5 | | 2. subroutine getdEdT in EOS.f90 |
| 6 | where T is in cgs unit or Kelvin. |
| 7 | |
| 8 | In current version of AstroBEAR, we have |
| 9 | $$\frac{\partial E}{\partial T}\frac{\partial T}{\partial t}=\frac{10\kappa_{0}K_{B}^{n}}{(\gamma-1)C_{v}}\frac{\partial}{\partial x_{cgs}}\left[T^{n}\frac{\partial T}{\partial x_{cgs}}\right]$$ |
| 10 | |
| 11 | And same as blog:bliu01092014, we define |
| 12 | |
| 13 | $$ \kappa_{1}=\frac{10\kappa_{0}K_{B}^{n}}{(\gamma-1)C_{v} } $$ |
| 14 | $$ q^{*}_{cgs}=\kappa_{1}T^{*}\frac{\partial T}{\partial x_{cgs}}$$ |
| 15 | |
| 16 | And so same as blog:bliu01092014, we have |
| 17 | |
| 18 | In Betti's data, $C_{v}=7.816e26$ and $\gamma=5/3$ so |
| 19 | $$q_{0}=\frac{2}{3}*7.816*1.38*10^{4}*q^{*}_{cgs}$$ |
| 20 | |
| 21 | 2. Scales for converting from cgs to cu |
| 22 | ScaleFlux is the scale which converts the heat flux from cgs units to computational units in AstroBEAR. Since |
| 23 | $$\frac{\partial E}{\partial T}\frac{\partial T}{\partial t}=\frac{\partial Q}{\partial x}$$ |
| 24 | The new scaleFlux is $EScale*velScale$ or $pScale*velScale$ as the temperature is in Kelvin now. |
| 25 | While in the older version where the temperature is in c.u. scale, |
| 26 | $$\frac{1}{\gamma-1}\rho\frac{\partial T}{\partial t}=\frac{\partial Q}{\partial x}$$ |
| 27 | So $scaleFlux is rScale*TempScale*velScale$ instead... |
| 28 | |
| 29 | scaleDiff is the scale that converts the kappa1 from cgs units to computational units. Since |
| 30 | $$ q^{*}_{cgs}=\kappa_{1}T^{*}\frac{\partial T}{\partial x_{cgs}}$$ |
| 31 | So |
| 32 | $$scaleDiff=scaleFlux*lScale$$ |
| 33 | |
| 34 | 3. subroutine getdEdT in EOS.f90 |