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Witdwerg: Verskil tussen weergawes

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’n '''Witdwerg''' is ’n klein [[ster]] wat vorm nadat ’n [[hoofreeks]]ster met ’n gemiddelde massa die einde van sy leeftyd bereik het. Hulle is baie dig: hul massa is vergelykbaar met dié van die [[Son]] en hul grootte met dié van die [[Aarde]]. Hul dowwe lig kom van die uitstraling van gebergte termiese energie.<ref name="osln">{{cite web |last=Johnson |first=J. |year=2007 |url=http://www.astronomy.ohio-state.edu/~jaj/Ast162/lectures/notesWL22.html |title=Extreme Stars: White Dwarfs & Neutron Stars |work=Aantekeninge, Astronomie 162 |publisher=Ohio-staatsuniversiteit |access-date=17 Oktober 2011 |language=en |archive-url=https://web.archive.org/web/20191115223455/http://www.astronomy.ohio-state.edu:80/~jaj/Ast162/lectures/notesWL22.html |archive-date=15 November 2019 |url-status=live|df=dmy-all}}</ref><ref name="rln">{{cite web |last1=Richmond |first=M. |title=Late stages of evolution for low-mass stars |url=http://spiff.rit.edu/classes/phys230/lectures/planneb/planneb.html |work=Aantekeninge, Fisika 230 |publisher=Rochester-instituut vir Tegnologie |access-date=3 Mei 2007 |language=en |archive-url=https://web.archive.org/web/20200611225040/http://spiff.rit.edu/classes/phys230/lectures/planneb/planneb.html |archive-date=11 Junie 2020 |url-status=live|df=dmy-all}}</ref> Dit sal die laaste fase van [[evolusie]] wees van meer as 97% van die sterre in die [[Melkweg]].<ref name="cosmochronology">{{cite journal
|last=Johnson |first=J.
|year=2007
|url=http://www.astronomy.ohio-state.edu/~jaj/Ast162/lectures/notesWL22.html
|title=Extreme Stars: White Dwarfs & Neutron Stars
|work=Aantekeninge, Astronomie 162
|publisher=Ohio-staatsuniversiteit
|accessdate=17 Oktober 2011
}}</ref><ref name="rln">{{cite web
|last1=Richmond |first=M.
|title=Late stages of evolution for low-mass stars
|url=http://spiff.rit.edu/classes/phys230/lectures/planneb/planneb.html
|work=Aantekeninge, Fisika 230
|publisher=Rochester-instituut vir Tegnologie
|accessdate=3 Mei 2007
}}</ref> Dit sal die laaste fase van [[evolusie]] wees van meer as 97% van die sterre in die [[Melkweg]].<ref name="cosmochronology">{{cite journal
|last1=Fontaine |first1=G.
|last2=Brassard |first2=P.
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}}</ref>
 
Die naaste bekende witdwerg aan die Aarde is [[Sirius|Sirius B]], 8,6 [[ligjare]] van hier. Dit is die kleinste komponent van die Sirius-[[dubbelster]]. In Januarie 2009 is agt witdwerge getel in die honderd sterstelsels naaste aan die son.<ref>{{cite web |last1=Henry |first1=T. J. |date=1 Januarie 2009 |title=The One Hundred Nearest Star Systems |url=http://www.chara.gsu.edu/RECONS/TOP100.posted.htm |publisher=Research Consortium On Nearby Stars |access-date=21 Julie 2010 |language=en |archive-url=https://web.archive.org/web/20130329140328/http://www.chara.gsu.edu/RECONS/TOP100.posted.htm |archive-date=29 Maart 2013 |url-status=dead|df=dmy-all}}</ref> Die term is in 1922 deur Willem Luyten bekend gestel.<ref name="holberg">{{cite journal
|last1=Henry |first1=T. J.
|date=1 Januarie 2009
|title=The One Hundred Nearest Star Systems
|url=http://www.chara.gsu.edu/RECONS/TOP100.posted.htm
|publisher=Research Consortium On Nearby Stars
|accessdate=21 Julie 2010
}}</ref> Die term is in 1922 deur Willem Luyten bekend gestel.<ref name="holberg">{{cite journal
|bibcode=2005AAS...20720501H
|title=How Degenerate Stars Came to be Known as White Dwarfs
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