Chapters 14 and 15 stellar evolution and stellar remnants
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Chapters 14 and 15 Stellar Evolution and Stellar Remnants PowerPoint PPT Presentation


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Chapters 14 and 15 Stellar Evolution and Stellar Remnants. Star Birth: Nebula. Young star: Protostar. Adult: Main Sequence .

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Chapters 14 and 15 Stellar Evolution and Stellar Remnants

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Chapters 14 and 15 Stellar Evolution and Stellar Remnants


Star Birth: Nebula


Young star: Protostar


Adult: Main Sequence

  • As the temperature in the interior rises, nuclear reactions produce outward force and balances the inward force of gravity  hydrostatic equilibrium = star becomes stable and contraction stopsmain-sequence star


Energy Sources in Stars

  • 4 hydrogen nuclei fuse to become 1 helium nucleus

  • Since the mass of 4 hydrogen nuclei is greater than the mass of 1 helium nucleus, the leftover mass (0.7%) is converted to energy by Einstein’s equation: E=mc2


The end states of stars depends upon its mass!

The more massive a star, the faster it consumes its fuel, the shorter its lifetime


A B C


Evolution of Low Mass Stars including our Sun M < 10 Solar Masses


Old Age: Red Giant


Elderly, core:

White Dwarf

The core of the

white dwarf star is

now all carbon and

oxygen


Elderly, envelope:

Planetary nebula

Ring Nebula

Eskimo Nebula


Yeah, but what about the really Massive stars?


Old Age: Red Supergiant


Figure 13.19

Elderly, dying star:Supernova


Super Nova Remnants


Our Sun will never explode.

Only massive stars explode

as supernova!


Elderly, core:

Neutron Star

Core

High mass stars becomes so dense that protons and electrons combine to become neutrons and star becomes neutron star


Life Cycle of a Low Mass Star


Life Cycle of a High Mass Star


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