lec26 - Lecture 26 Evolution of Stars: Giants Lecture 26...

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Lecture 26 Evolution of Stars: Giants Purdue University, Astronomy 364 1 Lecture 26
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End of MS: Solar-Mass Stars • The main sequence phase ends with the depletion of hydrogen in the core. – Isothermal He core – hydrogen burning continues in a shell around the He core. Lecture 26 2 Purdue University, Astronomy 364
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Solar-Mass Stars • The H-shell burning phase produces even more energy than the core-burning phase – R and L increase, but T decreases – This is the subgiant branch Lecture 26 3 Purdue University, Astronomy 364
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Degenerate Cores When the density of a gas gets sufficiently high, the Pauli exclusion principle applies: no two fermions (e.g. electrons) can occupy the same quantum state. – Pressure becomes due to the zero-point motion of electrons, and is independent of temperature P ∝ ρ 5/3 A solar mass star’s core will collapse when it reaches ~13% of the total stellar mass. Lower mass stars have more degenerate cores: thus the
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lec26 - Lecture 26 Evolution of Stars: Giants Lecture 26...

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