons tested in space. The United States suspected that the Soviet Union might attempt to conduct secret nuclear tests after signing the Nuclear Test Ban Treaty in 1963. On July 2, 1967, at 14:19 UTC, the Vela 4 and Vela 3 satellites detected a flash of gamma radiation unlike any known nuclear weapons signature. Uncertain what had happened but not considering the matter particularly urgent, the team at the Los Alamos National Laboratory, led by Ray Klebesadel, filed the data away for investigation. As additional Vela satellites were launched with better instruments, the Los Alamos team continued to find inexplicable gamma-ray bursts in their data. By analyzing the different arrival times of the bursts as detected by different satellites, the team was able to determine rough estimates for the sky positions of 16 bursts and definitively rule out a terrestrial or solar origin. Contrary to popular belief, the data was never classified. After thorough analysis, the findings were published in 1973 as an Astrophysical Journal article entitled "Observations of Gamma-Ray Bursts of Cosmic Origin".

Most early hypotheses of gamma-ray bursts posited nearby sources within the Milky Way Galaxy. From 1991, the Compton Gamma Ray Observatory (CGRO) and its Burst and Transient Source Explorer (BATSE) instrument, an extremely sensitive gamma-ray detector, provided data that showed the distribution of GRBs is isotropic – not biased towards any particular direction in space. If the sources were from within our own galaxy, they would be strongly concentrated in or near the galactic plane. The absence of any such pattern in the case of GRBs provided strong evidence that gamma-ray bursts must come from beyond the Milky Way. However, some Milky Way models are still consistent with an isotropic distribution.

Counterpart objects as candidate sources

For decades after the discovery of GRBs, astronomers searched for a counterpart at other wavelengths: i.e., any astronomical object in positional coincidence with a recently observed burst. Astronomers considered many distinct classes of objects, including white dwarfs, pulsars, supernovae, globular clusters, quasars, Seyfert galaxies, and BL Lac objects. All such searches were unsuccessful, and in a few cases particularly well-localized bursts (those whose positions were determined with what was then a high degree of accuracy) could be clearly shown to have no bright objects of any nature consistent with the position derived from the detecting satellites. This suggested an origin of either very faint stars or extremely distant galaxies. Even the most accurate positions contained numerous faint stars and galaxies, and it was widely agreed that final resolution of the origins of cosmic gamma-ray bursts would require both new satellites and faster communication.

Afterglow

Several models for the origin of gamma-ray bursts postulated that the initial burst of gamma rays should be followed by afterglow: slowly fading emission at longer wavelengths created by collisions between the burst ejecta and interstellar gas. Early searches for this afterglow were unsuccessful, largely because it is difficult to observe a burst's position at longer wavelengths immediately after the initial burst. The breakthrough came in February 1997 when the satellite BeppoSAX detected a gamma-ray burst (GRB 970228) and when the X-ray camera was pointed towards the direction from which the burst had originated, it detected fading X-ray emission. The William Herschel Telescope identified a fading optical counterpart 20 hours after the burst. Once the GRB faded, deep imaging was able to identify a faint, distant host galaxy at the location of the GRB as pinpointed by the optical afterglow.

Because of the very faint luminosity of this galaxy, its exact distance was not measured for several years. Well after then, another major breakthrough occurred with the next event registered by BeppoSAX, GRB 970508. This event was localized within four hours of its discovery, allowing research teams to begin making observations much sooner than any previous burst. The spectrum of the object revealed a redshift of z = 0.835, placing the burst at a distance of roughly 6 billion light years from Earth. This was the first accurate determination of the distance to a GRB, and together with the discovery of the host galaxy of 970228 proved that GRBs occur in extremely distant galaxies. Within a few months, the controversy about the distance scale ended: GRBs were extragalactic events originating within faint galaxies at enormous distances. The following year, GRB 980425 was followed within a day by a bright supernova (SN 1998bw), coincident in location, indicating a clear connection between GRBs and the deaths of very massive stars. This burst provided the first strong clue about the nature of the systems that produce GRBs.

More recent instruments - launched from 2000

BeppoSAX functioned until 2002 and CGRO (with BATSE) was deorbited in 2000. However, the revolution in the study of gamma-ray bursts motivated the development of a number of additional instruments designed specifically to explore the nature of GRBs, especially in the earliest moments following the explosion. The first such mission, HETE-2, was launched in 2000 and functioned until 2006, providing most of the major discoveries during this period. One of the most successful space missions to date, Swift, was launched in 2004 and as of May 2024 is still operational. Swift is equipped with a very sensitive gamma-ray detector as well as on-board X-ray and optical telescopes, which can be rapidly and automatically slewed to observe afterglow emission following a burst. More recently, the Fermi mission was launched carrying the Gamma-Ray Burst Monitor, which detects bursts at a rate of several hundred per year, some of which are bright enough to be observed at extremely high energies with Fermi's Large Area Telescope. Meanwhile, on the ground, numerous optical telescopes have been built or modified to incorporate robotic control software that responds immediately to signals sent through the Gamma-ray Burst Coordinates Network. This allows the telescopes to rapidly repoint towards a GRB, often within seconds of receiving the signal and while the gamma-ray emission itself is still ongoing.

The Space Variable Objects Monitor is a small X-ray telescope satellite for studying the explosions of massive stars by analysing the resulting gamma-ray bursts, developed by China National Space Administration (CNSA), Chinese Academy of Sciences (CAS) and the French Space Agency (CNES), launched on 22 June 2024 (07:00:00 UTC).

The Taiwan Space Agency is launching a cubesat called The Gamma-ray Transients Monitor to track GRBs and other bright gamma-ray transients with energies ranging from 50 keV to 2 MeV in Q4 2026.

Short bursts and other observations

New developments since the 2000s include the recognition of short gamma-ray bursts as a separate class (likely from merging neutron stars and not associated with supernovae), the discovery of extended, erratic flaring activity at X-ray wavelengths lasting for many minutes after most GRBs, and the discovery of the most luminous (GRB 080319B) and the former most distant (GRB 090423) objects in the universe. Prior to a flurry of discoveries from the James Webb Space Telescope, GRB 090429B was the most distant known object in the universe.

In October 2018, astronomers reported that GRB 150101B (detected in 2015) and GW170817, a gravitational wave event detected in 2017 (which has been associated with GRB 170817A, a burst detected 1.7 seconds later), may have been produced by the same mechanism—the merger of two neutron stars. The similarities between the two events, in terms of gamma ray, optical, and x-ray emissions, as well as to the nature of the associated host galaxies, were considered "striking", suggesting the two separate events may both be the result of the merger of neutron stars, and both may be a kilonova, which may be more common in the universe than previously understood, according to the researchers.

The highest energy light observed from a gamma-ray burst was one teraelectronvolt, from GRB 190114C in 2019. Although enormous for such a distant event, this energy is around 3 orders of magnitude lower than the highest energy light observed from closer gamma ray sources within our Milky Way galaxy, for example a 2021 event of 1.4 petaelectronvolts.

Classification

The light curves of gamma-ray bursts are extremely diverse and complex. No two gamma-ray burst light curves are identical, with large variation observed in almost every property: the duration of observable emission can vary from milliseconds to tens of minutes, there can be a single peak or several individual subpulses, and individual peaks can be symmetric or with fast brightening and very slow fading. Some bursts are preceded by a "precursor" event, a weak burst that is then followed (after seconds to minutes of no emission at all) by the much more intense "true" bursting episode. The light curves of some events have extremely chaotic and complicated profiles with almost no discernible patterns.

Although some light curves can be roughly reproduced using certain simplified models, little progress has been made in understanding the full diversity observed. Many classification schemes have been proposed, but these are often based solely on differences in the appearance of light curves and may not always reflect a true physical difference in the progenitors of the explosions. However, plots of the distribution of the observed duration for a large number of gamma-ray bursts show a clear bimodality, suggesting the existence of two separate populations: a "short" population with an average duration of about 0.3 seconds and a "long" population with an average duration of about 30 seconds. Both distributions are very broad with a significant overlap region in which the identity of a given event is not clear from duration alone. Additional classes beyond this two-tiered system have been proposed on both observational and theoretical grounds.

Short gamma-ray bursts

Events with a duration of less than about two seconds are classified as short gamma-ray bursts (sGRB). These account for about 30% of gamma-ray bursts, but until 2005, no afterglow had been successfully detected from any short event and little was known about their origins. Following this, several dozen short gamma-ray burst afterglows were detected and localized, several of them associated with regions of little or no star formation, such as large elliptical galaxies. This ruled out a link to massive stars, confirming the short events to be physically distinct from long events. In addition, there had been no association with supernovae.

The true nature of these objects was thus initially unknown, but the leading hypothesis was that they originated from the mergers of binary neutron stars or a neutron star with a black hole. Such mergers were hypothesized to produce kilonovae, and evidence for a kilonova associated with short GRB 130603B was reported in 2013. The mean duration of sGRB events of around 200 milliseconds implied (due to causality) that the sources must be of very small physical diameter in stellar terms: less than 0.2 light-seconds (60,000 km or 37,000 miles) – about four times the Earth's diameter. The observation of minutes to hours of X-ray flashes after an sGRB was seen as consistent with small particles of a precursor object like a neutron star initially being swallowed by a black hole in less than two seconds, followed by some hours of lower-energy events as remaining fragments of tidally disrupted neutron star material (no longer neutronium) would remain in orbit, spiraling into the black hole over a longer period of time. The origin of short gamma-ray bursts in kilonovae was finally conclusively established in 2017, when short GRB 170817A co-occurred with the detection of gravitational wave GW170817, a signal from the merger of two neutron stars.

Unrelated to these cataclysmic origins, short-duration gamma-ray signals are also produced by giant flares from soft gamma repeaters in our own—or nearby—galaxies.

Long gamma-ray bursts

Most observed events (70%) have a duration of greater than two seconds and are classified as long gamma-ray bursts. Because these events constitute the majority of the population and because they tend to have the brightest afterglows, they have been observed in much greater detail than their short counterparts. Almost every well-studied long gamma-ray burst has been linked to a galaxy with rapid star formation, and in many cases to a core-collapse supernova as well, unambiguously associating long GRBs with the deaths of massive stars. Long GRB afterglow observations, at high redshift, are also consistent with the GRB having originated in star-forming regions.

In December 2022, astronomers reported the observation of GRB 211211A for 51 seconds, the first evidence of a long GRB produced by a neutron star merger. Following this, GRB 191019A (2019, 64s) and GRB 230307A (2023, 35s) have been argued to signify an emerging class of long GRBs which originate from neutron star mergers.

Ultra-long gamma-ray bursts

ulGRB are defined as GRB lasting more than 10,000 seconds, covering the upper range to the limit of the GRB duration distribution. They have been proposed to form a separate class, caused by the collapse of a blue supergiant star, a tidal disruption event or a new-born magnetar. Only a small number have been identified to date, their primary characteristic being their gamma ray emission duration. The most studied ultra-long events include GRB 101225A and GRB 111209A. The low detection rate may be a result of low sensitivity of current detectors to long-duration events, rather than a reflection of their true frequency. A 2013 study, on the other hand, shows that the existing evidence for a separate ultra-long GRB population with a new type of progenitor is inconclusive, and further multi-wavelength observations are needed to draw a firmer conclusion.

Energetics

Gamma-ray bursts are very bright as observed from Earth despite their typically immense distances. An average long GRB has a bolometric flux comparable to a bright star of our galaxy despite a distance of billions of light years (compared to a few tens of light years for most visible stars). Most of this energy is released in gamma rays, although some GRBs have extremely luminous optical counterparts as well. GRB 080319B, for example, was accompanied by an optical counterpart that peaked at a visible magnitude of 5.8, comparable to that of the dimmest naked-eye stars despite the burst's distance of 7.5 billion light years. This combination of brightness and distance implies an extremely energetic source. Assuming the gamma-ray explosion to be spherical, the energy output of GRB 080319B would be within a factor of two of the rest-mass energy of the Sun (the energy which would be released were the Sun to be converted entirely into radiation).

Gamma-ray bursts are thought to be highly focused explosions, with most of the explosion energy collimated into a narrow jet. The jets of gamma-ray bursts are ultrarelativistic, and are the most relativistic jets in the universe. The matter in gamma-ray burst jets may also become superluminal, or faster than the speed of light in the jet medium, with there also being effects of time reversibility. The approximate angular width of the jet (that is, the degree of spread of the beam) can be estimated directly by observing the achromatic "jet breaks" in afterglow light curves: a time after which the slowly decaying afterglow begins to fade rapidly as the jet slows and can no longer beam its radiation as effectively. Observations suggest significant variation in the jet angle from between 2 and 20 degrees.

Because their energy is strongly focused, the gamma rays emitted by most bursts are expected to miss the Earth and never be detected. When a gamma-ray burst is pointed towards Earth, the focusing of its energy along a relatively narrow beam causes the burst to appear much brighter than it would have been were its energy emitted spherically. The total energy of typical gamma-ray bursts has been estimated at 3 × 10 J, – which is larger than the total energy (10 J) of ordinary supernovae (type Ia, Ibc, II), with gamma-ray bursts also being more powerful than the typical supernova. Very bright supernovae have been observed to accompany several of the nearest GRBs. Further support for focusing of the output of GRBs comes from observations of strong asymmetries in the spectra of nearby type Ic supernovae and from radio observations taken long after bursts when their jets are no longer relativistic.

However, a competing model, the binary-driven hypernova model, developed by Remo Ruffini and others at ICRANet, accepts the extreme isotropic energy totals as being true, with there being no need to correct for beaming. They also note that the extreme beaming angles in the standard "fireball" model have never been physically corroborated.

With the discovery of GRB 190114C, astronomers may have been missing half of the total energy that gamma-ray bursts produce, with Konstancja Satalecka, an astrophysicist at the German Electron Synchrotron, stating that "Our measurements show that the energy released in very-high-energy gamma-rays is comparable to the amount radiated at all lower energies taken together".

Short (time duration) GRBs appear to come from a lower-redshift (i.e. less distant) population and are less luminous than long GRBs. The degree of beaming in short bursts has not been accurately measured, but as a population they are likely less collimated than long GRBs or possibly not collimated at all in some cases.

Progenitors

Because of the immense distances of most gamma-ray burst sources from Earth, identification of the progenitors, the systems that produce these explosions, is challenging. The association of some long GRBs with supernovae and the fact that their host galaxies are rapidly star-forming offer very strong evidence that long gamma-ray bursts are associated with massive stars. The most widely accepted mechanism for the origin of long-duration GRBs is the collapsar model, in which the core of an extremely massive, low-metallicity, rapidly rotating star collapses into a black hole in the final stages of its evolution. Matter near the star's core rains down towards the center and swirls into a high-density accretion disk. The infall of this material into a black hole drives a pair of relativistic jets out along the rotational axis, which pummel through the stellar envelope and eventually break through the stellar surface and radiate as gamma rays. Some alternative models replace the black hole with a newly formed magnetar, although most other aspects of the model (the collapse of the core of a massive star and the formation of relativistic jets) are the same.

However, a new model which has gained support and was developed by the Italian astrophysicist Remo Ruffini and other scientists at ICRANet is that of the binary-driven hypernova (BdHN) model. The model succeeds and improves upon both the fireshell model and the induced gravitational collapse (IGC) paradigm suggested before, and explains all aspects of gamma-ray bursts. The model posits long gamma-ray bursts as occurring in binary systems with a carbon–oxygen core and a companion neutron star or a black hole. Furthermore, the energy of GRBs in the model is isotropic instead of collimated. The creators of the model have noted the numerous drawbacks of the standard "fireball" model as motivation for developing the model, such as the markedly different energetics for supernova and gamma-ray bursts, and the fact that the existence of extremely narrow beaming angles have never been observationally corroborated.

The closest analogs within the Milky Way galaxy of the stars producing long gamma-ray bursts are likely the Wolf–Rayet stars, extremely hot and massive stars, which have shed most or all of their hydrogen envelope. Eta Carinae, Apep, and WR 104 have been cited as possible future gamma-ray burst progenitors. It is unclear if any star in the Milky Way has the appropriate characteristics to produce a gamma-ray burst.

The massive-star model probably does not explain all types of gamma-ray burst. There is strong evidence that some short-duration gamma-ray bursts occur in systems with no star formation and no massive stars, such as elliptical galaxies and galaxy halos. The favored hypothesis for the origin of most short gamma-ray bursts is the merger of a binary system consisting of two neutron stars. According to this model, the two stars in a binary slowly spiral towards each other because gravitational radiation releases energy until tidal forces suddenly rip the neutron stars apart and they collapse into a single black hole. The infall of matter into the new black hole produces an accretion disk and releases a burst of energy, analogous to the collapsar model. Numerous other models have also been proposed to explain short gamma-ray bursts, including the merger of a neutron star and a black hole, the accretion-induced collapse of a neutron star, or the evaporation of primordial black holes.

An alternative explanation proposed by Friedwardt Winterberg is that in the course of a gravitational collapse and in reaching the event horizon of a black hole, all matter disintegrates into a burst of gamma radiation.

Tidal disruption events

This class of GRB-like events was first discovered through the detection of Swift J1644+57 (originally classified as GRB 110328A) by the Swift Gamma-Ray Burst Mission on 28 March 2011. This event had a gamma-ray duration of about 2 days, much longer than even ultra-long GRBs, and was detected in many frequencies for months and years after. It occurred at the center of a small elliptical galaxy at redshift 3.8 billion light years away. This event has been accepted as a tidal disruption event (TDE), where a star wanders too close to a supermassive black hole, shredding the star. In the case of Swift J1644+57, an astrophysical jet traveling at near the speed of light was launched, and lasted roughly 1.5 years before turning off.

Since 2011, only 4 jetted TDEs have been discovered, of which 3 were detected in gamma-rays (including Swift J1644+57). It is estimated that just 1% of all TDEs are jetted events.

Emission mechanisms

The means by which gamma-ray bursts convert energy into radiation remains poorly understood, and as of 2010 there was still no generally accepted model for how this process occurs. Any successful model of GRB emission must explain the physical process for generating gamma-ray emission that matches the observed diversity of light curves, spectra, and other characteristics. Particularly challenging is the need to explain the very high efficiencies that are inferred from some explosions: some gamma-ray bursts may convert as much as half (or more) of the explosion energy into gamma-rays. Early observations of the bright optical counterparts to GRB 990123 and to GRB 080319B, whose optical light curves were extrapolations of the gamma-ray light spectra, have suggested that inverse Compton scattering may be the dominant process in some events. In this model, pre-existing low-energy photons are scattered by relativistic electrons within the explosion, augmenting their energy by a large factor and transforming them into gamma-rays.

The nature of the longer-wavelength afterglow emission (ranging from X-ray through radio) that follows gamma-ray bursts is better understood. Any energy released by the explosion not radiated away in the burst itself takes the form of matter or energy moving outward at nearly the speed of light. As this matter collides with the surrounding interstellar gas, it creates a relativistic shock wave that then propagates forward into interstellar space. A second shock wave, the reverse shock, may propagate back into the ejected matter. Extremely energetic electrons within the shock wave are accelerated by strong local magnetic fields and radiate as synchrotron emission across most of the electromagnetic spectrum. This model has generally been successful in modeling the behavior of many observed afterglows at late times (generally, hours to days after the explosion), although there are difficulties explaining all features of the afterglow very shortly after the gamma-ray burst has occurred.

Rate of occurrence and potential effects on life

Gamma ray bursts can have harmful or destructive effects on life. Considering the universe as a whole, the safest environments for life similar to that on Earth are the lowest density regions in the outskirts of large galaxies. Our knowledge of galaxy types and their distribution suggests that life as we know it can only exist in about 10% of all galaxies. Furthermore, galaxies with a redshift, z, higher than 0.5 are unsuitable for life as we know it, because of their higher rate of GRBs and their stellar compactness.

All GRBs observed to date have occurred well outside the Milky Way galaxy and have been harmless to Earth. However, if a GRB were to occur within the Milky Way within 5,000 to 8,000 light-years and its emission were beamed straight towards Earth, the effects could be harmful and potentially devastating for its ecosystems. Currently, orbiting satellites detect on average approximately one GRB per day. The closest observed GRB as of March 2014 was GRB 980425, located 40 megaparsecs (130,000,000 ly) away (z=0.0085) in an SBc-type dwarf galaxy. GRB 980425 was far less energetic than the average GRB and was associated with the Type Ib supernova SN 1998bw.

Estimating the exact rate at which GRBs occur is difficult; for a galaxy of approximately the same size as the Milky Way, estimates of the expected rate (for long-duration GRBs) can range from one burst every 10,000 years, to one burst every 1,000,000 years. Only a small percentage of these would be beamed towards Earth. Estimates of rate of occurrence of short-duration GRBs are even more uncertain because of the unknown degree of collimation, but are probably comparable.

Since GRBs are thought to involve beamed emission along two jets in opposing directions, only planets in the path of these jets would be subjected to the high energy gamma radiation. A GRB could potentially vaporize anything in its beams' paths within a range of around 200 light-years.

Although nearby GRBs hitting Earth with a destructive shower of gamma rays are only hypothetical events, high energy processes across the galaxy have been observed to affect the Earth's atmosphere.

Effects on Earth

Earth's atmosphere is very effective at absorbing high energy electromagnetic radiation such as x-rays and gamma rays, so these types of radiation would not reach any dangerous levels at the surface during the burst event itself. The immediate effect on life on Earth from a GRB within a few kiloparsecs would only be a short increase in ultraviolet radiation at ground level, lasting from less than a second to tens of seconds. This ultraviolet radiation could potentially reach dangerous levels depending on the exact nature and distance of the burst, but it seems unlikely to be able to cause a global catastrophe for life on Earth.

The long-term effects from a nearby burst are more dangerous. Gamma rays cause chemical reactions in the atmosphere involving oxygen and nitrogen molecules, creating first nitrogen oxide then nitrogen dioxide gas. The nitrogen oxides cause dangerous effects on three levels. First, they deplete ozone, with models showing a possible global reduction of 25–35%, with as much as 75% in certain locations, an effect that would last for years. This reduction is enough to cause a dangerously elevated UV index at the surface. Secondly, the nitrogen oxides cause photochemical smog, which darkens the sky and blocks out parts of the sunlight spectrum. This would affect photosynthesis, but models show only about a 1% reduction of the total sunlight spectrum, lasting a few years. However, the smog could potentially cause a cooling effect on Earth's climate, producing a "cosmic winter" (similar to an impact winter, but without an impact), but only if it occurs simultaneously with a global climate instability. Thirdly, the elevated nitrogen dioxide levels in the atmosphere would wash out and produce acid rain. Nitric acid is toxic to a variety of organisms, including amphibian life, but models predict that it would not reach levels that would cause a serious global effect. The nitrates might in fact be of benefit to some plants.

All in all, a GRB within a few kiloparsecs, with its energy directed towards Earth, will mostly damage life by raising the UV levels during the burst itself and for a few years thereafter. Models show that the destructive effects of this increase can cause up to 16 times the normal levels of DNA damage. It has proved difficult to assess a reliable evaluation of the consequences of this on the terrestrial ecosystem, because of the uncertainty in biological field and laboratory data.

Hypothetical effects on Earth in the past

There is a very good chance (but no certainty) that at least one lethal GRB took place during the past 5 billion years close enough to Earth as to significantly damage life. There is a 50% chance that such a lethal GRB took place within two kiloparsecs of Earth during the last 500 million years, causing one of the major mass extinction events.

The major Ordovician–Silurian extinction event 450 million years ago may have been caused by a GRB. Estimates suggest that approximately 20–60% of the total phytoplankton biomass in the Ordovician oceans would have perished in a GRB, because the oceans were mostly oligotrophic and clear. The late Ordovician species of trilobites that spent portions of their lives in the plankton layer near the ocean surface were much harder hit than deep-water dwellers, which tended to remain within quite restricted areas. This is in contrast to the usual pattern of extinction events, wherein species with more widely spread populations typically fare better. A possible explanation is that trilobites remaining in deep water would be more shielded from the increased UV radiation associated with a GRB. Also supportive of this hypothesis is the fact that during the late Ordovician, burrowing bivalve species were less likely to go extinct than bivalves that lived on the surface.

A case has been made that the 774–775 carbon-14 spike was the result of a short GRB, though a very strong solar flare is another possibility.

GRB candidates in the Milky Way

No gamma-ray bursts from within our own galaxy, the Milky Way, have been observed, and the question of whether one has ever occurred remains unresolved. In light of evolving understanding of gamma-ray bursts and their progenitors, the scientific literature records a growing number of local, past, and future GRB candidates. Long duration GRBs are related to superluminous supernovae, or hypernovae, and most luminous blue variables (LBVs) and rapidly spinning Wolf–Rayet stars are thought to end their life cycles in core-collapse supernovae with an associated long-duration GRB. Knowledge of GRBs, however, is from metal-poor galaxies of former epochs of the universe's evolution, and it is impossible to directly extrapolate to encompass more evolved galaxies and stellar environments with a higher metallicity, such as the Milky Way.

See also

• BOOTES – Network of robotic astronomical observatories
• Fast blue optical transient
• Fast radio burst
• Gamma-ray burst precursor
• Gamma-ray Search for Extraterrestrial Intelligence
• Horizons: Exploring the Universe
• List of gamma-ray bursts
  • GRB 020813, GRB 031203, GRB 070714B
  • GRB 080916C, GRB 100621A, GRB 130427A
  • GRB 190114C, GRB 221009A
• Relativistic jet – Beam of ionized matter flowing along the axis of a rotating astronomical objectPages displaying short descriptions of redirect targets
• Soft gamma repeater – Astronomical object which emits bursts of gamma or x-rays at irregular intervals
• Stellar evolution
• Terrestrial gamma-ray flashes

Notes

1. A notable exception is the 5 March event of 1979, an extremely bright burst that was successfully localized to supernova remnant N49 in the Large Magellanic Cloud. This event is now interpreted as a magnetar giant flare, more related to SGR flares than "true" gamma-ray bursts.
2. GRBs are named after the date on which they are discovered: the first two digits being the year, followed by the two-digit month and two-digit day and a letter with the order they were detected during that day. The letter 'A' is appended to the name for the first burst identified, 'B' for the second, and so on. For bursts before the year 2010, this letter was only appended if more than one burst occurred that day.
3. The duration of a burst is typically measured by T90, the duration of the period which 90 percent of the burst's energy is emitted. Recently some otherwise "short" GRBs have been shown to be followed by a second, much longer emission episode that when included in the burst light curve results in T90 durations of up to several minutes: these events are only short in the literal sense when this component is excluded.

Citations

1. Reddy, Francis (2023-03-28). "NASA Missions Study What May Be a 1-In-10,000-Year Gamma-ray Burst - NASA". nasa.gov. Retrieved 2023-09-29.
2. Gehrels, Neil; Mészáros, Péter (2012-08-24). "Gamma-Ray Bursts". Science. 337 (6097): 932–936. arXiv:1208.6522. Bibcode:2012Sci...337..932G. doi:10.1126/science.1216793. ISSN 0036-8075. PMID 22923573.
3. Misra, Kuntal; Ghosh, Ankur; Resmi, L. (2023). "The Detection of Very High Energy Photons in Gamma Ray Bursts" (PDF). Physics News. 53. Tata Institute of Fundamental Research: 42–45.
4. NASA Universe Web Team (2023-06-09). "Gamma-Ray Bursts: Black Hole Birth Announcements". science.nasa.gov. Retrieved 2024-05-18.
5. "Gamma Rays". NASA. Archived from the original on 2012-05-02.
6. Zhang, Bing (2018). The Physics of Gamma-Ray Bursts. Cambridge University Press. pp. xv, 2. ISBN 978-1-107-02761-9.
7. Atkinson, Nancy (2013-04-16). "New Kind of Gamma Ray Burst is Ultra Long-Lasting". Universe Today. Retrieved 2022-01-03.
8. ^ Kouveliotou 1994
9. Vedrenne & Atteia 2009
10. ^ Abbott, B. P.; et al. (LIGO Scientific Collaboration & Virgo Collaboration) (16 October 2017). "GW170817: Observation of Gravitational Waves from a Binary Neutron Star Inspiral". Physical Review Letters. 119 (16): 161101. arXiv:1710.05832. Bibcode:2017PhRvL.119p1101A. doi:10.1103/PhysRevLett.119.161101. PMID 29099225. S2CID 217163611.
11. Arizona State University (26 July 2017). "Massive star's dying blast caught by rapid-response telescopes". PhysOrg. Retrieved 27 July 2017.
12. Podsiadlowski 2004
13. ^ Melott 2004
14. ^ Melott, A.L. & Thomas, B.C. (2009). "Late Ordovician geographic patterns of extinction compared with simulations of astrophysical ionizing radiation damage". Paleobiology. 35 (3): 311–320. arXiv:0809.0899. Bibcode:2009Pbio...35..311M. doi:10.1666/0094-8373-35.3.311. S2CID 11942132.
15. ^ Rodríguez-López, Lien; Cardenas, Rolando; González-Rodríguez, Lisdelys; Guimarais, Mayrene; Horvath, Jorge (24 January 2021). "Influence of a galactic gamma ray burst on ocean plankton". Astronomical Notes. 342 (1–2): 45–48. arXiv:2011.08433. Bibcode:2021AN....342...45R. doi:10.1002/asna.202113878. S2CID 226975864. Retrieved 21 October 2022.
16. ^ Thomas, Brian C.; Jackman, Charles H.; Melott, Adrian L.; Laird, Claude M.; Stolarski, Richard S.; Gehrels, Neil; Cannizzo, John K.; Hogan, Daniel P. (28 February 2005). "Terrestrial Ozone Depletion due to a Milky Way Gamma-Ray Burst". The Astrophysical Journal. 622 (2): L153 – L156. arXiv:astro-ph/0411284. Bibcode:2005ApJ...622L.153T. doi:10.1086/429799. hdl:2060/20050179464. S2CID 11199820. Retrieved 22 October 2022.
17. ^ Bonnell, J. T.; Klebesadel, R. W. (1996). "A brief history of the discovery of cosmic gamma-ray bursts". AIP Conference Proceedings. 384: 979. Bibcode:1996AIPC..384..977B. doi:10.1063/1.51630.
18. ^ Klebesadel R.W.; Strong I.B.; Olson R.A. (1973). "Observations of Gamma-Ray Bursts of Cosmic Origin". Astrophysical Journal Letters. 182: L85. Bibcode:1973ApJ...182L..85K. doi:10.1086/181225.
19. Hurley 2003
20. Bonnell, JT; Klebesadel, RW (1996). "A brief history of the discovery of cosmic gamma-ray bursts". AIP Conference Proceedings. 384 (1): 977–980. Bibcode:1996AIPC..384..977B. doi:10.1063/1.51630.
21. ^ Schilling 2002, pp. 12–16
22. Klebesadel, R. W.; et, al (1973). "Observations of Gamma-Ray Bursts of Cosmic Origin". Astrophysical Journal. 182: 85. Bibcode:1973ApJ...182L..85K. doi:10.1086/181225.
23. Meegan 1992
24. ^ Vedrenne & Atteia 2009, pp. 16–40
25. Schilling 2002, pp. 36–37
26. Paczyński 1999, p. 6
27. Piran 1992
28. Lamb 1995
29. Hurley 1986, p. 33
30. Pedersen 1987
31. Hurley 1992
32. ^ Fishman & Meegan 1995
33. Paczynski 1993
34. van Paradijs 1997
35. ^ Vedrenne & Atteia 2009, pp. 90–93
36. Schilling 2002, p. 102
37. Reichart 1995
38. Schilling 2002, pp. 118–123
39. ^ Galama 1998
40. Ricker 2003
41. McCray 2008
42. Gehrels 2004
43. Akerlof 2003
44. Akerlof 1999
45. "Lobster-inspired £3.8m super lightweight mirror chosen for Chinese-French space mission". University of Leicester. 26 October 2015. Archived from the original on 28 Jan 2021. Retrieved 20 May 2021.
46. Chang, Hsiang-Kuang; Lin, Chi-Hsun; Tsao, Che-Chih; Chu, Che-Yen; Yang, Shun-Chia; Huang, Chien-You; Wang, Chao-Hsi; Su, Tze-Hsiang; Chung, Yun-Hsin; Chang, Yung-Wei; Gong, Zi-Jun; Hsiang, Jr-Yue; Lai, Keng-Li; Lin, Tsu-Hsuan; Lu, Chia-Yu (2022-01-15). "The Gamma-ray Transients Monitor (GTM) on board Formosat-8B and its GRB detection efficiency". Advances in Space Research. 69 (2): 1249–1255. Bibcode:2022AdSpR..69.1249C. doi:10.1016/j.asr.2021.10.044. ISSN 0273-1177.
47. ^ Bloom 2009
48. Reddy 2009
49. University of Maryland (16 October 2018). "All in the family: Kin of gravitational wave source discovered – New observations suggest that kilonovae – immense cosmic explosions that produce silver, gold and platinum – may be more common than thought". EurekAlert! (Press release). Archived from the original on 16 October 2018. Retrieved 17 October 2018.
50. Troja, E.; et al. (16 October 2018). "A luminous blue kilonova and an off-axis jet from a compact binary merger at z = 0.1341". Nature Communications. 9 (4089 (2018)): 4089. arXiv:1806.10624. Bibcode:2018NatCo...9.4089T. doi:10.1038/s41467-018-06558-7. PMC 6191439. PMID 30327476.
51. Mohon, Lee (16 October 2018). "GRB 150101B: A Distant Cousin to GW170817". NASA. Retrieved 17 October 2018.
52. Wall, Mike (17 October 2018). "Powerful Cosmic Flash Is Likely Another Neutron-Star Merger". Space.com. Retrieved 17 October 2018.
53. Veres, P; et al. (20 November 2019). "Observation of inverse Compton emission from a long γ-ray burst". Nature. 575 (7783): 459–463. arXiv:2006.07251. Bibcode:2019Natur.575..459M. doi:10.1038/s41586-019-1754-6. PMID 31748725. S2CID 208191199.
54. Conover, Emily (2021-05-21). "Record-breaking light has more than a quadrillion electron volts of energy". Science News. Retrieved 2022-05-11.
55. Katz 2002, p. 37
56. Marani 1997
57. Lazatti 2005
58. Simić 2005
59. Horvath 1998
60. Hakkila 2003
61. Chattopadhyay 2007
62. Virgili 2009
63. "Hubble captures infrared glow of a kilonova blast". Image Gallery. ESA/Hubble. 5 August 2013. Retrieved 14 August 2013.
64. Laskar, Tanmoy; Escorial, Alicia Rouco; Schroeder, Genevieve; Fong, Wen-fai; Berger, Edo; Veres, Péter; Bhandari, Shivani; Rastinejad, Jillian; Kilpatrick, Charles D.; Tohuvavohu, Aaron; Margutti, Raffaella; Alexander, Kate D.; DeLaunay, James; Kennea, Jamie A.; Nugent, Anya (2022-08-01). "The First Short GRB Millimeter Afterglow: The Wide-angled Jet of the Extremely Energetic SGRB 211106A". The Astrophysical Journal Letters. 935 (1): L11. arXiv:2205.03419. Bibcode:2022ApJ...935L..11L. doi:10.3847/2041-8213/ac8421. S2CID 248572470.
65. "Out With a Bang: Explosive Neutron Star Merger Captured for the First Time in Millimeter Light". National Radio Astronomy Observatory. Retrieved 2022-08-14.
66. "Explosive neutron star merger captured for first time in millimeter light". news.northwestern.edu. Retrieved 2022-08-14.
67. ^ In a Flash NASA Helps Solve 35-year-old Cosmic Mystery. NASA (2005-10-05) The 30% figure is given here, as well as afterglow discussion.
68. Bloom 2006
69. Hjorth 2005
70. Gehrels 2005
71. ^ Woosley & Bloom 2006
72. Li, Li-Xin; Paczyński, Bohdan (1998-09-21). "Transient Events from Neutron Star Mergers". The Astrophysical Journal. 507 (1): L59. arXiv:astro-ph/9807272. Bibcode:1998ApJ...507L..59L. doi:10.1086/311680. ISSN 0004-637X. S2CID 3091361.
73. Tanvir, N. R.; Levan, A. J.; Fruchter, A. S.; Hjorth, J.; Hounsell, R. A.; Wiersema, K.; Tunnicliffe, R. L. (2013). "A 'kilonova' associated with the short-duration γ-ray burst GRB 130603B". Nature. 500 (7464): 547–549. arXiv:1306.4971. Bibcode:2013Natur.500..547T. doi:10.1038/nature12505. PMID 23912055. S2CID 205235329.
74. Gugliucci, Nicole (7 August 2013). "Kilonova Alert! Hubble Solves Gamma Ray Burst Mystery". Discovery News. Archived from the original on 3 March 2016. Retrieved 22 January 2015.
75. Frederiks 2008
76. Hurley 2005
77. Hjorth, Jens; Sollerman, Jesper; Møller, Palle; Fynbo, Johan P. U.; Woosley, Stan E.; Kouveliotou, Chryssa; Tanvir, Nial R.; Greiner, Jochen; Andersen, Michael I.; Castro-Tirado, Alberto J.; Castro Cerón, José María; Fruchter, Andrew S.; Gorosabel, Javier; Jakobsson, Páll; Kaper, Lex (2003-06-19). "A very energetic supernova associated with the γ-ray burst of 29 March 2003". Nature. 423 (6942): 847–850. arXiv:astro-ph/0306347. Bibcode:2003Natur.423..847H. doi:10.1038/nature01750. ISSN 0028-0836. PMID 12815425.
78. Pontzen et al. 2010
79. Rastinejad, Jillian C.; Gompertz, Benjamin P.; Levan, Andrew J.; Fong, Wen-fai; Nicholl, Matt; Lamb, Gavin P.; Malesani, Daniele B.; Nugent, Anya E.; Oates, Samantha R.; Tanvir, Nial R.; de Ugarte Postigo, Antonio; Kilpatrick, Charles D.; Moore, Christopher J.; Metzger, Brian D.; Ravasio, Maria Edvige (2022-12-08). "A kilonova following a long-duration gamma-ray burst at 350 Mpc". Nature. 612 (7939): 223–227. arXiv:2204.10864. Bibcode:2022Natur.612..223R. doi:10.1038/s41586-022-05390-w. ISSN 0028-0836. PMID 36477128.
80. Troja, E.; Fryer, C. L.; O’Connor, B.; Ryan, G.; Dichiara, S.; Kumar, A.; Ito, N.; Gupta, R.; Wollaeger, R. T.; Norris, J. P.; Kawai, N.; Butler, N. R.; Aryan, A.; Misra, K.; Hosokawa, R. (2022-12-08). "A nearby long gamma-ray burst from a merger of compact objects". Nature. 612 (7939): 228–231. arXiv:2209.03363. Bibcode:2022Natur.612..228T. doi:10.1038/s41586-022-05327-3. ISSN 0028-0836. PMC 9729102. PMID 36477127.
81. "Kilonova Discovery Challenges our Understanding of Gamma-Ray Bursts". Gemini Observatory. 2022-12-07. Retrieved 2022-12-11.
82. Levan, Andrew J.; Malesani, Daniele B.; Gompertz, Benjamin P.; Nugent, Anya E.; Nicholl, Matt; Oates, Samantha R.; Perley, Daniel A.; Rastinejad, Jillian; Metzger, Brian D.; Schulze, Steve; Stanway, Elizabeth R.; Inkenhaag, Anne; Zafar, Tayyaba; Agüí Fernández, J. Feliciano; Chrimes, Ashley A. (2023-06-22). "A long-duration gamma-ray burst of dynamical origin from the nucleus of an ancient galaxy". Nature Astronomy. 7 (8): 976–985. arXiv:2303.12912. Bibcode:2023NatAs...7..976L. doi:10.1038/s41550-023-01998-8. ISSN 2397-3366.
83. "GCN - Circulars - 33410: Solar Orbiter STIX observation of GRB 230307A".
84. "GCN - Circulars - 33412: GRB 230307A: AGILE/MCAL detection".
85. Wodd, Charlie (11 December 2023). "Extra-Long Blasts Challenge Our Theories of Cosmic Cataclysms". Quanta magazine.
86. Gendre, B.; Stratta, G.; Atteia, J. L.; Basa, S.; Boër, M.; Coward, D. M.; Cutini, S.; d'Elia, V.; Howell, E. J; Klotz, A.; Piro, L. (2013). "The Ultra-Long Gamma-Ray Burst 111209A: The Collapse of a Blue Supergiant?". The Astrophysical Journal. 766 (1): 30. arXiv:1212.2392. Bibcode:2013ApJ...766...30G. doi:10.1088/0004-637X/766/1/30. S2CID 118618287.
87. ^ Greiner, Jochen; Mazzali, Paolo A.; Kann, D. Alexander; Krühler, Thomas; Pian, Elena; Prentice, Simon; Olivares E., Felipe; Rossi, Andrea; Klose, Sylvio; Taubenberger, Stefan; Knust, Fabian; Afonso, Paulo M. J.; Ashall, Chris; Bolmer, Jan; Delvaux, Corentin; Diehl, Roland; Elliott, Jonathan; Filgas, Robert; Fynbo, Johan P. U.; Graham, John F.; Guelbenzu, Ana Nicuesa; Kobayashi, Shiho; Leloudas, Giorgos; Savaglio, Sandra; Schady, Patricia; Schmidl, Sebastian; Schweyer, Tassilo; Sudilovsky, Vladimir; Tanga, Mohit; et al. (2015-07-08). "A very luminous magnetar-powered supernova associated with an ultra-long γ-ray burst". Nature. 523 (7559): 189–192. arXiv:1509.03279. Bibcode:2015Natur.523..189G. doi:10.1038/nature14579. PMID 26156372. S2CID 4464998.
88. ^ Levan, A. J.; Tanvir, N. R.; Starling, R. L. C.; Wiersema, K.; Page, K. L.; Perley, D. A.; Schulze, S.; Wynn, G. A.; Chornock, R.; Hjorth, J.; Cenko, S. B.; Fruchter, A. S.; O'Brien, P. T.; Brown, G. C.; Tunnicliffe, R. L.; Malesani, D.; Jakobsson, P.; Watson, D.; Berger, E.; Bersier, D.; Cobb, B. E.; Covino, S.; Cucchiara, A.; de Ugarte Postigo, A.; Fox, D. B.; Gal-Yam, A.; Goldoni, P.; Gorosabel, J.; Kaper, L.; et al. (2014). "A new population of ultra-long duration gamma-ray bursts". The Astrophysical Journal. 781 (1): 13. arXiv:1302.2352. Bibcode:2014ApJ...781...13L. doi:10.1088/0004-637x/781/1/13. S2CID 24657235.
89. Ioka, Kunihito; Hotokezaka, Kenta; Piran, Tsvi (2016-12-12). "Are Ultra-Long Gamma-Ray Bursts Caused by Blue Supergiant Collapsars, Newborn Magnetars, or White Dwarf Tidal Disruption Events?". The Astrophysical Journal. 833 (1): 110. arXiv:1608.02938. Bibcode:2016ApJ...833..110I. doi:10.3847/1538-4357/833/1/110. S2CID 118629696.
90. Boer, Michel; Gendre, Bruce; Stratta, Giulia (2013). "Are Ultra-long Gamma-Ray Bursts different?". The Astrophysical Journal. 800 (1): 16. arXiv:1310.4944. Bibcode:2015ApJ...800...16B. doi:10.1088/0004-637X/800/1/16. S2CID 118655406.
91. Virgili, F. J.; Mundell, C. G.; Pal'Shin, V.; Guidorzi, C.; Margutti, R.; Melandri, A.; Harrison, R.; Kobayashi, S.; Chornock, R.; Henden, A.; Updike, A. C.; Cenko, S. B.; Tanvir, N. R.; Steele, I. A.; Cucchiara, A.; Gomboc, A.; Levan, A.; Cano, Z.; Mottram, C. J.; Clay, N. R.; Bersier, D.; Kopač, D.; Japelj, J.; Filippenko, A. V.; Li, W.; Svinkin, D.; Golenetskii, S.; Hartmann, D. H.; Milne, P. A.; et al. (2013). "Grb 091024A and the Nature of Ultra-Long Gamma-Ray Bursts". The Astrophysical Journal. 778 (1): 54. arXiv:1310.0313. Bibcode:2013ApJ...778...54V. doi:10.1088/0004-637X/778/1/54. S2CID 119023750.
92. Zhang, Bin-Bin; Zhang, Bing; Murase, Kohta; Connaughton, Valerie; Briggs, Michael S. (2014). "How Long does a Burst Burst?". The Astrophysical Journal. 787 (1): 66. arXiv:1310.2540. Bibcode:2014ApJ...787...66Z. doi:10.1088/0004-637X/787/1/66. S2CID 56273013.
93. ^ Racusin 2008
94. Rykoff 2009
95. Abdo 2009
96. Dereli-Bégué, Hüsne; Pe’er, Asaf; Ryde, Felix; Oates, Samantha R.; Zhang, Bing; Dainotti, Maria G. (2022-09-24). "A wind environment and Lorentz factors of tens explain gamma-ray bursts X-ray plateau". Nature Communications. 13 (1): 5611. arXiv:2207.11066. Bibcode:2022NatCo..13.5611D. doi:10.1038/s41467-022-32881-1. ISSN 2041-1723. PMC 9509382. PMID 36153328.
97. Pe’er, Asaf (2019). "Plasmas in Gamma-Ray Bursts: Particle Acceleration, Magnetic Fields, Radiative Processes and Environments". Galaxies. 7 (1): 33. arXiv:1902.02562. Bibcode:2019Galax...7...33P. doi:10.3390/galaxies7010033. ISSN 2075-4434.
98. Hakkila, Jon; Nemiroff, Robert (2019-09-23). "Time-reversed Gamma-Ray Burst Light-curve Characteristics as Transitions between Subluminal and Superluminal Motion". The Astrophysical Journal. 883 (1): 70. arXiv:1908.07306. Bibcode:2019ApJ...883...70H. doi:10.3847/1538-4357/ab3bdf. ISSN 0004-637X.
99. Ratner, Paul (2019-09-25). "Astrophysicists: Gamma-ray jets exceed the speed of light". Big Think. Retrieved 2023-10-11.
100. Siegel, Ethan (2019-10-05). "Ask Ethan: Can Gamma-Ray Jets Really Travel Faster Than The Speed Of Light?". Forbes. Retrieved 2023-10-11.
101. Sari 1999
102. Burrows 2006
103. ^ Frail 2001
104. Melia, Fulvio (2009). High-Energy Astrophysics. Princeton University Press. p. 241. ISBN 978-0-691-13543-4.
105. Mazzali 2005
106. Frail 2000
107. ^ Rueda, Jorge A.; Ruffini, Remo; Moradi, Rahim; Wang, Yu (2021). "A brief review of binary-driven hypernova". International Journal of Modern Physics D. 30 (15). arXiv:2201.03500. Bibcode:2021IJMPD..3030007R. doi:10.1142/S021827182130007X. ISSN 0218-2718.
108. Aimuratov, Y.; Becerra, L. M.; Bianco, C. L.; Cherubini, C.; Valle, M. Della; Filippi, S.; Li, Liang; Moradi, R.; Rastegarnia, F.; Rueda, J. A.; Ruffini, R.; Sahakyan, N.; Wang, Y.; Zhang, S. R. (2023). "GRB-SN Association within the Binary-driven Hypernova Model". The Astrophysical Journal. 955 (2): 93. arXiv:2303.16902. Bibcode:2023ApJ...955...93A. doi:10.3847/1538-4357/ace721. ISSN 0004-637X.
109. ^ Rueda, J. A.; Ruffini, R.; Wang, Y. (2019-05-09). "Induced Gravitational Collapse, Binary-Driven Hypernovae, Long Gramma-ray Bursts and Their Connection with Short Gamma-ray Bursts". Universe. 5 (5): 110. arXiv:1905.06050. Bibcode:2019Univ....5..110R. doi:10.3390/universe5050110. ISSN 2218-1997.
110. Billings, Lee (2019-11-20). "Record-Breaking Gamma Rays Reveal Secrets of the Universe's Most Powerful Explosions". Scientific American. Retrieved 2023-09-17.
111. Choi, Charles Q. (2019-11-20). "The Most Powerful Explosions in the Universe Emit Way More Energy Than Anyone Thought". Space.com. Retrieved 2023-09-17.
112. ^ Prochaska 2006
113. Watson 2006
114. Grupe 2006
115. MacFadyen 1999
116. Zhang, Bing; Mészáros, Peter (2001-05-01). "Gamma-Ray Burst Afterglow with Continuous Energy Injection: Signature of a Highly Magnetized Millisecond Pulsar". The Astrophysical Journal Letters. 552 (1): L35 – L38. arXiv:astro-ph/0011133. Bibcode:2001ApJ...552L..35Z. doi:10.1086/320255. S2CID 18660804.
117. Troja, E.; Cusumano, G.; O'Brien, P. T.; Zhang, B.; Sbarufatti, B.; Mangano, V.; Willingale, R.; Chincarini, G.; Osborne, J. P. (2007-08-01). "Swift Observations of GRB 070110: An Extraordinary X-Ray Afterglow Powered by the Central Engine". The Astrophysical Journal. 665 (1): 599–607. arXiv:astro-ph/0702220. Bibcode:2007ApJ...665..599T. doi:10.1086/519450. S2CID 14317593.
118. Ruffini, R.; Muccino, M.; Bianco, C. L.; Enderli, M.; Izzo, L.; Kovacevic, M.; Penacchioni, A. V.; Pisani, G. B.; Rueda, J. A.; Wang, Y. (2014-05-01). "On binary-driven hypernovae and their nested late X-ray emission". Astronomy & Astrophysics. 565: L10. arXiv:1404.3946. Bibcode:2014A&A...565L..10R. doi:10.1051/0004-6361/201423812. ISSN 0004-6361.
119. Fryer, Chris L.; Rueda, Jorge A.; Ruffini, Remo (2014-09-16). "Hypercritical Accretion, Induced Gravitational Collapse, and Binary-Driven Hypernovae". The Astrophysical Journal. 793 (2): L36. arXiv:1409.1473. Bibcode:2014ApJ...793L..36F. doi:10.1088/2041-8205/793/2/l36. ISSN 2041-8213.
120. "Binary-driven hypernova model gains observational support". phys.org. 2020-05-19. Retrieved 2024-05-22.
121. Plait 2008
122. Stanek 2006
123. Abbott 2007
124. Kochanek 1993
125. Vietri 1998
126. MacFadyen 2006
127. Blinnikov 1984
128. Cline 1996
129. Winterberg, Friedwardt (2001 Aug 29). "Gamma-Ray Bursters and Lorentzian Relativity". Z. Naturforsch 56a: 889–892.
130. Cendes, Yvette (8 December 2021). "How do black holes swallow stars?". Astronomy Magazine. Retrieved 8 May 2024.
131. ^ Hensley, Kerry (8 November 2023). "Why Are Jets from Disrupted Stars So Rare?". AAS Nova.
132. Stern 2007
133. Fishman, G. 1995
134. Fan & Piran 2006
135. Liang, E. P.; Crider, A.; Boettcher, M.; Smith, I. A. (1999-03-29). "GRB990123: The Case for Saturated Comptonization". The Astrophysical Journal. 519 (1): L21 – L24. arXiv:astro-ph/9903438. Bibcode:1999ApJ...519L..21L. doi:10.1086/312100. S2CID 16005521.
136. Wozniak 2009
137. Meszaros 1997
138. Sari 1998
139. Nousek 2006
140. "ESO Telescopes Observe Swift Satellite's 1000th Gamma-ray Burst". 6 November 2015. Retrieved 9 November 2015.
141. Piran, Tsvi; Jimenez, Raul (5 December 2014). "Possible Role of Gamma Ray Bursts on Life Extinction in the Universe". Physical Review Letters. 113 (23): 231102. arXiv:1409.2506. Bibcode:2014PhRvL.113w1102P. doi:10.1103/PhysRevLett.113.231102. PMID 25526110. S2CID 43491624.
142. Schirber, Michael (2014-12-08). "Focus: Gamma-Ray Bursts Determine Potential Locations for Life". Physics. 7: 124. doi:10.1103/Physics.7.124.
143. Cain, Fraser (January 12, 2015). "Are Gamma Ray Bursts Dangerous?".
144. Soderberg, A. M.; Kulkarni, S. R.; Berger, E.; Fox, D. W.; Sako, M.; Frail, D. A.; Gal-Yam, A.; Moon, D. S.; Cenko, S. B.; Yost, S. A.; Phillips, M. M.; Persson, S. E.; Freedman, W. L.; Wyatt, P.; Jayawardhana, R.; Paulson, D. (2004). "The sub-energetic γ-ray burst GRB 031203 as a cosmic analogue to the nearby GRB 980425". Nature. 430 (7000): 648–650. arXiv:astro-ph/0408096. Bibcode:2004Natur.430..648S. doi:10.1038/nature02757. hdl:2027.42/62961. PMID 15295592. S2CID 4363027.
145. Le Floc'h, E.; Charmandaris, V.; Gordon, K.; Forrest, W. J.; Brandl, B.; Schaerer, D.; Dessauges-Zavadsky, M.; Armus, L. (2011). "The first Infrared study of the close environment of a long Gamma-Ray Burst". The Astrophysical Journal. 746 (1): 7. arXiv:1111.1234. Bibcode:2012ApJ...746....7L. doi:10.1088/0004-637X/746/1/7. S2CID 51474244.
146. Kippen, R.M.; Briggs, M. S.; Kommers, J. M.; Kouveliotou, C.; Hurley, K.; Robinson, C. R.; Van Paradijs, J.; Hartmann, D. H.; Galama, T. J.; Vreeswijk, P. M. (October 1998). "On the Association of Gamma-Ray Bursts with Supernovae". The Astrophysical Journal. 506 (1): L27 – L30. arXiv:astro-ph/9806364. Bibcode:1998ApJ...506L..27K. doi:10.1086/311634. S2CID 2677824.
147. Morelle, Rebecca (2013-01-21). "Gamma-ray burst 'hit Earth in 8th Century'". BBC News. Retrieved January 21, 2013.
148. Guetta and Piran 2006
149. Welsh, Jennifer (2011-07-10). "Can gamma-ray bursts destroy life on Earth?". MSN. Archived from the original on November 22, 2013. Retrieved October 27, 2011.
150. "Gamma-ray bursts: are we safe?". www.esa.int. 2003-09-17. Retrieved 2023-09-17.
151. Lincoln, Don (2023-06-06). "Scientists are exploring how deadly gamma-ray bursts could sterilize — or vaporize — the Earth". Big Think. Retrieved 2023-09-17.
152. "Cosmic energy burst disturbs Earth's atmosphere". NASA Science. September 29, 1998. Archived from the original on January 24, 2023. Retrieved July 12, 2017.
153. ^ Thomas, B.C. (2009). "Gamma-ray bursts as a threat to life on Earth". International Journal of Astrobiology. 8 (3): 183–186. arXiv:0903.4710. Bibcode:2009IJAsB...8..183T. doi:10.1017/S1473550409004509. S2CID 118579150.
154. ^ Martin, Osmel; Cardenas, Rolando; Guimarais, Mayrene; Peñate, Liuba; Horvath, Jorge; Galante, Douglas (2010). "Effects of gamma ray bursts in Earth's biosphere". Astrophysics and Space Science. 326 (1): 61–67. arXiv:0911.2196. Bibcode:2010Ap&SS.326...61M. doi:10.1007/s10509-009-0211-7. S2CID 15141366.
155. Piran, Tsvi; Jimenez, Raul (2014-12-05). "Possible Role of Gamma Ray Bursts on Life Extinction in the Universe". Physical Review Letters. 113 (23): 231102. arXiv:1409.2506. Bibcode:2014PhRvL.113w1102P. doi:10.1103/PhysRevLett.113.231102. hdl:2445/133018. PMID 25526110. S2CID 43491624.
156. Thomas, Brian C.; Melott, Adrian Lewis; Jackman, Charles H.; Laird, Claude M.; Medvedev, Mikhail V.; Stolarski, Richard S.; Gehrels, Neil; Cannizzo, John K.; Hogan, Daniel P.; Ejzak, Larissa M. (20 November 2005). "Gamma-Ray Bursts and the Earth: Exploration of Atmospheric, Biological, Climatic, and Biogeochemical Effects". The Astrophysical Journal. 634 (1): 509–533. arXiv:astro-ph/0505472. Bibcode:2005ApJ...634..509T. doi:10.1086/496914. S2CID 2046052. Retrieved 22 October 2022.
157. Pavlov, A.K.; Blinov, A.V.; Konstantinov, A.N.; et al. (2013). "AD 775 pulse of cosmogenic radionuclides production as imprint of a Galactic gamma-ray burst". Mon. Not. R. Astron. Soc. 435 (4): 2878–2884. arXiv:1308.1272. Bibcode:2013MNRAS.435.2878P. doi:10.1093/mnras/stt1468. S2CID 118638711.
158. Hambaryan, V.V.; Neuhauser, R. (2013). "A Galactic short gamma-ray burst as cause for the C peak in AD 774/5". Monthly Notices of the Royal Astronomical Society. 430 (1): 32–36. arXiv:1211.2584. Bibcode:2013MNRAS.430...32H. doi:10.1093/mnras/sts378. S2CID 765056.
159. Mekhaldi; et al. (2015). "Multiradionuclide evidence for the solar origin of the cosmic-ray events of ᴀᴅ 774/5 and 993/4". Nature Communications. 6: 8611. Bibcode:2015NatCo...6.8611M. doi:10.1038/ncomms9611. PMC 4639793. PMID 26497389.
160. "Illustration of a Short Gamma-Ray Burst Caused by a Collapsing Star". July 26, 2021. Retrieved August 3, 2021.
161. Lauren Fuge (20 November 2018). "Milky Way star set to go supernova". Cosmos. Retrieved 7 April 2019.
162. Vink JS (2013). "Gamma-ray burst progenitors and the population of rotating Wolf-Rayet stars". Philos Trans Royal Soc A. 371 (1992): 20120237. Bibcode:2013RSPTA.37120237V. doi:10.1098/rsta.2012.0237. PMID 23630373.
163. Y-H. Chu; C-H. Chen; S-P. Lai (2001). "Superluminous supernova remnants". In Mario Livio; Nino Panagia; Kailash Sahu (eds.). Supernovae and Gamma-Ray Bursts: The Greatest Explosions Since the Big Bang. Cambridge University Press. p. 135. ISBN 978-0-521-79141-0.
164. Van Den Heuvel, E. P. J.; Yoon, S.-C. (2007). "Long gamma-ray burst progenitors: Boundary conditions and binary models". Astrophysics and Space Science. 311 (1–3): 177–183. arXiv:0704.0659. Bibcode:2007Ap&SS.311..177V. doi:10.1007/s10509-007-9583-8. S2CID 38670919.