ASTR 1000 Lecture Notes - Lecture 16: Escape Velocity, Hypernova, Schwarzschild Radius
16 Mar 2017
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Document Summary
Start as high mass stars until he core burning. Reach supergiant stage, but gravity cannot hold on to the atmosphere. Get a large planetary nebula which carries off 75-90% of the star"s mass. Not enough mass left to fuse carbon -> turns into a white dwarf. If a star is in a binary system, the companion star can change how the star evolves. The more massive star with run out of h(ydrogen) first and become a giant star. If the companion is close enough, the companion star can steal the atmosphere of the giant star, reducing its mass. The loss of mass by the larger star can make it stop fusing heavier elements before it normally would if isolated. The companion star gains mass, causing it to change spectral type and shortens its lifetime on the main sequence. Is supported by electron degeneracy pressure, and is composed of elements heavier than hydrogen.
