11:3:09 Life of Stars

11:3:09 Life of Stars - 08:45:00 o...

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03/11/2009 08:45:00 What about high mass stars? Early stages are similar to those of low mass stars o Main Sequence: H fuses to He in core o Red Supergiant: H fuses to He in shell around He core o Helium Core Burning: He fuses to C in core But it doesn’t stop there… Advanced nuclear fusion reactions require extremely high temperatures and  densities Only high mass stars can attain high enough core temperatures before  degeneracy pressure stops contraction Need more massive star to have enough gravitational pressure  Supernova Supernova explosion releases huge amount of energy o -> heating -> lots of photons Luminosity in photons can be similar to that of whole galaxy full of stars Stellar Graveyard Low mass stars – end up as White Dwarfs o White dwarfs are the remaining cores of dead low-mass stars o Electron degeneracy pressure supports them against gravity
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This note was uploaded on 10/17/2011 for the course ISP 205 taught by Professor Donahue during the Fall '08 term at Michigan State University.

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11:3:09 Life of Stars - 08:45:00 o...

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