PHYS 1010 Chapter Notes - Chapter 12: Helium Flash, Main Sequence, The Sequence
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23 Apr 2016
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During the stay on the main sequence, any fluctuations in a star"s condition are quickly restored, the star is in equilibrium. The sun will expand till the forces are once again balanced, expand, decrease temperature and contract. Eventually as hydrogen in the core is consumed, the star begins to leave the main sequence. Its evolution from then on depends very much on the mass of the start. High mass stars go out with a bang! (high mass= more than 8 solar masses) Stages of a star leaving the main sequence (table in the book) Over 90% of the star"s life is spent on the 7th stage. Even while on the main sequence, the composition of a star"s core is changing. When there is a significant amount of helium, it dies! The core hydrogen has been largely deleted and we get a core of helium forming. The temperature is not enough for helium fusion.
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