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Astronomy - Session 11

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Parandis Khavari

Astronomy - Session 11  life of a star after the main sequence stage  after core depleted of Hydrogen  100% Helium  Hydrogen stops fusion  no energy  more pressure  gravity contracts core  temperature rises  gravitational contractions  a thin shell burns  is added to the (mass of) the core  Helium core (and Hydrogen shell burning)  energy from burning shell  gravitational energy  temperature rises to 100,000,000K  Helium fuses into Carbon and Oxygen  Helium core  red giant  yellow giant  burning of Helium  enough energy to stop gravitational contraction  same as Horizontal Branch stars  once the core is depleted of Helium  star begins to contract  soon, a burning shell will form immediately around the core  the upper Hydrogen shell burning deposits Helium in a layer between the two shells  the star cools and expands  becomes a giant again  it moves along an evolutionary track called the Asymptotic Giant Branch  (AGB) Asymptotic Giant Branch    (I) red giant  Hydrogen shell burning  expands and cools down  (II) horizontal branch (yellow giant)  Helium in core is fused  Hydrogen shell burning  dormant core of Helium  contraction and heats up  (III) Asymptotic Giant Branch (AGB)  dormant Carbon and Oxygen core  Helium and Hydrogen shell burning  expanding and cooling down  Asymptotic Giant Branch (AGB)  very bright  solar wind envelopes AGB in dust  dust covers AGB  dust absorbs photons  makes light (look) infrared  the core is inert in the case of AGB stars  1. What is the consequence of this?  lack of energy results in gravitational contraction  2. How doe
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