Chapter 14.Stellar Remnants

Chapter 14.Stellar Remnants - Stellar Remnants: White...

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1 Stellar Remnants : White Dwarfs, Neutron Stars, and Black Holes Chapter 14
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2 Origin of a White Dwarf
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3 Gravitational Red Shift
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4 What “holds up” a white dwarf? density ~ 10 6 grams/cm 3 electrons are packed very close together Pauli exclusion principle limits this packing The electrons are said to be “degenerate.” There is an upper mass limit , called the Chandrasekhar limit. Upper limit to mass of a white dwarf = 1.4 the mass of the Sun.
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5 Accretion onto a White Dwarf → Accretion could push the mass beyond 1.4 M sun .
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6 One result of accretion - Nova
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7 Another result of accretion – Type I supernova Massive single stars can also become supernovae: Type II.
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8 What happens to the core after a supernova? The next step depends on mass! neutron star
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What’s left after a supernova? Mysterious radio signals were detected in 1967 by J. Bell and A. Hewish. LGM?
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Chapter 14.Stellar Remnants - Stellar Remnants: White...

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