Unformatted text preview: Problem 10: Stellar cores Do you think convection would signiFcantly contribute to the stability of stars via turbulent ram pressure ( ∼ ρ V 2 )? Hint: recall typical values of the convection velocity and consult the momentum conservation equation. Do you think it is justiFed to assume adiabatic stratiFcation of temperature and density of the material inside stars as a reasonable approximation? Assuming adiabatic stratiFcation with adiabatic index γ = 1 . 4 , can you estimate the mass density in the core of the sun, if you know the core temperature to be 15 million degrees, the surface temperature as 6.000 degrees, and the surface mass density ρ s = 3 · 107 gr cm3 ?...
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 Fall '08
 RABE
 Physics, Energy, Work, Fundamental physics concepts, Interstellar medium

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