WhiteDwarfs - o Produced in binary systems where hydrogen...

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White Dwarfs and Neutron Stars Nova accretion rates onto the WD are 10^-10 to 10^-8 Msun/year The temperature, density of accreted matter eventually becomes hot enough for H fusion – not in core, on surface Surface erupts in thermonuclear explosion – nova Recurrent Novae Nova star system temporarily occurs much brighter The explosion drives accreted matter out into space Energy of nova event usually not enough to break the White Dwarf apart: Novae can recur o Can be thousands to hundred of thousands times brighter than original system
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Unformatted text preview: o Produced in binary systems where hydrogen rich material falling onto surface of white dwarf “Non-Recurrent Novae” • Chandrasekher Limit for a white dwarf o Limiting mass that can be supported by electron degeneracy pressure • White dwarfs in binaries gain mass; what happens if they gain so much mass they exceed 1.4x mass of the sun? o Star blow up via Carbon Deflagration (WD shrinks, interior heats up, carbon starts to fuse under explosive conditions) o Produces a supernovae (Type Ia): complete destruction of White Dwarf...
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This note was uploaded on 03/16/2011 for the course ASTRO 2 taught by Professor Corcoran during the Spring '11 term at GWU.

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