Evolution of High Mass Stars

Evolution of High Mass Stars - Evolution of High Mass Stars...

Info iconThis preview shows pages 1–2. Sign up to view the full content.

View Full Document Right Arrow Icon
Evolution of High Mass Stars (>8 Msun) Similar to that of low mass stars o Hydrogen core fusion (main sequence) o Hydrogen shell burning (supergiant) o Helium core fusion (supergiant) But higher core pressures and temperatures means conditions acceptable for fusion of even higher elements past He Advanced Nuclear Burning o Cores of higher mass stars o Temperature of contracting core in stars with more than 8 times the mass of the sun allow fusion of elements all the way up to iron o Advanced nuclear burning proceeds in a series of nested shells “onion skin model” H core fusion: 10^6 years He core fusion: 10^5 Si core fusion: days o Iron is dead end for fusion because nuclear reactions involving iron do not release energy o Iron has lowest mass per nuclear particle, so anything that iron fuses to has more mass than the iron nucleus; similarly anything that iron splits into has more mass than the original iron nucleus o Now what? Inert iron core forms and collapses, the star explodes and
Background image of page 1

Info iconThis preview has intentionally blurred sections. Sign up to view the full version.

View Full DocumentRight Arrow Icon
Image of page 2
This is the end of the preview. Sign up to access the rest of the document.

Page1 / 2

Evolution of High Mass Stars - Evolution of High Mass Stars...

This preview shows document pages 1 - 2. Sign up to view the full document.

View Full Document Right Arrow Icon
Ask a homework question - tutors are online