Editing Supernova (section)

===Role in stellar evolution===
{{Main|Supernova remnant}}
Remnants of many supernovae consist of a compact object and a rapidly expanding shock wave of material. This cloud of material sweeps up surrounding [[interstellar medium]] during a free expansion phase, which can last for up to two centuries. The wave then gradually undergoes a period of [[adiabatic process|adiabatic expansion]], and will slowly cool and mix with the surrounding interstellar medium over a period of about 10,000 years.<ref>
{{cite journal
 |last1=Cox |first1=D. P.
 |year=1972
 |title=Cooling and Evolution of a Supernova Remnant
 |journal=Astrophysical Journal
 |volume=178 |pages=159
 |bibcode=1972ApJ...178..159C
 |doi=10.1086/151775
|doi-access=free
 }}</ref>

[[Image:STScl-2005-15.png|thumb|upright=1.2|Supernova remnant N 63A lies within a clumpy region of gas and dust in the [[Large Magellanic Cloud]].]]
The [[Big Bang]] produced hydrogen, [[helium]] and traces of [[lithium]], while all heavier elements are synthesised in stars, supernovae, and collisions between neutron stars (thus being indirectly due to supernovae). Supernovae tend to enrich the surrounding interstellar medium with elements other than hydrogen and helium, which usually astronomers refer to as "metals".<ref name="Johnson2019">{{Cite journal |last=Johnson |first=Jennifer A. |date=February 2019 |title=Populating the periodic table: Nucleosynthesis of the elements |journal=Science |language=en |volume=363 |issue=6426 |pages=474–478 |doi=10.1126/science.aau9540 |pmid=30705182 |bibcode=2019Sci...363..474J |s2cid=59565697 |issn=0036-8075|doi-access=free }}</ref> These ejected elements ultimately enrich the [[molecular cloud]]s that are the sites of star formation.<ref>
{{cite journal
 |last1=Sandstrom |first1=K. M.
 |last2=Bolatto |first2=A. D.
 |last3=Stanimirović |first3=S. | author3-link=Snežana Stanimirović
 |last4=Van Loon |first4=J. Th.
 |last5=Smith |first5=J. D. T.
 |year=2009
 |title=Measuring Dust Production in the Small Magellanic Cloud Core-Collapse Supernova Remnant 1E 0102.2–7219
 |journal=The Astrophysical Journal
 |volume=696 |issue=2 |pages=2138–2154
 |arxiv=0810.2803
 |bibcode=2009ApJ...696.2138S
 |doi=10.1088/0004-637X/696/2/2138
|s2cid=8703787
 }}</ref> Thus, each stellar generation has a slightly different composition, going from an almost pure mixture of hydrogen and helium to a more metal-rich composition. Supernovae are the dominant mechanism for distributing these heavier elements, which are formed in a star during its period of nuclear fusion. The different abundances of elements in the material that forms a star have important influences on the star's life,<ref name="Johnson2019"/><ref>{{Cite journal |last1=Salaris |first1=Maurizio |last2=Cassisi |first2=Santi |date=August 2017 |title=Chemical element transport in stellar evolution models |doi-access=free |journal=Royal Society Open Science |language=en |volume=4 |issue=8 |pages=170192 |doi=10.1098/rsos.170192 |pmid=28878972 |pmc=5579087 |bibcode=2017RSOS....470192S |arxiv=1707.07454 |issn=2054-5703}}</ref> and may influence the possibility of having [[planet]]s orbiting it: more [[giant planet]]s form around stars of higher metallicity.<ref>{{cite journal|last1=Fischer |first1=Debra A. |last2=Valenti |first2=Jeff |title=The planet-metallicity correlation |journal=The Astrophysical Journal |bibcode=2005ApJ...622.1102F |doi=10.1086/428383 |volume=622 |year=2005 |issue=2 |pages=1102–1117|s2cid=121872365 |doi-access=free }}</ref><ref>{{cite journal|doi=10.1146/annurev-astro-112420-020055 |bibcode=2021ARA&A..59..291Z |arxiv=2103.02127 |title=Exoplanet Statistics and Theoretical Implications |journal=Annual Review of Astronomy and Astrophysics |volume=59 |year=2021 |last1=Zhu |first1=Wei |last2=Dong |first2=Subo |pages=291–336|s2cid=232105177 }}</ref>

The kinetic energy of an expanding supernova remnant can trigger star formation by compressing nearby, dense molecular clouds in space.<ref>
{{cite journal
 |last1=Preibisch |first1=T. 
 |last2=Zinnecker |first2=H. 
 |year=2001
 |title=Triggered Star Formation in the Scorpius-Centaurus OB Association (Sco OB2) 
 |journal=From Darkness to Light: Origin and Evolution of Young Stellar Clusters 
 |volume=243 |pages=791 
 |arxiv=astro-ph/0008013
 |bibcode=2001ASPC..243..791P
}}</ref> The increase in turbulent pressure can also prevent star formation if the cloud is unable to lose the excess energy.<ref name="aaa128">
{{cite journal
 |last1=Krebs |first1=J.
 |last2=Hillebrandt |first2=W.
 |year=1983
 |title=The interaction of supernova shockfronts and nearby interstellar clouds
 |journal=Astronomy and Astrophysics
 |volume=128 |issue=2 |pages=411
 |bibcode=1983A&A...128..411K
}}</ref>

Evidence from daughter products of short-lived [[radioactive isotope]]s shows that a nearby supernova helped determine the composition of the [[Solar System]] 4.5&nbsp;billion years ago, and may even have triggered the formation of this system.<ref>
{{cite journal
 |last1=Cameron |first1=A.G.W.
 |last2=Truran |first2=J.W.
 |year=1977
 |title=The supernova trigger for formation of the solar system
 |journal=Icarus
 |volume=30 |issue=3 |pages=447
 |bibcode=1977Icar...30..447C
 |doi=10.1016/0019-1035(77)90101-4
}}</ref>

[[Fast radio burst]]s (FRBs) are intense, transient pulses of radio waves that typically last no more than milliseconds. Many explanations for these events have been proposed; [[magnetar]]s produced by core-collapse supernovae are leading candidates.<ref name="AJL-20200601">{{cite journal |author=Bhandan, Shivani |date=1 June 2020 |title=The Host Galaxies and Progenitors of Fast Radio Bursts Localised with the Australian Square Kilometre Array Pathfinder |journal=[[The Astrophysical Journal Letters]] |volume=895 |pages=L37 |arxiv=2005.13160 |bibcode=2020ApJ...895L..37B |doi=10.3847/2041-8213/ab672e |s2cid=218900539 |number=2 |doi-access=free }}</ref><ref>{{Cite journal |last=Zhang |first=Bing |date=2020-11-05 |title=The physical mechanisms of fast radio bursts |url=https://www.nature.com/articles/s41586-020-2828-1 |journal=Nature |language=en |volume=587 |issue=7832 |pages=45–53 |doi=10.1038/s41586-020-2828-1 |pmid=33149290 |arxiv=2011.03500 |bibcode=2020Natur.587...45Z |s2cid=226259246 |issn=0028-0836}}</ref><ref>{{Cite web |last=Chu |first=Jennifer |date=2022-07-13 |title=Astronomers detect a radio "heartbeat" billions of light-years from Earth |url=https://news.mit.edu/2022/astronomers-detect-radio-heartbeat-billions-light-years-earth-0713 |access-date=2023-03-19 |website=MIT News |publisher=[[Massachusetts Institute of Technology]] |language=en}}</ref><ref>{{Cite journal |last1=Petroff |first1=E. |last2=Hessels |first2=J. W. T. |last3=Lorimer |first3=D. R. |date=2022-03-29 |title=Fast radio bursts at the dawn of the 2020s |url=https://doi.org/10.1007/s00159-022-00139-w |journal=The Astronomy and Astrophysics Review |language=en |volume=30 |issue=1 |pages=2 |doi=10.1007/s00159-022-00139-w |arxiv=2107.10113 |bibcode=2022A&ARv..30....2P |s2cid=253690001 |issn=1432-0754}}</ref>