highmassstars.pdf - The Evolution of High-mass Stars core...

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The Evolution of High-mass Stars
coretemperatureIf the core’s mass is <1.4 M(entire star’s mass is <8 M), gravity isn’tstrong enough to compress it further, so the collapse is halted. Thisresistance to compression is calledelectron degeneracy.C/O
coretemperatureIf the core’s mass is >1.4 M(entire star’s mass is >8 M), gravity isstrong enough to continue compressing it, and the collapse continues.C/O
coretemperatureC/OIf the core’s mass is >1.4 M(entire star’s mass is >8 M), gravity isstrong enough to continue compressing it, and the collapse continues.
coretemperatureC/OIf the core’s mass is >1.4 M(entire star’s mass is >8 M), gravity isstrong enough to continue compressing it, and the collapse continues.
Eventually, the core contracts enoughthat it is hot enough for carbon andoxygen fusion, which produces silicon.The energy produced by carbonand oxygen fusion halts thecore’s collapse.coretemperature0.5-2 billion KC/Ofusion
Carbon and oxygen fusion ends when theseelements are fully transformed into silicon.Si
Now that the energy fromfusion is gone, the coreresumes its collapse.coretemperatureSi
Now that the energy fromfusion is gone, the coreresumes its collapse.coretemperatureSi
Now that the energy fromfusion is gone, the coreresumes its collapse.coretemperatureSi
Now that the energy fromfusion is gone, the coreresumes its collapse.coretemperatureSi
Eventually, the core contractsenough that it is hot enough forsilicon fusion, which produces iron.

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Term
Spring
Professor
MILLER,DAVIDEMAN
Tags
Supernova, Neutron star

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