Editing Gamma-ray burst

{{Short description|Flash of gamma rays from a distant galaxy}}
{{For-multi|bursts of gamma rays of terrestrial origin|terrestrial gamma-ray flash|the constant beam of ionized matter|astrophysical jet}}
[[File:Gamma ray burst.jpg|thumb|300px|Artist's illustration showing the life of a [[star#Massive stars|massive star]]: [[Nuclear fusion]] converts lighter elements into heavier ones; when fusion no longer generates enough pressure to counteract gravity, the star collapses into a [[black hole]]. During this collapse, energy may be released as a momentary burst of gamma-rays aligned to the axis of rotation.]]

In [[gamma-ray astronomy]], '''gamma-ray bursts''' ('''GRBs''') are extremely energetic events occurring in distant [[Galaxy|galaxies]] which represent the brightest and most powerful class of explosion<!-- silent MOS:TYPOFIX "explosions" per MOS:SIC --> in the universe.<ref>{{Cite web |last=Reddy |first=Francis |date=2023-03-28 |title=NASA Missions Study What May Be a 1-In-10,000-Year Gamma-ray Burst - NASA |url=https://www.nasa.gov/universe/nasa-missions-study-what-may-be-a-1-in-10000-year-gamma-ray-burst/ |access-date=2023-09-29 |website=nasa.gov |language=en-US}}</ref><ref>{{Cite journal |last1=Gehrels |first1=Neil |author-link=Neil Gehrels |last2=Mészáros |first2=Péter |author-link2=Péter Mészáros |date=2012-08-24 |title=Gamma-Ray Bursts |url=https://www.science.org/doi/10.1126/science.1216793 |journal=Science |language=en |volume=337 |issue=6097 |pages=932–936 |doi=10.1126/science.1216793 |pmid=22923573 |issn=0036-8075|arxiv=1208.6522 |bibcode=2012Sci...337..932G }}</ref><ref>{{Cite journal |last1=Misra |first1=Kuntal |last2=Ghosh |first2=Ankur |last3=Resmi |first3=L. |date=2023 |title=The Detection of Very High Energy Photons in Gamma Ray Bursts |url=https://www.tifr.res.in/~ipa1970/news/V53-12/Vol53-12-A11.pdf |journal=Physics News |publisher=[[Tata Institute of Fundamental Research]] |volume=53 |pages=42–45}}</ref><ref>{{Cite web |last=NASA Universe Web Team |date=2023-06-09 |title=Gamma-Ray Bursts: Black Hole Birth Announcements |url=https://science.nasa.gov/universe/gamma-ray-bursts-black-hole-birth-announcements/ |access-date=2024-05-18 |website=science.nasa.gov |language=en-US}}</ref> These extreme [[Electromagnetic radiation|electromagnetic]] emissions are second only to the [[Big Bang]] as the most energetic and luminous phenomenon ever known.<ref>{{cite web|title=Gamma Rays|url=http://missionscience.nasa.gov/ems/12_gammarays.html|work=NASA|url-status=dead|archive-url=https://web.archive.org/web/20120502232209/http://missionscience.nasa.gov/ems/12_gammarays.html|archive-date=2012-05-02}}</ref><ref>{{Cite book |last=Zhang |first=Bing |title=The Physics of Gamma-Ray Bursts |publisher=Cambridge University Press |year=2018 |isbn=978-1-107-02761-9 |pages=xv, 2 |language=en}}</ref> Gamma-ray bursts can last from a few milliseconds to several hours.<ref>{{Cite web|last=Atkinson|first=Nancy|date=2013-04-16|title=New Kind of Gamma Ray Burst is Ultra Long-Lasting|url=https://www.universetoday.com/101486/new-kind-of-gamma-ray-burst-is-ultra-long-lasting/|access-date=2022-01-03|website=Universe Today|language=en-US}}</ref><ref name="Kouveliotou" /> After the initial flash of [[gamma ray]]s, a longer-lived afterglow is emitted, usually in the longer wavelengths of [[X-ray]], [[ultraviolet]], [[visible spectrum|optical]], [[infrared]], [[microwave]] or [[radio waves|radio]] frequencies.<ref>[[#VedrenneAtteia|Vedrenne & Atteia 2009]]</ref>

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]]. Short-duration (sGRB) events are a subclass of GRB signals that are now known to originate from the cataclysmic [[Neutron star merger|merger of binary neutron stars]].<ref name="PhysRev" />

The sources of most GRB are billions of [[light year]]s 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)<ref>{{cite web |title=Massive star's dying blast caught by rapid-response telescopes |url=https://phys.org/news/2017-07-massive-star-dying-blast-caught.html |date=26 July 2017 |work=PhysOrg |author=Arizona State University |access-date=27 July 2017 }}</ref> and extremely rare (a few per galaxy per million years).<ref name="rates">[[#Podsiadlowski|Podsiadlowski 2004]]</ref> All GRBs in recorded history have originated from outside the [[Milky Way galaxy]], although a related class of phenomena, [[soft gamma repeater]]s, are associated with [[magnetar]]s within our galaxy. A gamma-ray burst in the Milky Way pointed directly at Earth would likely sterilize the planet or effect a [[mass extinction]].<ref name="Melott2004">[[#Melott|Melott 2004]]</ref> The [[Late Ordovician mass extinction]] has been hypothesised by some researchers to have occurred as a result of such a gamma-ray burst.<ref name="GeographicPatterns">{{cite journal |author1=Melott, A.L. |author2=Thomas, B.C. |name-list-style=amp |title=Late Ordovician geographic patterns of extinction compared with simulations of astrophysical ionizing radiation damage |journal=[[Paleobiology (journal)|Paleobiology]] |year=2009 |volume=35 |issue=3 |pages=311–320 |arxiv=	0809.0899 |doi=10.1666/0094-8373-35.3.311|bibcode=2009Pbio...35..311M |s2cid=11942132 }}</ref><ref name="renamed_from_2021_on_20231204051223"/><ref name="TerrestrialOzoneDepletion" />

GRB signals were first detected in 1967 by the [[Vela (satellite)|Vela satellites]], which were designed to detect [[Partial Nuclear Test Ban Treaty|covert nuclear weapons tests]]; after an "exhaustive" period of analysis,<ref name="BK" />{{rp|979}} this was published as academic research in 1973.<ref name="KSO" /> Following their discovery, hundreds of theoretical models were proposed to explain these bursts, such as collisions between [[comet]]s and [[neutron star]]s.<ref>[[#HurleyBib|Hurley 2003]]</ref> 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 [[redshift]]s using optical [[spectroscopy]], and thus their distances and energy outputs. These discoveries—and subsequent studies of the galaxies and [[supernova]]e associated with the bursts—clarified the distance and [[luminosity]] of GRBs, definitively placing them in distant galaxies.

== History ==
{{Main|History of gamma-ray burst research}}
[[File:BATSE 2704.jpg|thumb|Positions on the sky of all gamma-ray bursts detected during the BATSE mission. The distribution is [[isotropic]], with no concentration towards the plane of the Milky Way, which runs horizontally through the center of the image.]]Gamma-ray bursts were first observed in the late 1960s by the U.S. [[Vela (satellite)|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.<ref>{{cite journal | title = A brief history of the discovery of cosmic gamma-ray bursts | last1 = Bonnell | first1 = JT | last2 = Klebesadel | first2 = RW | date = 1996 | journal = AIP Conference Proceedings | volume = 384 | issue = 1 | pages = 977–980 | doi = 10.1063/1.51630| bibcode = 1996AIPC..384..977B }}</ref> 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.<ref name="FlashVela" /> 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 [[Star position|sky positions]] of 16 bursts<ref name="FlashVela">[[#Schilling|Schilling 2002]], pp. 12–16</ref><ref>{{Cite journal |last1=Klebesadel |first1=R. W. |last2=et |first2=al |date=1973 |title=Observations of Gamma-Ray Bursts of Cosmic Origin |url=https://adsabs.harvard.edu/full/1973ApJ...182L..85K |journal=Astrophysical Journal |volume=182 |pages=85|doi=10.1086/181225 |bibcode=1973ApJ...182L..85K }}</ref> and definitively rule out a terrestrial or solar origin. Contrary to popular belief, the data was never classified.<ref name="BK">{{cite journal |last1=Bonnell |first1=J. T. |last2=Klebesadel |first2=R. W. |title=A brief history of the discovery of cosmic gamma-ray bursts |journal=AIP Conference Proceedings |date=1996 |volume=384 |page=979 |doi=10.1063/1.51630 |bibcode=1996AIPC..384..977B }}</ref> After thorough analysis, the findings were published in 1973 as an ''[[Astrophysical Journal]]'' article entitled "Observations of Gamma-Ray Bursts of Cosmic Origin".<ref name="KSO">{{cite journal|bibcode=1973ApJ...182L..85K |title=Observations of Gamma-Ray Bursts of Cosmic Origin |author1=Klebesadel R.W. |author2=Strong I.B. |author3=Olson R.A. |date=1973 |journal=Astrophysical Journal Letters |volume=182 |page=L85 |doi=10.1086/181225}}</ref>

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 ([[CGRO#Instruments|BATSE]]) instrument, an extremely sensitive gamma-ray detector, provided data that showed the distribution of GRBs is [[Isotropy|isotropic]] (that is, not biased towards any particular direction in space).<ref>[[#Meegan|Meegan 1992]]</ref> 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.<ref name="Vedrenne p. 16–40">[[#VedrenneAtteia|Vedrenne & Atteia 2009]], pp. 16–40</ref><ref>[[#Schilling|Schilling 2002]], pp. 36–37</ref><ref>[[#Pac95|Paczyński 1999]], p. 6</ref><ref name="Piran92">[[#Piran92|Piran 1992]]</ref> However, some Milky Way models are still consistent with an isotropic distribution.<ref name="Vedrenne p. 16–40" /><ref name="Lamb">[[#Lamb|Lamb 1995]]</ref>

=== 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 dwarf]]s, [[pulsar]]s, [[supernova]]e, [[globular cluster]]s, [[quasar]]s, [[Seyfert galaxy|Seyfert galaxies]], and [[BL Lac object]]s.<ref name="spatial">[[#HurleyConf|Hurley 1986]], p. 33</ref> All such searches were unsuccessful,<ref group="nb" name="790305b">A notable exception is the [[GRB 790305b|5 March event]] of 1979, an extremely bright burst that was successfully localized to supernova remnant [[LMC N49|N49]] in the [[Large Magellanic Cloud]]. This event is now interpreted as a [[magnetar]] [[Gamma-ray burst progenitors#Magnetar giant flares|giant flare]], more related to [[soft gamma repeater|SGR]] flares than "true" gamma-ray bursts.</ref> 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.<ref>[[#Pedersen|Pedersen 1987]]</ref><ref>[[#Hurley92|Hurley 1992]]</ref> 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.<ref name="CFishman" />

=== Afterglow ===
[[File:BeppoSAX.jpg|thumb|The Italian–Dutch satellite [[BeppoSAX]], launched in April 1996, provided the first accurate positions of gamma-ray bursts, allowing follow-up observations and identification of the sources.]]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.<ref>[[#Pac93|Paczynski 1993]]</ref> 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]]<ref group="nb" name="grbnames">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.</ref>) 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.<ref>[[#Paradijs|van Paradijs 1997]]</ref> 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.<ref name="Vedrenne p. 90">[[#VedrenneAtteia|Vedrenne & Atteia 2009]], pp. 90–93</ref><ref>[[#Schilling|Schilling 2002]], p. 102</ref>

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 [[absorption spectrum|spectrum]] of the object revealed a [[redshift]] of ''z''&nbsp;=&nbsp;0.835, placing the burst at a distance of roughly 6&nbsp;billion&nbsp;[[light year]]s from Earth.<ref>[[#Reichart|Reichart 1995]]</ref> 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.<ref name="Vedrenne p. 90" /><ref>[[#Schilling|Schilling 2002]], pp. 118–123</ref> 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.<ref name="98bw">[[#Galama|Galama 1998]]</ref>

=== More recent instruments – launched from 2000 ===
[[File:Swift spacecraft.jpg|thumb|left|[[NASA]]'s [[Swift Gamma-Ray Burst Mission|Swift Spacecraft]] launched in November 2004]]
BeppoSAX functioned until 2002 and [[Compton Gamma Ray Observatory|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, [[High Energy Transient Explorer|HETE-2]],<ref>[[#HETE|Ricker 2003]]</ref> 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 Gamma-Ray Burst Mission|Swift]], was launched in 2004 and as of May 2024 is still operational.<ref>[[#NASA2008|McCray 2008]]</ref><ref>[[#Gehrels04|Gehrels 2004]]</ref> 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 [[Slew (spacecraft)|slewed]] to observe afterglow emission following a burst. More recently, the [[Fermi Gamma-ray Space Telescope|Fermi]] mission was launched carrying the [[Fermi Gamma-ray Burst Monitor|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 [[Fermi LAT|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.<ref>[[#ROTSE|Akerlof 2003]]</ref><ref>[[#Akerlof99|Akerlof 1999]]</ref>

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]]),<ref name="Leicester">{{cite web|url=https://www2.le.ac.uk/offices/press/press-releases/2015/october/lobster-inspired-ps3-8m-super-lightweight-mirror-chosen-for-chinese-french-space-mission|title=Lobster-inspired £3.8m super lightweight mirror chosen for Chinese-French space mission|publisher=University of Leicester|date=26 October 2015|access-date=20 May 2021 |url-status=dead |archive-url=https://web.archive.org/web/20210128093757/https://www2.le.ac.uk/offices/press/press-releases/2015/october/lobster-inspired-ps3-8m-super-lightweight-mirror-chosen-for-chinese-french-space-mission |archive-date=28 Jan 2021 }}</ref> launched on 22 June 2024 (07:00:00 UTC).

The [[Taiwan Space Agency]] is launching a [[CubeSat|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.<ref>{{Cite journal |last1=Chang |first1=Hsiang-Kuang |last2=Lin |first2=Chi-Hsun |last3=Tsao |first3=Che-Chih |last4=Chu |first4=Che-Yen |last5=Yang |first5=Shun-Chia |last6=Huang |first6=Chien-You |last7=Wang |first7=Chao-Hsi |last8=Su |first8=Tze-Hsiang |last9=Chung |first9=Yun-Hsin |last10=Chang |first10=Yung-Wei |last11=Gong |first11=Zi-Jun |last12=Hsiang |first12=Jr-Yue |last13=Lai |first13=Keng-Li |last14=Lin |first14=Tsu-Hsuan |last15=Lu |first15=Chia-Yu |date=2022-01-15 |title=The Gamma-ray Transients Monitor (GTM) on board Formosat-8B and its GRB detection efficiency |journal=Advances in Space Research |volume=69 |issue=2 |pages=1249–1255 |doi=10.1016/j.asr.2021.10.044 |bibcode=2022AdSpR..69.1249C |issn=0273-1177|doi-access=free }}</ref>

===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 {{nowrap|([[GRB 080319B]])}} and the former most distant {{nowrap|([[GRB 090423]])}} emissive sources in the universe.<ref name="Bloom">[[#Bloom|Bloom 2009]]</ref><ref>[[#090423|Reddy 2009]]</ref> Prior to a flurry of discoveries from the [[James Webb Space Telescope]], the presumptive source of {{nowrap|[[GRB 090429B]]}} was the most distant known object in the universe.

In October 2018, astronomers reported that {{nowrap|GRB 150101B}} (detected in 2015) and [[GW170817]], a [[gravitational wave]] event detected in 2017 (which has been associated with {{nowrap|GRB 170817A}}, a burst detected 1.7 seconds later), may have been produced by the same mechanism—the [[Neutron star merger|merger]] of two [[neutron star]]s. 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 [[Galaxy|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.<ref name="EA-20181016">{{cite press release |author=University of Maryland |title=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 |url=https://www.eurekalert.org/pub_releases/2018-10/uom-ait101518.php |date=16 October 2018 |work=[[EurekAlert!]] |access-date=17 October 2018 |author-link=University of Maryland |archive-date=16 October 2018 |archive-url=https://web.archive.org/web/20181016142323/https://www.eurekalert.org/pub_releases/2018-10/uom-ait101518.php |url-status=dead }}</ref><ref name="NC-20181016">{{cite journal |author=Troja, E.|display-authors=etal |title=A luminous blue kilonova and an off-axis jet from a compact binary merger at z = 0.1341 |date=16 October 2018 |journal=[[Nature Communications]] |volume=9 |pages=4089 |number=4089 (2018) |doi=10.1038/s41467-018-06558-7 |pmid=30327476 |pmc=6191439 |arxiv=1806.10624 |bibcode=2018NatCo...9.4089T }}</ref><ref name="NASA-20181016">{{cite news |last=Mohon |first=Lee |title=GRB 150101B: A Distant Cousin to GW170817 |url=https://www.nasa.gov/mission_pages/chandra/images/grb-150101b-a-distant-cousin-to-gw170817.html |date=16 October 2018 |work=[[NASA]] |access-date=17 October 2018 }}</ref><ref name="SPC-20181017">{{cite web |last=Wall |first=Mike |title=Powerful Cosmic Flash Is Likely Another Neutron-Star Merger |url=https://www.space.com/42158-another-neutron-star-crash-detected.html |date=17 October 2018 |work=[[Space.com]] |access-date=17 October 2018 }}</ref>

The highest energy light observed from a gamma-ray burst was one [[Electronvolt|teraelectronvolt]], from {{nowrap|[[GRB 190114C]]}} in 2019.<ref name="NAT-20191120">{{cite journal |author=Veres, P |s2cid=208191199 |display-authors=et al. |title=Observation of inverse Compton emission from a long γ-ray burst |date=20 November 2019 |journal=[[Nature (journal)|Nature]] |volume=575 |issue=7783 |pages=459–463 |doi=10.1038/s41586-019-1754-6 |pmid=31748725 |arxiv=2006.07251 |bibcode=2019Natur.575..459M }}</ref> 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.<ref>{{Cite web |date=2021-05-21 |title=Record-breaking light has more than a quadrillion electron volts of energy |url=https://www.sciencenews.org/article/light-energy-record-gamma-ray |access-date=2022-05-11 |website=Science News |first=Emily |last=Conover |language=en-US}}</ref>

== Classification ==
[[File:GRB BATSE 12lightcurves.png|thumb|Gamma-ray burst light curves]]The [[light curve]]s of gamma-ray bursts are extremely diverse and complex.<ref>[[#Katz|Katz 2002]], p. 37</ref> No two gamma-ray burst light curves are identical,<ref>[[#Marani|Marani 1997]]</ref> 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 "[[Gamma-ray burst precursor|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.<ref name="Lazzati">[[#Lazzati|Lazatti 2005]]</ref> The light curves of some events have extremely chaotic and complicated profiles with almost no discernible patterns.<ref name="CFishman">[[#CFishman|Fishman & Meegan 1995]]</ref>

Although some light curves can be roughly reproduced using certain simplified models,<ref>[[#Simic|Simić 2005]]</ref> 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<ref group="nb" name="T90">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.</ref> for a large number of gamma-ray bursts show a clear [[bimodal distribution|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.<ref name="Kouveliotou">[[#Kouveliotou|Kouveliotou 1994]]</ref> 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.<ref name="Horvath98">[[#Horvath98|Horvath 1998]]</ref><ref name="Hakkila">[[#Hakkila|Hakkila 2003]]</ref><ref name="Chattopadhyay">[[#Chattopadhyay|Chattopadhyay 2007]]</ref><ref name="Virgili">[[#Virgili|Virgili 2009]]</ref>

=== Short gamma-ray bursts ===
[[File:Hubble captures infrared glow of a kilonova blast.jpg|thumb|left|[[Hubble Space Telescope|Hubble]] image of the infrared glow of a [[kilonova]] blast.<ref>{{cite web|title=Hubble captures infrared glow of a kilonova blast |url=http://www.spacetelescope.org/images/opo1329a/|work=Image Gallery|publisher=ESA/Hubble |date=5 August 2013 |access-date=14 August 2013}}</ref>]][[File:GRB211106A.gif|thumb|GRB 211106A, one of the most energetic sGRB ever registered, in the first-ever time-lapse movie of a GRB in millimeter-wavelength light, as seen by the Atacama Large Millimeter/{{zwsp}}submillimeter Array (ALMA)<ref>{{Cite journal |last1=Laskar |first1=Tanmoy |last2=Escorial |first2=Alicia Rouco |last3=Schroeder |first3=Genevieve |last4=Fong |first4=Wen-fai |last5=Berger |first5=Edo |last6=Veres |first6=Péter |last7=Bhandari |first7=Shivani |last8=Rastinejad |first8=Jillian |last9=Kilpatrick |first9=Charles D. |last10=Tohuvavohu |first10=Aaron |last11=Margutti |first11=Raffaella |last12=Alexander |first12=Kate D. |last13=DeLaunay |first13=James |last14=Kennea |first14=Jamie A. |last15=Nugent |first15=Anya |date=2022-08-01 |title=The First Short GRB Millimeter Afterglow: The Wide-angled Jet of the Extremely Energetic SGRB 211106A |journal=The Astrophysical Journal Letters |volume=935 |issue=1 |pages=L11 |doi=10.3847/2041-8213/ac8421 |arxiv=2205.03419 |bibcode=2022ApJ...935L..11L |s2cid=248572470 |doi-access=free }}</ref><ref>{{Cite web |title=Out With a Bang: Explosive Neutron Star Merger Captured for the First Time in Millimeter Light |url=https://public.nrao.edu/news/neutron-star-merger-millimeter-alma/ |access-date=2022-08-14 |website=National Radio Astronomy Observatory |language=en-US}}</ref><ref>{{Cite web |title=Explosive neutron star merger captured for first time in millimeter light |url=https://news.northwestern.edu/stories/2022/08/explosive-neutron-star-merger-captured-for-first-time-in-millimeter-light/ |access-date=2022-08-14 |website=news.northwestern.edu |language=en}}</ref>]]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.<ref name=r1>[http://www.nasa.gov/mission_pages/swift/bursts/short_burst_oct5.html 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.</ref> 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 galaxy|elliptical galaxies]].<ref>[[#Bloom06|Bloom 2006]]</ref><ref>[[#Hjorth|Hjorth 2005]]</ref><ref>[[#Gehrels05|Gehrels 2005]]</ref> 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.<ref name="Woosley06" />

The true nature of these objects was thus initially unknown, but the leading hypothesis was that they originated from the [[Neutron star merger|mergers of binary neutron stars]] or a neutron star with a [[black hole]]. Such mergers were hypothesized to produce [[kilonova]]e,<ref>{{Cite journal |last1=Li |first1=Li-Xin |last2=Paczyński |first2=Bohdan |date=1998-09-21 |title=Transient Events from Neutron Star Mergers |url=https://iopscience.iop.org/article/10.1086/311680/meta |journal=The Astrophysical Journal |language=en |volume=507 |issue=1 |pages=L59 |doi=10.1086/311680 |arxiv=astro-ph/9807272 |bibcode=1998ApJ...507L..59L |s2cid=3091361 |issn=0004-637X}}</ref> and evidence for a kilonova associated with short GRB 130603B was reported in 2013.<ref name=Tanvir2013>{{cite journal | doi = 10.1038/nature12505| pmid = 23912055| title = A 'kilonova' associated with the short-duration γ-ray burst GRB 130603B| journal = Nature| volume = 500| issue = 7464| pages = 547–549| year = 2013| last1 = Tanvir | first1 = N. R.| last2 = Levan | first2 = A. J.| last3 = Fruchter | first3 = A. S.| last4 = Hjorth | first4 = J.| last5 = Hounsell | first5 = R. A.| last6 = Wiersema | first6 = K.| last7 = Tunnicliffe | first7 = R. L.| s2cid = 205235329|arxiv = 1306.4971 |bibcode = 2013Natur.500..547T }}</ref><ref name=Dnews>{{cite web |url=http://news.discovery.com/space/astronomy/how-a-kilonova-solved-a-gamma-ray-burst-mystery-130807.htm |title=Kilonova Alert! Hubble Solves Gamma Ray Burst Mystery |access-date=22 January 2015 |date=7 August 2013 |website=Discovery News |first=Nicole |last=Gugliucci |archive-date=3 March 2016 |archive-url=https://web.archive.org/web/20160303182001/http://news.discovery.com/space/astronomy/how-a-kilonova-solved-a-gamma-ray-burst-mystery-130807.htm |url-status=dead }}</ref> The mean duration of sGRB events of around 200 milliseconds implied (due to [[Special relativity#Causality and prohibition of motion faster than light|causality]]) that the sources must be of very small physical diameter in stellar terms: less than 0.2 light-seconds (60,000&nbsp;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 would remain in orbit, spiraling into the black hole over a longer period of time.<ref name=r1 />

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.<ref name="PhysRev">{{cite journal|last1=Abbott|first1=B. P.|collaboration=[[LIGO Scientific Collaboration]] & [[Virgo interferometer|Virgo Collaboration]]|title=GW170817: Observation of Gravitational Waves from a Binary Neutron Star Inspiral|journal=Physical Review Letters|date=16 October 2017|volume=119|issue=16|pages=161101|doi=10.1103/PhysRevLett.119.161101|pmid=29099225|arxiv=1710.05832|bibcode=2017PhRvL.119p1101A|s2cid=217163611 }}</ref>

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.<ref name="Frederiks">[[#Frederiks|Frederiks 2008]]</ref><ref>[[#Hurley05|Hurley 2005]]</ref>

=== Long gamma-ray bursts===
{{main category|Long-duration gamma-ray bursts}}
[[File:Xrt image crop.jpg|thumb|Swift captured the afterglow of [[GRB 221009A]] about an hour after it was first detected reaching Earth on October 9, 2022. The bright rings form as a result of X-rays scattered from otherwise unobservable dust layers within our galaxy that lie in the direction of the burst.]]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.<ref name="Woosley06">[[#Woosley06|Woosley & Bloom 2006]]</ref><ref>{{Cite journal |last1=Hjorth |first1=Jens |last2=Sollerman |first2=Jesper |last3=Møller |first3=Palle |last4=Fynbo |first4=Johan P. U. |last5=Woosley |first5=Stan E. |last6=Kouveliotou |first6=Chryssa |last7=Tanvir |first7=Nial R. |last8=Greiner |first8=Jochen |last9=Andersen |first9=Michael I. |last10=Castro-Tirado |first10=Alberto J. |last11=Castro Cerón |first11=José María |last12=Fruchter |first12=Andrew S. |last13=Gorosabel |first13=Javier |last14=Jakobsson |first14=Páll |last15=Kaper |first15=Lex |date=2003-06-19 |title=A very energetic supernova associated with the γ-ray burst of 29 March 2003 |url=https://www.nature.com/articles/nature01750 |journal=Nature |language=en |volume=423 |issue=6942 |pages=847–850 |doi=10.1038/nature01750 |pmid=12815425 |issn=0028-0836|arxiv=astro-ph/0306347 |bibcode=2003Natur.423..847H }}</ref> Long GRB afterglow observations, at high redshift, are also consistent with the GRB having originated in star-forming regions.<ref name="Pontzen">[[#Pontzen|Pontzen et al. 2010]]</ref>

In December 2022, astronomers reported the observation of GRB&nbsp;211211A for 51 seconds, the first evidence of a long GRB likely associated with mergers of "compact binary objects" such as [[neutron star merger|neutron stars]] or [[white dwarf]]s.<ref>{{Cite journal |last1=Rastinejad |first1=Jillian C. |last2=Gompertz |first2=Benjamin P. |last3=Levan |first3=Andrew J. |last4=Fong |first4=Wen-fai |last5=Nicholl |first5=Matt |last6=Lamb |first6=Gavin P. |last7=Malesani |first7=Daniele B. |last8=Nugent |first8=Anya E. |last9=Oates |first9=Samantha R. |last10=Tanvir |first10=Nial R. |last11=de Ugarte Postigo |first11=Antonio |last12=Kilpatrick |first12=Charles D. |last13=Moore |first13=Christopher J. |last14=Metzger |first14=Brian D. |last15=Ravasio |first15=Maria Edvige |date=2022-12-08 |title=A kilonova following a long-duration gamma-ray burst at 350 Mpc |url=https://www.nature.com/articles/s41586-022-05390-w |journal=Nature |language=en |volume=612 |issue=7939 |pages=223–227 |doi=10.1038/s41586-022-05390-w |pmid=36477128 |issn=0028-0836|arxiv=2204.10864 |bibcode=2022Natur.612..223R }}</ref><ref>{{Cite journal |last1=Troja |first1=E. |last2=Fryer |first2=C. L. |last3=O’Connor |first3=B. |last4=Ryan |first4=G. |last5=Dichiara |first5=S. |last6=Kumar |first6=A. |last7=Ito |first7=N. |last8=Gupta |first8=R. |last9=Wollaeger |first9=R. T. |last10=Norris |first10=J. P. |last11=Kawai |first11=N. |last12=Butler |first12=N. R. |last13=Aryan |first13=A. |last14=Misra |first14=K. |last15=Hosokawa |first15=R. |date=2022-12-08 |title=A nearby long gamma-ray burst from a merger of compact objects |journal=Nature |language=en |volume=612 |issue=7939 |pages=228–231 |doi=10.1038/s41586-022-05327-3 |issn=0028-0836 |pmc=9729102 |pmid=36477127|arxiv=2209.03363 |bibcode=2022Natur.612..228T }}</ref><ref>{{Cite web |date=2022-12-07 |title=Kilonova Discovery Challenges our Understanding of Gamma-Ray Bursts |url=https://www.gemini.edu/pr/kilonova-discovery-challenges-our-understanding-gamma-ray-bursts |access-date=2022-12-11 |website=Gemini Observatory |language=en}}</ref> Following this, GRB&nbsp;191019A (2019, 64s)<ref>{{Cite journal |last1=Levan |first1=Andrew J. |last2=Malesani |first2=Daniele B. |last3=Gompertz |first3=Benjamin P. |last4=Nugent |first4=Anya E. |last5=Nicholl |first5=Matt |last6=Oates |first6=Samantha R. |last7=Perley |first7=Daniel A. |last8=Rastinejad |first8=Jillian |last9=Metzger |first9=Brian D. |last10=Schulze |first10=Steve |last11=Stanway |first11=Elizabeth R. |last12=Inkenhaag |first12=Anne |last13=Zafar |first13=Tayyaba |last14=Agüí Fernández |first14=J. Feliciano |last15=Chrimes |first15=Ashley A. |date=2023-06-22 |title=A long-duration gamma-ray burst of dynamical origin from the nucleus of an ancient galaxy |url=https://www.nature.com/articles/s41550-023-01998-8 |journal=Nature Astronomy |language=en |volume=7 |issue=8 |pages=976–985 |doi=10.1038/s41550-023-01998-8 |issn=2397-3366|arxiv=2303.12912 |bibcode=2023NatAs...7..976L }}</ref> and [[GRB 230307A]] (2023, 35s)<ref>{{cite web |title=GCN - Circulars - 33410: Solar Orbiter STIX observation of GRB 230307A |url=https://gcn.nasa.gov/circulars/33410}}</ref><ref>{{cite web |title=GCN - Circulars - 33412: GRB 230307A: AGILE/MCAL detection |url=https://gcn.nasa.gov/circulars/33412}}</ref> have been argued to signify an emerging class of long GRB which may originate from these types of progenitor events.<ref>{{Cite web |last=Wodd |first=Charlie |date=11 December 2023 |title=Extra-Long Blasts Challenge Our Theories of Cosmic Cataclysms |url=https://www.quantamagazine.org/extra-long-blasts-challenge-our-theories-of-cosmic-cataclysms-20231211/ |website=[[Quanta magazine]]}}</ref>

=== 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|blue supergiant star]],<ref>{{cite journal |bibcode=2013ApJ...766...30G |doi=10.1088/0004-637X/766/1/30 |title=The Ultra-Long Gamma-Ray Burst 111209A: The Collapse of a Blue Supergiant? |journal=The Astrophysical Journal |volume=766 |issue=1 |page=30 |date=2013 |last1=Gendre |first1=B. |last2=Stratta |first2=G. |last3=Atteia |first3=J. L. |last4=Basa |first4=S. |last5=Boër |first5=M. |last6=Coward |first6=D. M. |last7=Cutini |first7=S. |last8=d'Elia |first8=V. |last9=Howell |first9=E. J |last10=Klotz |first10=A. |last11=Piro |first11=L. |s2cid=118618287 |arxiv = 1212.2392 }}</ref> a [[tidal disruption event]]<ref name="Greiner Mazzali Kann Krühler pp. 189–192">{{cite journal | last1=Greiner | first1=Jochen | last2=Mazzali | first2=Paolo A. | last3=Kann | first3=D. Alexander | last4=Krühler | first4=Thomas | last5=Pian | first5=Elena | last6=Prentice | first6=Simon | last7=Olivares E. | first7=Felipe | last8=Rossi | first8=Andrea | last9=Klose | first9=Sylvio | last10=Taubenberger | first10=Stefan | last11=Knust | first11=Fabian | last12=Afonso | first12=Paulo M. J. | last13=Ashall | first13=Chris | last14=Bolmer | first14=Jan | last15=Delvaux | first15=Corentin | last16=Diehl | first16=Roland | last17=Elliott | first17=Jonathan | last18=Filgas | first18=Robert | last19=Fynbo | first19=Johan P. U. | last20=Graham | first20=John F. | last21=Guelbenzu | first21=Ana Nicuesa | last22=Kobayashi | first22=Shiho | last23=Leloudas | first23=Giorgos | last24=Savaglio | first24=Sandra | last25=Schady | first25=Patricia |author25-link= Patricia Schady | last26=Schmidl | first26=Sebastian | last27=Schweyer | first27=Tassilo | last28=Sudilovsky | first28=Vladimir | last29=Tanga | first29=Mohit | last30=Updike | first30=Adria C. | last31=van Eerten | first31=Hendrik | last32=Varela | first32=Karla | s2cid=4464998 | title=A very luminous magnetar-powered supernova associated with an ultra-long γ-ray burst | journal=Nature | volume=523 | issue=7559 | date=2015-07-08  | doi=10.1038/nature14579 | pmid=26156372 | display-authors=29 | pages=189–192|arxiv = 1509.03279 |bibcode = 2015Natur.523..189G }}</ref><ref name="Levan Tanvir Starling Wiersema">{{cite journal | last1=Levan | first1=A. J. | last2=Tanvir | first2=N. R. | last3=Starling | first3=R. L. C. | last4=Wiersema | first4=K. | last5=Page | first5=K. L. | last6=Perley | first6=D. A. | last7=Schulze | first7=S. | last8=Wynn | first8=G. A. | last9=Chornock | first9=R. | last10=Hjorth | first10=J. | last11=Cenko | first11=S. B. | last12=Fruchter | first12=A. S. | last13=O'Brien | first13=P. T. | last14=Brown | first14=G. C. | last15=Tunnicliffe | first15=R. L. | last16=Malesani | first16=D. | last17=Jakobsson | first17=P. | last18=Watson | first18=D. | last19=Berger | first19=E. | last20=Bersier | first20=D. | last21=Cobb | first21=B. E. | last22=Covino | first22=S. | last23=Cucchiara | first23=A. | last24=de Ugarte Postigo | first24=A. | last25=Fox | first25=D. B. | last26=Gal-Yam | first26=A. | last27=Goldoni | first27=P. | last28=Gorosabel | first28=J. | last29=Kaper | first29=L. | last30=Krühler | first30=T. | last31=Karjalainen | first31=R. | last32=Osborne | first32=J. P. | last33=Pian | first33=E. | last34=Sánchez-Ramírez | first34=R. | last35=Schmidt | first35=B. | last36=Skillen | first36=I. | last37=Tagliaferri | first37=G. | last38=Thöne | first38=C. | last39=Vaduvescu | first39=O. | last40=Wijers | first40=R. A. M. J. | last41=Zauderer | first41=B. A. | title=A new population of ultra-long duration gamma-ray bursts | journal=The Astrophysical Journal | volume=781 | issue=1 | year=2014 |display-authors=29 | arxiv=1302.2352 | doi=10.1088/0004-637x/781/1/13 | page=13 | bibcode=2014ApJ...781...13L| s2cid=24657235 }}</ref> or a new-born [[magnetar]].<ref name="Greiner Mazzali Kann Krühler pp. 189–192" /><ref name="Ioka Hotokezaka Piran p=110">{{cite journal | last1=Ioka | first1=Kunihito | last2=Hotokezaka | first2=Kenta | last3=Piran | first3=Tsvi | s2cid=118629696 | title=Are Ultra-Long Gamma-Ray Bursts Caused by Blue Supergiant Collapsars, Newborn Magnetars, or White Dwarf Tidal Disruption Events? | journal=The Astrophysical Journal | volume=833 | issue=1 | date=2016-12-12  | doi=10.3847/1538-4357/833/1/110 | page=110|arxiv = 1608.02938 |bibcode = 2016ApJ...833..110I | doi-access=free }}</ref> 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]].<ref name="Levan Tanvir Starling Wiersema"/><ref>{{cite journal |arxiv=1310.4944 |last1=Boer |first1=Michel |title=Are Ultra-long Gamma-Ray Bursts different? |journal=The Astrophysical Journal |volume=800 |issue=1 |pages=16 |last2=Gendre |first2=Bruce |last3=Stratta |first3=Giulia |s2cid=118655406 |doi=10.1088/0004-637X/800/1/16 |date=2013 |bibcode = 2015ApJ...800...16B }}</ref><ref>{{cite journal |bibcode=2013ApJ...778...54V |doi=10.1088/0004-637X/778/1/54 |title=Grb 091024A and the Nature of Ultra-Long Gamma-Ray Bursts |journal=The Astrophysical Journal |volume=778 |issue=1 |page=54 |date=2013 |last1=Virgili |first1=F. J. |last2=Mundell |first2=C. G. |last3=Pal'Shin |first3=V. |last4=Guidorzi |first4=C. |last5=Margutti |first5=R. |last6=Melandri |first6=A. |last7=Harrison |first7=R. |last8=Kobayashi |first8=S. |last9=Chornock |first9=R. |last10=Henden |first10=A. |last11=Updike |first11=A. C. |last12=Cenko |first12=S. B. |last13=Tanvir |first13=N. R. |last14=Steele |first14=I. A. |last15=Cucchiara |first15=A. |last16=Gomboc |first16=A. |last17=Levan |first17=A. |last18=Cano |first18=Z. |last19=Mottram |first19=C. J. |last20=Clay |first20=N. R. |last21=Bersier |first21=D. |last22=Kopač |first22=D. |last23=Japelj |first23=J. |last24=Filippenko |first24=A. V. |last25=Li |first25=W. |last26=Svinkin |first26=D. |last27=Golenetskii |first27=S. |last28=Hartmann |first28=D. H. |last29=Milne |first29=P. A. |last30=Williams |first30=G. |s2cid=119023750 |display-authors=29 |arxiv = 1310.0313 }}</ref> 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.<ref name="Levan Tanvir Starling Wiersema"/> A 2013 study,<ref>{{cite journal |arxiv=1310.2540 |last1=Zhang |first1=Bin-Bin |title=How Long does a Burst Burst? |journal=The Astrophysical Journal |volume=787 |issue=1 |page=66 |last2=Zhang |first2=Bing |last3=Murase |first3=Kohta |last4=Connaughton |first4=Valerie |last5= Briggs |first5=Michael S. |s2cid=56273013 |year=2014 |doi=10.1088/0004-637X/787/1/66 |bibcode = 2014ApJ...787...66Z }}</ref> 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 ==
[[File:GRB080319B illustration NASA.jpg|thumb|Artist's illustration of a bright gamma-ray burst occurring in a star-forming region. Energy from the explosion is beamed into two narrow, oppositely directed jets.]]Gamma-ray bursts are very bright as observed from Earth despite their typically immense distances. An average long GRB has a [[bolometric magnitude|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,<ref name="Racusin">[[#Racusin08|Racusin 2008]]</ref> comparable to that of the dimmest naked-eye stars despite the burst's distance of 7.5&nbsp;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 [[Mass–energy equivalence|rest-mass energy]] of the [[Sun]] (the energy which would be released were the Sun to be converted entirely into radiation).<ref name="Bloom" />

Gamma-ray bursts are thought to be highly focused explosions, with most of the explosion energy [[collimated light|collimated]] into a narrow [[relativistic jet|jet]].<ref>[[#Rykoff|Rykoff 2009]]</ref><ref>[[#Abdo|Abdo 2009]]</ref> The jets of gamma-ray bursts are [[Ultrarelativistic limit|ultrarelativistic]], and are the most relativistic jets in the universe.<ref>{{Cite journal |last1=Dereli-Bégué |first1=Hüsne |last2=Pe’er |first2=Asaf |last3=Ryde |first3=Felix |last4=Oates |first4=Samantha R. |last5=Zhang |first5=Bing |last6=Dainotti |first6=Maria G. |date=2022-09-24 |title=A wind environment and Lorentz factors of tens explain gamma-ray bursts X-ray plateau |journal=Nature Communications |language=en |volume=13 |issue=1 |pages=5611 |doi=10.1038/s41467-022-32881-1 |pmid=36153328 |pmc=9509382 |arxiv=2207.11066 |bibcode=2022NatCo..13.5611D |issn=2041-1723}}</ref><ref>{{Cite journal |last=Pe’er |first=Asaf |date=2019 |title=Plasmas in Gamma-Ray Bursts: Particle Acceleration, Magnetic Fields, Radiative Processes and Environments |journal=Galaxies |language=en |volume=7 |issue=1 |pages=33 |doi=10.3390/galaxies7010033 |arxiv=1902.02562 |bibcode=2019Galax...7...33P |issn=2075-4434 |doi-access=free }}</ref> The matter in gamma-ray burst jets may also become [[Faster-than-light|superluminal]], or faster than the speed of light in the jet medium, with there also being effects of [[time reversibility]].<ref>{{Cite journal |last1=Hakkila |first1=Jon |last2=Nemiroff |first2=Robert |date=2019-09-23 |title=Time-reversed Gamma-Ray Burst Light-curve Characteristics as Transitions between Subluminal and Superluminal Motion |journal=The Astrophysical Journal |language=en |volume=883 |issue=1 |pages=70 |doi=10.3847/1538-4357/ab3bdf |arxiv=1908.07306 |bibcode=2019ApJ...883...70H |issn=0004-637X |doi-access=free }}</ref><ref>{{Cite web |last=Ratner |first=Paul |date=2019-09-25 |title=Astrophysicists: Gamma-ray jets exceed the speed of light |url=https://bigthink.com/hard-science/astrophysicists-gamma-ray-jets-speed-of-light/ |access-date=2023-10-11 |website=Big Think |language=en-US}}</ref><ref>{{Cite web |last=Siegel |first=Ethan |author-link=Ethan Siegel |date=2019-10-05 |title=Ask Ethan: Can Gamma-Ray Jets Really Travel Faster Than The Speed Of Light? |url=https://www.forbes.com/sites/startswithabang/2019/10/05/ask-ethan-can-gamma-ray-jets-really-travel-faster-than-the-speed-of-light/ |access-date=2023-10-11 |website=Forbes |language=en}}</ref> 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 [[relativistic beaming|beam]] its radiation as effectively.<ref name="Sari99">[[#Sari99|Sari 1999]]</ref><ref>[[#Burrows|Burrows 2006]]</ref> Observations suggest significant variation in the jet angle from between 2 and 20 degrees.<ref name="Frail">[[#Frail|Frail 2001]]</ref>

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<sup>44</sup>&nbsp;J,{{snd}}which is larger than the total energy (10<sup>44</sup>&nbsp;J) of ordinary [[supernova]]e (type [[Type Ia supernova|Ia]], [[Type Ib and Ic supernovae|Ibc]], [[Type II supernova|II]]),<ref name="Frail" /> with gamma-ray bursts also being more [[Power (physics)|powerful]] than the typical supernova.<ref>{{Cite book |last=Melia |first=Fulvio |author-link=Fulvio Melia |title=High-Energy Astrophysics |publisher=Princeton University Press |year=2009 |isbn=978-0-691-13543-4 |pages=241 |language=en}}</ref> Very bright supernovae have been observed to accompany several of the nearest GRBs.<ref name="98bw" /> Further support for focusing of the output of GRBs comes from observations of strong asymmetries in the spectra of nearby [[Type Ib and Ic supernovae|type Ic supernovae]]<ref>[[#Mazzali|Mazzali 2005]]</ref> and from radio observations taken long after bursts when their jets are no longer relativistic.<ref>[[#Frail2000|Frail 2000]]</ref>

The discovery of [[GRB 190114C]] suggests that previous observations may have underestimated the total energy output of GRBs.<ref>{{Cite web |last=Billings |first=Lee |date=2019-11-20 |title=Record-Breaking Gamma Rays Reveal Secrets of the Universe's Most Powerful Explosions |url=https://www.scientificamerican.com/article/record-breaking-gamma-rays-reveal-secrets-of-the-universes-most-powerful-explosions/ |access-date=2023-09-17 |website=Scientific American |language=en}}</ref> Measurements indicate that the energy released in very-high-energy gamma rays may be comparable to the combined energy emitted at all lower wavelengths.<ref>{{Cite web |last=Choi |first=Charles Q. |date=2019-11-20 |title=The Most Powerful Explosions in the Universe Emit Way More Energy Than Anyone Thought |url=https://www.space.com/gamma-ray-bursts-high-energy-light.html |access-date=2023-09-17 |website=Space.com |language=en}}</ref>

Short (time duration) GRBs appear to come from a lower-redshift (i.e. less distant) population and are less luminous than long GRBs.<ref name="SHBhosts">[[#Prochaska|Prochaska 2006]]</ref> The degree of beaming in short bursts has not been accurately measured, but as a population they are likely less collimated than long GRBs<ref>[[#Watson|Watson 2006]]</ref> or possibly not collimated at all in some cases.<ref>[[#Grupe|Grupe 2006]]</ref>

== Progenitors ==
{{Main|Gamma-ray burst progenitors}}
[[File:Wolf rayet2.jpg|thumb|Hubble Space Telescope image of [[Wolf–Rayet star]] [[WR 124]] and its surrounding nebula. Wolf–Rayet stars are candidates for being progenitors of long-duration GRBs.]]
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 [[Hypernova|collapsar]] model,<ref>[[#Mac99|MacFadyen 1999]]</ref> in which the core of an extremely massive, low-[[metallicity]], rapidly rotating star collapses into a [[black hole]] in the final stages of its [[stellar evolution|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 jet]]s 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]],<ref>{{Cite journal |last1=Zhang |first1=Bing |last2=Mészáros |first2=Peter |s2cid=18660804 |date=2001-05-01 |title=Gamma-Ray Burst Afterglow with Continuous Energy Injection: Signature of a Highly Magnetized Millisecond Pulsar |bibcode=2001ApJ...552L..35Z |journal=The Astrophysical Journal Letters |volume=552 |issue=1 |pages=L35–L38 |doi=10.1086/320255 |arxiv = astro-ph/0011133 }}</ref><ref>{{Cite journal |last1=Troja |first1=E. |last2=Cusumano |first2=G. |last3=O'Brien |first3=P. T. |last4=Zhang |first4=B. |last5=Sbarufatti |first5=B. |last6=Mangano |first6=V. |last7=Willingale |first7=R. |last8=Chincarini |first8=G. |last9=Osborne |first9=J. P. |s2cid=14317593 |date=2007-08-01 |title=Swift Observations of GRB 070110: An Extraordinary X-Ray Afterglow Powered by the Central Engine |bibcode=2007ApJ...665..599T |journal=The Astrophysical Journal |volume=665 |issue=1 |pages=599–607 |doi=10.1086/519450 |arxiv = astro-ph/0702220 }}</ref> 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.

The closest analogs within the Milky Way galaxy of the stars producing long gamma-ray bursts are likely the [[Wolf–Rayet star]]s, extremely hot and massive stars, which have shed most or all of their hydrogen envelope. [[Eta Carinae]], [[Apep (star system)|Apep]], and [[WR 104]] have been cited as possible future gamma-ray burst progenitors.<ref>[[#Plait|Plait 2008]]</ref> It is unclear if any star in the Milky Way has the appropriate characteristics to produce a gamma-ray burst.<ref name="Stanek">[[#Stanek|Stanek 2006]]</ref>

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 halo]]s.<ref name="SHBhosts" /> 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<ref>[[#Abbott|Abbott 2007]]</ref><ref>[[#Kochanek|Kochanek 1993]]</ref> 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 [[black hole evaporation|evaporation]] of [[primordial black hole]]s.<ref>[[#Vietri|Vietri 1998]]</ref><ref>[[#Mac2006|MacFadyen 2006]]</ref><ref>[[#Blinnikov|Blinnikov 1984]]</ref><ref name="cline">[[#Cline|Cline 1996]]</ref>

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.<ref>Winterberg, Friedwardt (2001 Aug 29). "Gamma-Ray Bursters and Lorentzian Relativity". Z. Naturforsch 56a: 889–892.</ref>

=== Tidal disruption events ===
{{Main|Tidal disruption event}}
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.<ref>{{cite news |last1=Cendes |first1=Yvette |title=How do black holes swallow stars? |url=https://www.astronomy.com/science/how-do-black-holes-swallow-stars/ |access-date=8 May 2024 |work=Astronomy Magazine |date=8 December 2021}}</ref>

Since 2011, only 4 jetted TDEs have been discovered, of which 3 were detected in gamma-rays (including Swift J1644+57).<ref name="TDE-jets">{{cite web |last1=Hensley |first1=Kerry |title=Why Are Jets from Disrupted Stars So Rare? |url=https://aasnova.org/2023/11/08/why-are-jets-from-disrupted-stars-so-rare/ |website=AAS Nova |date=8 November 2023}}</ref>  It is estimated that just 1% of all TDEs are jetted events.<ref name="TDE-jets" />

== Emission mechanisms ==
{{Main|Gamma-ray burst emission mechanisms}}
[[File:Gamma-ray-burst-Mechanism.jpg|thumb|left|400px|Gamma-ray burst mechanism]]
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.<ref>[[#Stern|Stern 2007]]</ref> 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.<ref>[[#GFishman|Fishman, G. 1995]]</ref> 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.<ref>[[#FanPiran|Fan & Piran 2006]]</ref> 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,<ref name="Racusin" /><ref name="Liang Crider Boettcher Smith 1999">{{cite journal | last1=Liang | first1=E. P. | last2=Crider | first2=A. | last3=Boettcher | first3=M. | last4=Smith | first4=I. A. | title=GRB990123: The Case for Saturated Comptonization | journal=The Astrophysical Journal | date=1999-03-29 | volume=519 | issue=1 | pages=L21–L24 | doi=10.1086/312100 | bibcode=1999ApJ...519L..21L | s2cid=16005521 | arxiv=astro-ph/9903438 }}</ref> have suggested that [[Compton scattering|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.<ref>[[#Wozniak09|Wozniak 2009]]</ref>

The nature of the longer-wavelength afterglow emission (ranging from [[X-ray]] through [[radio waves|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 speed|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]].<ref>[[#Meszaros|Meszaros 1997]]</ref><ref>[[#Sari98|Sari 1998]]</ref> 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.<ref>[[#Nousek|Nousek 2006]]</ref>
{{clear|left}}

== Rate of occurrence and potential effects on life ==
[[File:GROND image of the gamma-ray burst GRB 151027B.jpg|thumb|On 27 October 2015, at 22:40 GMT, the NASA/ASI/UKSA Swift satellite discovered its 1000th gamma-ray burst (GRB).<ref>{{cite web|title=ESO Telescopes Observe Swift Satellite's 1000th Gamma-ray Burst|url=http://www.eso.org/public/announcements/ann15085/ |date=6 November 2015 |access-date=9 November 2015}}</ref>]]

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.<ref>{{cite journal |last1=Piran |first1=Tsvi |last2=Jimenez |first2=Raul |s2cid=43491624 |title=Possible Role of Gamma Ray Bursts on Life Extinction in the Universe |journal=Physical Review Letters |date=5 December 2014 |volume=113 |issue=23 |pages=231102 |doi=10.1103/PhysRevLett.113.231102|pmid=25526110 |arxiv=1409.2506 |bibcode=2014PhRvL.113w1102P }}</ref><ref>{{cite journal |last=Schirber |first=Michael |title=Focus: Gamma-Ray Bursts Determine Potential Locations for Life |journal=Physics |volume=7 |page=124|date=2014-12-08 |doi=10.1103/Physics.7.124 }}</ref>

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<ref>{{Cite web|url=https://www.universetoday.com/118140/are-gamma-ray-bursts-dangerous/|title=Are Gamma Ray Bursts Dangerous?|first=Fraser|last=Cain|date=January 12, 2015}}</ref> and its emission were beamed straight towards Earth, the effects could be harmful and potentially devastating for its [[ecosystem]]s. Currently, orbiting satellites detect on average approximately one GRB per day. The closest observed GRB as of March 2014 was [[GRB 980425]], located {{convert|40|Mpc|ly}}<ref>{{cite journal |last1=Soderberg |first1= A. M. |author1-link=Alicia M. Soderberg |title=The sub-energetic γ-ray burst GRB 031203 as a cosmic analogue to the nearby GRB 980425 |journal=Nature |date=2004 |volume=430 |issue=7000 |pages=648–650 |doi= 10.1038/nature02757 |pmid=15295592 |last2=Kulkarni |first2=S. R. |last3=Berger |first3=E. |last4=Fox |first4=D. W. |last5=Sako |first5=M. |last6=Frail |first6=D. A. |last7=Gal-Yam |first7=A. |last8=Moon |first8=D. S. |last9=Cenko |first9=S. B. |last10=Yost |first10=S. A. |last11=Phillips |first11=M. M. |last12=Persson |first12=S. E. |last13=Freedman |first13=W. L. |last14=Wyatt |first14=P. |last15=Jayawardhana |first15=R. |last16=Paulson |first16=D. |s2cid= 4363027 |arxiv = astro-ph/0408096 |bibcode = 2004Natur.430..648S |hdl= 2027.42/62961 }}</ref> away ([[Redshift#Measurement, characterization, and interpretation|z]]=0.0085) in an SBc-type dwarf galaxy.<ref>{{cite journal |arxiv=1111.1234|doi=10.1088/0004-637X/746/1/7|last1= Le Floc'h|first1= E.|title= The first Infrared study of the close environment of a long Gamma-Ray Burst|journal=The Astrophysical Journal|volume=746|issue=1|pages=7|last2= Charmandaris|first2= V.|last3= Gordon|first3= K.|last4= Forrest|first4= W. J.|last5= Brandl|first5= B.|last6= Schaerer|first6= D.|last7= Dessauges-Zavadsky|first7= M.|last8= Armus|first8= L.|s2cid=51474244|date= 2011|bibcode = 2012ApJ...746....7L }}</ref> GRB 980425 was far less energetic than the average GRB and was associated with the [[Type Ib and Ic supernovae|Type Ib supernova]] [[SN 1998bw]].<ref name="Kippen et al. (1998)">{{cite journal |last1=Kippen |first1=R.M. |title=On the Association of Gamma-Ray Bursts with Supernovae |journal=The Astrophysical Journal |date=October 1998 |volume=506 |issue=1 |pages=L27–L30 |doi=10.1086/311634 |last2=Briggs |first2=M. S. |last3=Kommers |first3=J. M. |last4=Kouveliotou |first4=C. |last5=Hurley |first5=K. |last6=Robinson |first6=C. R. |last7=Van Paradijs |first7=J. |last8=Hartmann |first8=D. H. |last9=Galama |first9=T. J. |last10=Vreeswijk |first10=P. M. |s2cid=2677824 |arxiv = astro-ph/9806364 |bibcode = 1998ApJ...506L..27K }}</ref>

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.<ref>{{cite web|url=https://www.bbc.co.uk/news/science-environment-21082617|title=Gamma-ray burst 'hit Earth in 8th Century'|work=BBC News|first=Rebecca |last=Morelle|author-link=Rebecca Morelle|date=2013-01-21|access-date=January 21, 2013}}</ref> 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.<ref>[[#Guetta|Guetta and Piran 2006]]</ref>

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.<ref>{{cite web | url=http://www.nbcnews.com/id/44823014 | archive-url=https://web.archive.org/web/20131122132000/http://www.nbcnews.com/id/44823014 | url-status=dead | archive-date=November 22, 2013 | title=Can gamma-ray bursts destroy life on Earth? | publisher=MSN | author=Welsh, Jennifer | date=2011-07-10 | access-date=October 27, 2011}}</ref> A GRB could potentially vaporize anything in its beams' paths within a range of around 200 light-years.<ref name=":0">{{Cite web |date=2003-09-17 |title=Gamma-ray bursts: are we safe? |url=https://www.esa.int/Science_Exploration/Space_Science/Space_for_you/Gamma-ray_bursts_are_we_safe |access-date=2023-09-17 |website=www.esa.int |language=en}}</ref><ref name=":1">{{Cite web |last=Lincoln |first=Don |author-link=Don Lincoln |date=2023-06-06 |title=Scientists are exploring how deadly gamma-ray bursts could sterilize — or vaporize — the Earth |url=https://bigthink.com/hard-science/gamma-ray-bursts-sterilize-vaporize-earth/ |access-date=2023-09-17 |website=Big Think |language=en-US}}</ref>

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.<ref>{{Cite web|url=https://science.nasa.gov/science-news/science-at-nasa/1998/ast29sep98_2/|title=Cosmic energy burst disturbs Earth's atmosphere|website=NASA Science|date=September 29, 1998|access-date=July 12, 2017|archive-date=January 24, 2023|archive-url=https://web.archive.org/web/20230124045705/https://science.nasa.gov/science-news/science-at-nasa/1998/ast29sep98_2/|url-status=dead}}</ref>

=== 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 kilo[[parsec]]s 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.<ref name=Threat>{{Cite journal |arxiv = 0903.4710|doi = 10.1017/S1473550409004509|title = Gamma-ray bursts as a threat to life on Earth|journal = International Journal of Astrobiology|volume = 8|issue = 3|pages = 183–186|year = 2009|last1 = Thomas|first1 = B.C.|s2cid = 118579150|bibcode = 2009IJAsB...8..183T}}</ref><ref name="Effects">{{Cite journal | doi=10.1007/s10509-009-0211-7| title=Effects of gamma ray bursts in Earth's biosphere| journal=Astrophysics and Space Science| volume=326| issue=1| pages=61–67| year=2010| last1=Martin| first1=Osmel| last2=Cardenas| first2=Rolando| last3=Guimarais| first3=Mayrene| last4=Peñate| first4=Liuba| last5=Horvath| first5=Jorge| last6=Galante| first6=Douglas| s2cid=15141366| bibcode=2010Ap&SS.326...61M| arxiv=0911.2196}}</ref>

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 layer|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.<ref name=Threat/><ref name="Effects"/>

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.<ref name=Threat/><ref name="Effects"/>

==== 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.<ref>{{Cite journal |last1=Piran |first1=Tsvi |last2=Jimenez |first2=Raul |date=2014-12-05 |title=Possible Role of Gamma Ray Bursts on Life Extinction in the Universe |url=https://link.aps.org/doi/10.1103/PhysRevLett.113.231102 |journal=Physical Review Letters |volume=113 |issue=23 |pages=231102 |doi=10.1103/PhysRevLett.113.231102|pmid=25526110 |arxiv=1409.2506 |bibcode=2014PhRvL.113w1102P |hdl=2445/133018 |s2cid=43491624 }}</ref><ref name="TerrestrialOzoneDepletion">{{cite journal |last1=Thomas |first1=Brian C. |last2=Jackman |first2=Charles H. |last3=Melott |first3=Adrian L. |last4=Laird |first4=Claude M. |last5=Stolarski |first5=Richard S. |last6=Gehrels |first6=Neil |last7=Cannizzo |first7=John K. |last8=Hogan |first8=Daniel P. |date=28 February 2005 |title=Terrestrial Ozone Depletion due to a Milky Way Gamma-Ray Burst |url=https://iopscience.iop.org/article/10.1086/429799/meta |journal=The Astrophysical Journal |volume=622 |issue=2 |pages=L153–L156 |doi=10.1086/429799 |arxiv=astro-ph/0411284 |bibcode=2005ApJ...622L.153T |hdl=2060/20050179464 |s2cid=11199820 |access-date=22 October 2022}}</ref>

The major [[Ordovician–Silurian extinction event]] 450 million years ago may have been caused by a GRB.<ref name="GeographicPatterns" /><ref name="GammaRayBurstsAndTheEarth">{{cite journal |last1=Thomas |first1=Brian C. |last2=Melott |first2=Adrian Lewis |last3=Jackman |first3=Charles H. |last4=Laird |first4=Claude M. |last5=Medvedev |first5=Mikhail V. |last6=Stolarski |first6=Richard S. |last7=Gehrels |first7=Neil |last8=Cannizzo |first8=John K. |last9=Hogan |first9=Daniel P. |last10=Ejzak |first10=Larissa M. |date=20 November 2005 |title=Gamma-Ray Bursts and the Earth: Exploration of Atmospheric, Biological, Climatic, and Biogeochemical Effects |url=https://iopscience.iop.org/article/10.1086/496914/meta |journal=[[The Astrophysical Journal]] |volume=634 |issue=1 |pages=509–533 |doi=10.1086/496914 |arxiv=astro-ph/0505472 |bibcode=2005ApJ...634..509T |s2cid=2046052 |access-date=22 October 2022}}</ref> 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.<ref name="renamed_from_2021_on_20231204051223">{{cite journal |last1=Rodríguez-López |first1=Lien |last2=Cardenas |first2=Rolando |last3=González-Rodríguez |first3=Lisdelys |last4=Guimarais |first4=Mayrene |last5=Horvath |first5=Jorge |date=24 January 2021 |title=Influence of a galactic gamma ray burst on ocean plankton |url=https://onlinelibrary.wiley.com/doi/abs/10.1002/asna.202113878 |journal=Astronomical Notes |volume=342 |issue=1–2 |pages=45–48 |doi=10.1002/asna.202113878 |arxiv=2011.08433 |bibcode=2021AN....342...45R |s2cid=226975864 |access-date=21 October 2022}}</ref> The [[late Ordovician]] species of [[trilobite]]s 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.<ref name="Melott2004" />

A case has been made that the [[774–775 carbon-14 spike]] was the result of a short GRB,<ref name="pavlov">{{cite journal | last1=Pavlov | first1=A.K. | last2=Blinov | first2=A.V. | last3=Konstantinov | first3=A.N. | s2cid=118638711 | display-authors=etal | title=AD 775 pulse of cosmogenic radionuclides production as imprint of a Galactic gamma-ray burst | journal=Mon. Not. R. Astron. Soc. | date=2013 | volume=435 | issue=4 | pages=2878–2884 | doi=10.1093/mnras/stt1468 | doi-access=free | arxiv=1308.1272 | bibcode=2013MNRAS.435.2878P}}</ref><ref name="hamb">{{cite journal | last1=Hambaryan | first1=V.V. | last2=Neuhauser | first2=R. | s2cid=765056 | date=2013 | title=A Galactic short gamma-ray burst as cause for the <sup>14</sup>C peak in AD 774/5 | journal=[[Monthly Notices of the Royal Astronomical Society]] | volume=430 | issue=1 | pages=32–36 | arxiv=1211.2584 | bibcode=2013MNRAS.430...32H | doi=10.1093/mnras/sts378| doi-access=free }}</ref> though a very strong [[solar flare]] is another possibility.<ref name="mek15">{{cite journal | date=2015 | author=Mekhaldi | display-authors=etal | journal =Nature Communications | volume=6 | pages=8611 | doi=10.1038/ncomms9611 | title=Multiradionuclide evidence for the solar origin of the cosmic-ray events of ᴀᴅ 774/5 and 993/4 |bibcode = 2015NatCo...6.8611M | pmid=26497389 | pmc=4639793}}</ref>

== GRB candidates in the Milky Way ==
[[File:Short_Gamma-Ray_Burst.jpg|thumb|Illustration of a short gamma-ray burst caused by a collapsing star.<ref>{{cite web|title=Illustration of a Short Gamma-Ray Burst Caused by a Collapsing Star|url=https://noirlab.edu/public/images/noirlab2121a/|date=July 26, 2021 |access-date=August 3, 2021}}</ref>]]
No gamma-ray bursts from within our own galaxy, the [[Milky Way Galaxy|Milky Way]], have been observed,<ref name="set to go supernova">{{cite web|url=https://cosmosmagazine.com/space/milky-way-star-set-to-go-supernova|title=Milky Way star set to go supernova|author=Lauren Fuge|publisher=Cosmos|date=20 November 2018|access-date=7 April 2019}}</ref> 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 variable]]s (LBVs) and rapidly spinning [[Wolf–Rayet star]]s 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 [[history of the universe|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.<ref>{{cite journal | pmid =  23630373 | doi=10.1098/rsta.2012.0237 | volume=371 | issue=1992 | title=Gamma-ray burst progenitors and the population of rotating Wolf-Rayet stars | journal=Philos Trans Royal Soc A | pages=20120237 | author=Vink JS|bibcode = 2013RSPTA.37120237V | year=2013 | doi-access=free }}</ref><ref>{{cite book|editor1=Mario Livio|editor2=Nino Panagia|editor3=Kailash Sahu|author1=Y-H. Chu|author2=C-H. Chen|author3=S-P. Lai|chapter=Superluminous supernova remnants|title=Supernovae and Gamma-Ray Bursts: The Greatest Explosions Since the Big Bang|chapter-url=https://books.google.com/books?id=VlfSviM9eIIC&pg=PA135|year=2001|publisher=Cambridge University Press|isbn=978-0-521-79141-0|page=135}}</ref><ref>{{cite journal |bibcode=2007Ap&SS.311..177V |arxiv=0704.0659 |title=Long gamma-ray burst progenitors: Boundary conditions and binary models |journal=Astrophysics and Space Science |volume=311 |issue=1–3 |pages=177–183 |last1=Van Den Heuvel |first1=E. P. J. |last2=Yoon |first2=S.-C. |s2cid=38670919 |year=2007 |doi=10.1007/s10509-007-9583-8}}</ref>

== See also ==
{{div col}}
* {{annotated link|BOOTES}}
* [[Fast blue optical transient]]
* [[Fast radio burst]]
* [[Gamma-ray burst precursor]]
* [[Search for extraterrestrial intelligence#Gamma-ray bursts|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]]
* {{annotated link|Relativistic jet}}
* {{annotated link|Soft gamma repeater}}
* [[Stellar evolution]] <!-- why or be more specific -->
* [[Terrestrial gamma-ray flashes]]
{{div col end}}

== Notes ==
<references group="nb" />

== Citations ==
{{Reflist}}

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{{Refend}}

== Further reading ==
* {{cite book
 |author1=Vedrenne, G. |author2=Atteia, J.-L.
 |date=2009
 |title=Gamma-Ray Bursts: The brightest explosions in the Universe
 |url=https://books.google.com/books?id=jZHSdrvzz0gC
 |publisher=[[Springer (publisher)|Springer]]
 |isbn=978-3-540-39085-5
}}
* {{cite book|title=Gamma-ray bursts|date=2012|publisher=Cambridge University Press|location=Cambridge|isbn=978-0-521-66209-3|editor1=Chryssa Kouveliotou |editor2=Stanford E. Woosley |editor3=Ralph A. M. J. }}
* {{cite book|title=The Physics of Gamma-Ray Bursts|date=2018|publisher=Cambridge University Press|location=Cambridge|isbn=9781139226530|author1= Bing Zhang}}

== External links ==
{{Sister project links|wikt=gamma-ray burst|commons=Category:Gamma ray bursts|b=General Astronomy/Introduction and Brief History of Gamma-Ray Bursts}}

;GRB mission sites
* [[Swift Gamma-Ray Burst Mission]]:
** [https://web.archive.org/web/20041014213023/http://swift.gsfc.nasa.gov/docs/swift/swiftsc.html Official NASA Swift Homepage]
** [http://www.swift.ac.uk/ UK Swift Science Data Centre]
** [http://www.swift.psu.edu/ Swift Mission Operations Center at Penn State]
* [http://space.mit.edu/HETE/ HETE-2: High Energy Transient Explorer] ([[High Energy Transient Explorer|Wiki entry]])
* [http://www.esa.int/science/integral INTEGRAL: INTErnational Gamma-Ray Astrophysics Laboratory] ([[INTEGRAL|Wiki entry]])
* [https://web.archive.org/web/20060715224642/http://www.batse.msfc.nasa.gov/batse/ BATSE: Burst and Transient Source Explorer]
* [http://fermi.gsfc.nasa.gov/ Fermi Gamma-ray Space Telescope] ([[Fermi Gamma-ray Space Telescope|Wiki entry]])
* [http://agile.rm.iasf.cnr.it/ AGILE: Astro-rivelatore Gamma a Immagini Leggero] ([[AGILE (satellite)|Wiki entry]])
* [http://exist.gsfc.nasa.gov/ EXIST: Energetic X-ray Survey Telescope] {{Webarchive|url=https://web.archive.org/web/20090404102921/http://exist.gsfc.nasa.gov/ |date=2009-04-04 }}
* [https://heasarc.gsfc.nasa.gov/grbcat/ Gamma Ray Burst Catalog at NASA]

;GRB follow-up programs
* [http://gcn.gsfc.nasa.gov/ The Gamma-ray bursts Coordinates Network (GCN)] ([[Gamma-ray Burst Coordinates Network|Wiki entry]])
* [http://bootes.iaa.es/ BOOTES: Burst Observer and Optical Transient Exploring System] {{Webarchive|url=https://web.archive.org/web/20130423131326/http://bootes.iaa.es/ |date=2013-04-23 }} ([[BOOTES|Wiki entry]])
* [http://www.mpe.mpg.de/~jcg/GROND/ GROND: Gamma-Ray Burst Optical Near-infrared Detector] ([[Gamma-Ray Burst Optical/Near-Infrared Detector|Wiki entry]])
* [https://web.archive.org/web/20080917153503/http://astro.berkeley.edu/~bait/kait.html KAIT: The Katzman Automatic Imaging Telescope] ([[Katzman Automatic Imaging Telescope|Wiki entry]])
* [http://observ.pereplet.ru/ MASTER: Mobile Astronomical System of the Telescope-Robots]
* [http://www.umich.edu/~rotse/ ROTSE: Robotic Optical Transient Search Experiment] ([[Robotic Optical Transient Search Experiment|Wiki entry]])

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