Supernòva : Diferéncia entre versions

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Les supernòvas dònan luòc a d'emissions de radiacions electromagneticas intensas que pòdon durar maites meses. Se caracterizan per una rapida aumentacion d'intensitat fins a aténher un pic, e aprés descreisson en luminositat d'un biais mai o mens suau fins a desaparéisser completament.
L'explosion de [[radiacion]]s extemament luminosa, embandís fòrça material estellar a una velocitat de mai de 30000km/s (10% de la [[velocitat de la lutz]]), en provocar una [[onda de tust]]<ref>
{{Cite journal
|last1=Schawinski |first1=Kevin
|last2=Justham |first2=Stephen
|last3=Wolf |first3=Christian
|last4=Podsiadlowski |first4=Philipp
|last5=Sullivan |first5=Mark
|last6=Steenbrugge |first6=Katrien<!-- sic --> C.
|last7=Bell |first7=Tony
|last8=Röser |first8=Hermann-Josef
|last9=Walker |first9=Emma S.
|last10=Astier |first10=Pierre
|last11=Balam |first11=David
|last12=Balland |first12=Christophe
|last13=Carlberg |first13=Raymond G.
|last14=Conley |first14=Alexander J.
|last15=Fouchez |first15=Dominique<!-- typo in arxiv -->
|last16=Guy |first16=Julien
|last17=Hardin |first17=Delphine
|last18=Hook |first18=Isobel M.
|last19=Howell |first19=D. Andrew
|last20=Pain |first20=Reynald
|last21=Perrett |first21=Kathryn M.
|last22=Pritchet |first22=Christopher J.
|last23=Regnault |first23=Nicolas
|last24=Yi |first24=Sukyoung K.
|display-authors=1
|year=2008
|title=Supernova Shock Breakout from a Red Supergiant
|journal=[[Science (journal)|Science]]
|volume=321 |issue=5886 |pages=223–226
|arxiv=0803.3596
|bibcode=2008Sci...321..223S
|doi=10.1126/science.1160456
|pmid=18556514
}}</ref> dins lo mitan interstellar a l'entorn. This shock wave sweeps up an expanding shell of gas and dust called a [[supernova remnant]]. Supernovae are potentially strong galactic sources of [[gravitational wave]]s.<ref>
{{Cite journal
|last1=Ott |first1=Christian D.
|last2=O'Connor |first2=Evan P.
|last3=Gossan |first3=Sarah E.
|last4=Abdikamalov |first4=Ernazar
|last5=Gamma |first5=Uschi C. T.
|last6=Drasco |first6=Steve
|display-authors=1
|year=2012
|title=Core-Collapse Supernovae, Neutrinos, and Gravitational Waves
|journal=[[Nuclear Physics B: Proceedings Supplement]]
|volume=235 |pages=381
|arxiv=1212.4250
|bibcode=2013NuPhS.235..381O
|doi=10.1016/j.nuclphysbps.2013.04.036
}}</ref> A great proportion of primary cosmic rays comes from supernovae.<ref name="ackermann-2013">
{{cite journal
|last1=Ackermann |first1=M.
|last2=Ajello |first2=M.
|last3=Allafort |first3=A.
|last4=Baldini |first4=L.
|last5=Ballet |first5=J.
|last6=Barbiellini |first6=G.
|last7=Baring |first7=M. G.
|last8=Bastieri |first8=D.
|last9=Bechtol |first9=K.
|last10=Bellazzini |first10=R.
|last11=Blandford |first11=R. D.
|last12=Bloom |first12=E. D.
|last13=Bonamente |first13=E
|last14=Borgland |first14=A. W.
|last15=Bottacini |first15=E.
|last16=Brandt |first16=T. J.
|last17=Bregeon |first17=J.
|last18=Brigida |first18=M.
|last19=Bruel |first19=P.
|last20=Buehler |first20=R.
|last21=Busetto |first21=G.
|last22=Buson |first22=S.
|last23=Caliandro |first23=G. A.
|last24=Cameron |first24=R. A.
|last25=Caraveo |first25=P. A.
|last26=Casandjian |first26=J. M.
|last27=Cecchi |first27=C.
|last28=Celik |first28=O.
|last29=Charles |first29=E.
|last30=Chaty |first30=S.
|display-authors=1
|title=Detection of the Characteristic Pion-Decay Signature in Supernova Remnants
|journal=[[Science (journal)|Science]]
|volume=339 |issue=6121 |pages=807–11
|year=2013
|arxiv=1302.3307
|bibcode=2013Sci...339..807A
|doi=10.1126/science.1231160
|pmid=23413352
}}</ref>
 
==Referéncias==
<references />
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