Magnetar

==Bright supernovae==

==Bright supernovae==

Unusually bright supernovae are thought to result from the death of very large stars as [[pair-instability supernova]]e (or pulsational pair-instability supernovae). However, recent research by astronomers{{cite journal|last=Kasen|first=D.|author2=L. Bildsten.|title=Supernova Light Curves Powered by Young Magnetars|journal=Astrophysical Journal|date=1 Jul 2010|volume=717|issue=1|pages=245–249|doi=10.1088/0004-637X/717/1/245|arxiv = 0911.0680 |bibcode = 2010ApJ...717..245K |s2cid=118630165}}{{cite journal|last=Woosley|first=S.|title=Bright Supernovae From Magnetar Birth|journal=Astrophysical Journal Letters|date=20 Aug 2010|volume=719|issue=2|pages=L204–L207|doi=10.1088/2041-8205/719/2/L204|arxiv = 0911.0698 |bibcode = 2010ApJ...719L.204W |s2cid=118564100}} has postulated that energy released from newly formed magnetars into the surrounding supernova remnants may be responsible for some of the brightest supernovae, such as SN 2005ap and SN 2008es.{{cite journal |title=Super Luminous Ic Supernovae: catching a magnetar by the tail |journal=The Astrophysical Journal |date=June 2013 |volume=770 |issue=2 |pages=128 |doi=10.1088/0004-637X/770/2/128 |arxiv=1304.3320 |bibcode=2013ApJ...770..128I |last1=Inserra |first1=C. |last2=Smartt |first2=S. J. |last3=Jerkstrand |first3=A. |last4=Valenti |first4=S. |last5=Fraser |first5=M. |last6=Wright |first6=D. |last7=Smith |first7=K. |last8=Chen |first8=T.-W. |last9=Kotak |first9=R. |last10=Pastorello |first10=A. |last11=Nicholl |first11=M. |last12=Bresolin |first12=F. |last13=Kudritzki |first13=R. P. |last14=Benetti |first14=S. |last15=Botticella |first15=M. T. |last16=Burgett |first16=W. S. |last17=Chambers |first17=K. C. |last18=Ergon |first18=M. |last19=Flewelling |first19=H. |last20=Fynbo |first20=J. P. U. |last21=Geier |first21=S. |last22=Hodapp |first22=K. W. |last23=Howell |first23=D. A. |last24=Huber |first24=M. |last25=Kaiser |first25=N. |last26=Leloudas |first26=G. |last27=Magill |first27=L. |last28=Magnier |first28=E. A. |last29=McCrum |first29=M. G. |last30=Metcalfe |first30=N. |s2cid=13122542 |display-authors=9}}{{cite web|last=Queen's University, Belfast|author-link=Queen's University, Belfast|title=New light on star death: Super-luminous supernovae may be powered by magnetars|url=https://www.sciencedaily.com/releases/2013/10/131016132155.htm|website=[[ScienceDaily]]|access-date=21 October 2013|date=16 October 2013}}{{cite journal

Unusually bright supernovae are thought to result from the death of very large stars as [[pair-instability supernova]]e (or pulsational pair-instability supernovae). However, recent research by astronomers{{cite journal|last=Kasen|first=D.|author2=L. Bildsten.|title=Supernova Light Curves Powered by Young Magnetars|journal=Astrophysical Journal|date=1 Jul 2010|volume=717|issue=1|pages=245–249|doi=10.1088/0004-637X/717/1/245|arxiv = 0911.0680 |bibcode = 2010ApJ...717..245K |s2cid=118630165}}{{cite journal|last=Woosley|first=S.|title=Bright Supernovae From Magnetar Birth|journal=Astrophysical Journal Letters|date=20 Aug 2010|volume=719|issue=2|pages=L204–L207|doi=10.1088/2041-8205/719/2/L204|arxiv = 0911.0698 |bibcode = 2010ApJ...719L.204W |s2cid=118564100}} has postulated that energy released from newly formed magnetars into the surrounding supernova remnants may be responsible for some of the brightest supernovae, such as SN 2005ap and SN 2008es.{{cite journal |title=Super Luminous Ic Supernovae: catching a magnetar by the tail |journal=The Astrophysical Journal |date=June 2013 |volume=770 |issue=2 |pages=128 |doi=10.1088/0004-637X/770/2/128 |arxiv=1304.3320 |bibcode=2013ApJ...770..128I |last1=Inserra |first1=C. |last2=Smartt |first2=S. J. |last3=Jerkstrand |first3=A. |last4=Valenti |first4=S. |last5=Fraser |first5=M. |last6=Wright |first6=D. |last7=Smith |first7=K. |last8=Chen |first8=T.-W. |last9=Kotak |first9=R. |last10=Pastorello |first10=A. |last11=Nicholl |first11=M. |last12=Bresolin |first12=F. |last13=Kudritzki |first13=R. P. |last14=Benetti |first14=S. |last15=Botticella |first15=M. T. |last16=Burgett |first16=W. S. |last17=Chambers |first17=K. C. |last18=Ergon |first18=M. |last19=Flewelling |first19=H. |last20=Fynbo |first20=J. P. U. |last21=Geier |first21=S. |last22=Hodapp |first22=K. W. |last23=Howell |first23=D. A. |last24=Huber |first24=M. |last25=Kaiser |first25=N. |last26=Leloudas |first26=G. |last27=Magill |first27=L. |last28=Magnier |first28=E. A. |last29=McCrum |first29=M. G. |last30=Metcalfe |first30=N. |s2cid=13122542 |display-authors=9}}{{cite web|last=Queen's University, Belfast|author-link=Queen's University, Belfast|title=New light on star death: Super-luminous supernovae may be powered by magnetars|url=https://www.sciencedaily.com/releases/2013/10/131016132155.htm|website=[[ScienceDaily]]|access-date=21 October 2013|date=16 October 2013}}{{cite journal

|author1=M. Nicholl |author2=S. J. Smartt |author3=A. Jerkstrand |author4=C. Inserra |author5=M. McCrum |author6=R. Kotak |author7=M. Fraser |author8=D. Wright |author9=T.-W. Chen |author10=K. Smith |author11=D. R. Young |author12=S. A. Sim |author13=S. Valenti |author14=D. A. Howell |author15=F. Bresolin |author16=R. P. Kudritzki |author17=J. L. Tonry |author18=M. E. Huber |author19=A. Rest |author20=A. Pastorello |author21=L. Tomasella |author22=E. Cappellaro |author23=S. Benetti |author24=S. Mattila |author25=E. Kankare |author26=T. Kangas |author27=G. Leloudas |author28=J. Sollerman |author29=F. Taddia |author30=E. Berger |author31=R. Chornock |author32=G. Narayan |author33=C. W. Stubbs |author34=R. J. Foley |author35=R. Lunnan |author36=A. Soderberg |author36-link= Alicia M. Soderberg |author37=N. Sanders |author38=D. Milisavljevic |author39=R. Margutti |author40=R. P. Kirshner |author41=N. Elias-Rosa |author42=A. Morales-Garoffolo |author43=S. Taubenberger |author44=M. T. Botticella |author45=S. Gezari |author46=Y. Urata |author47=S. Rodney |author48=A. G. Riess |author49=D. Scolnic |author49-link=Daniel M. Scolnic|author50=W. M. Wood-Vasey |author51=W. S. Burgett |author52=K. Chambers |author53=H. A. Flewelling |author54=E. A. Magnier |author55=N. Kaiser |author56=N. Metcalfe |author57=J. Morgan |author58=P. A. Price |author59=W. Sweeney |author60=C. Waters. |title=Slowly fading super-luminous supernovae that are not pair-instability explosions|journal=Nature|date=17 Oct 2013|volume=502|series=7471|issue=346|pages=346–9|doi=10.1038/nature12569|arxiv = 1310.4446 |bibcode = 2013Natur.502..346N|pmid=24132291|s2cid=4472977 }}

|author1=M. Nicholl |author2=S. J. Smartt |author3=A. Jerkstrand |author4=C. Inserra |author5=M. McCrum |author6=R. Kotak |author7=M. Fraser |author8=D. Wright |author9=T.-W. Chen |author10=K. Smith |author11=D. R. Young |author12=S. A. Sim |author13=S. Valenti |author14=D. A. Howell |author15=F. Bresolin |author16=R. P. Kudritzki |author17=J. L. Tonry |author18=M. E. Huber |author19=A. Rest |author20=A. Pastorello |author21=L. Tomasella |author22=E. Cappellaro |author23=S. Benetti |author24=S. Mattila |author25=E. Kankare |author26=T. Kangas |author27=G. Leloudas |author28=J. Sollerman |author29=F. Taddia |author30=E. Berger |author31=R. Chornock |author32=G. Narayan |author33=C. W. Stubbs |author34=R. J. Foley |author35=R. Lunnan |author36=A. Soderberg |author36-link= Alicia M. Soderberg |author37=N. Sanders |author38=D. Milisavljevic |author39=R. Margutti|author39-link=Raffaella Margutti |author40=R. P. Kirshner |author41=N. Elias-Rosa |author42=A. Morales-Garoffolo |author43=S. Taubenberger |author44=M. T. Botticella |author45=S. Gezari |author46=Y. Urata |author47=S. Rodney |author48=A. G. Riess |author49=D. Scolnic |author49-link=Daniel M. Scolnic|author50=W. M. Wood-Vasey |author51=W. S. Burgett |author52=K. Chambers |author53=H. A. Flewelling |author54=E. A. Magnier |author55=N. Kaiser |author56=N. Metcalfe |author57=J. Morgan |author58=P. A. Price |author59=W. Sweeney |author60=C. Waters. |title=Slowly fading super-luminous supernovae that are not pair-instability explosions|journal=Nature|date=17 Oct 2013|volume=502|series=7471|issue=346|pages=346–9|doi=10.1038/nature12569|arxiv = 1310.4446 |bibcode = 2013Natur.502..346N|pmid=24132291|s2cid=4472977 }}

==References==

==References==