ay45c5-page32 - from Schatzman (1958) -1.5 Van Maanen 2 o 2...

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Unformatted text preview: from Schatzman (1958) -1.5 Van Maanen 2 o 2 Eri B AC 70 8247 log10(R/R . ) -2.0 n = 3/2 polytrope Sirius B W 219 Ross 627 -2.5 L 930-80 n = 3 polytrope "Chandrasekhar Mass" -3.0 -3.5 -0.6 -0.4 -0.2 0 0.2 0.4 0.6 log10(M/M . ) So, over this range the radius for a given mass decreases; and at R = 0 (M = MCh) the relativistic electrons can no longer support the star. The points plotted on the curve are observational measurements of actual white dwarf stars, and demonstrate that our theory is basically correct, even accurate quantitatively! Note that e = 2 is appropriate because X ' 0: the star must have burned all its hydrogen en route (used up all nuclear fuel). In terms of fundamental constants, we can write ! hc 3=2 1 ;  MCh = 3:10 G m22 pe 144 ...
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This note was uploaded on 12/29/2011 for the course AST 350 taught by Professor Dion during the Fall '09 term at SUNY Stony Brook.

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