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Ch20 Stellar Evo Pt1

Vocabulary

TermDefinition
Stellar Evolution process by which a star changes over the course of time; determined by its mass
Hydrostatic Equilibrium when gravity's inward pull is balanced with internal forces from fusion's pressure
Core Contraction when a star's pressure from fusion is no longer equal to that of its gravity
Core Expansion when a star's pressure from fusion is greater than its gravity
Low-Mass Star star with a mass less than 8 times that of the Sun; progenitor of a planetary nebula
High Mass Star star with a mass more than 8 times that of the Sun; progenitor of a supernova
Nonburning Envelope outer layers of a star that are too cool to fuse
Burning Shell layer of a star that is hot enough to fuse between the nonburning ash and envelope
Nonburning Ash buildup of fusion products in the central core of a star not hot enough to fuse
Subgiant Branch evolutionary track of a star just after hydrogen "burning" ceases in the core
Red-Giant Branch evolutionary track of a star during intense hydrogen shell burning
Helium Fusion when helium is able to fuse to form carbon, requires temperatures of at least 100,000,000 K
Beryllium important intermediate in the helium fusion process
Alpha Particle helium-4 nucleus
Triple-Alpha Process creation of carbon-12 by the fusion of three helium-4 nuclei
Helium Flash explosive event when a low-mass star begins fusing helium in its core
Electron Degeneracy Pressure resistance of electrons to further compression once they are squeezed to the point of contact
Zero-Age Main Sequence where stars are on the H-R diagram at the start of core nuclear fusion
Horizontal Branch region of the H-R diagram where post-main-sequence stars reach equilibrium again
Asymptotic Giant Branch path on the H-R diagram after a star ceases burning helium in the core
CNO Cycle chain of reactions that converts H into He using carbon, nitrogen, and oxygen as catalysts in high mass stars
Created by: john_bailey720
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