... | ... | @@ -65,4 +65,11 @@ the stress tensor in the 2 dimensional case is: |
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+{1\over 2}D_{R\theta}^2-
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{1\over 3}(\nabla \cdot \vec v)^2)`$
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If we assume that the disk's two surfaces can radiate as Plank functions with temperature $`T_{eff}`$ then the radiative cooling rate is: $`Q^-=2\sigma_{SB}T_{eff}`$ |
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in the hypothesis the the gas has only Keplerian speed (no radial velocity and
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$`v_{\theta} = \Omega_K R`$ then:
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$`Q^+ = Sigma \nu D_{R\theta}^2 = {9\over 4}Sigma \nu \Omega_K^2`$
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this simple prescription can also be implemented in a 2 dimensional disk.
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If we assume that the disk's two surfaces can radiate as Plank functions with temperature $`T_{eff}`$ then the radiative cooling rate is: $`Q^-=2\sigma_{SB}T_{eff}^4`$ |
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