Changes between Version 15 and Version 16 of u/erica/radtimescales
- Timestamp:
- 03/30/16 14:31:20 (9 years ago)
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u/erica/radtimescales
v15 v16 77 77 If I assume the radiation output from the protostar (its accretion energy) is constant over time, I can kill the difference of E* on the LHS. This leaves, 78 78 79 [[latex($ t = \frac{ \triangle B(T)}{\kappa_P \rho cE_*}$)]]79 [[latex($ t = \frac{4 \pi \triangle B(T)}{\kappa_P \rho c^2 E_*}$)]] 80 80 81 81 Plugging in for B(T) puts this in terms of temperature: … … 83 83 [[latex($ t = \frac{a(T_2^4-T_1^4)}{\kappa_P \rho c E_*}$)]] 84 84 85 So the coupling time depends on the temperature difference you want to achieve, as well as the planck opacity, density, and radiation output from the protostar. 85 So the coupling time depends on the temperature difference you want to achieve, as well as the planck opacity, density, and radiation output from the protostar. Note, I may have made dropped a factor of 4pi/c in the case it isn't absorbed by 'a'.
