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 .

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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
Chapters 14 and 15 Stellar Evolution and Stellar Remnants




Chapters 14 and 15 stellar evolution and stellar remnants

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
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


Chapters 14 and 15 stellar evolution and stellar remnants

The end states of stars depends upon its mass!

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





Chapters 14 and 15 stellar evolution and stellar remnants

Elderly, core:

White Dwarf

The core of the

white dwarf star is

now all carbon and

oxygen


Chapters 14 and 15 stellar evolution and stellar remnants

Elderly, envelope:

Planetary nebula

Ring Nebula

Eskimo Nebula




Chapters 14 and 15 stellar evolution and stellar remnants

Figure 13.19

Elderly, dying star:Supernova



Chapters 14 and 15 stellar evolution and stellar remnants

Our Sun will never explode.

Only massive stars explode

as supernova!


Chapters 14 and 15 stellar evolution and stellar remnants

Elderly, core:

Neutron Star

Core

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




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