Changes between Version 17 and Version 18 of u/erica/RadFeedback
- Timestamp:
- 11/19/15 14:08:51 (9 years ago)
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u/erica/RadFeedback
v17 v18 23 23 [[latex($L=\frac{1}{2} \dot{m}v^2(r)+G(\frac{M_{*}}{R_{*}}-\frac{M_{r}}{r})\dot{m}$)]] 24 24 25 To first order, we make the following approximations. 1. Only mass within the accretion volume will contribute to the accretion luminosity. This is reasonable because all mass within this volume is accreted (albeit proportionally to density). 2. We take [[latex($v(r)$)]] to be the velocity of the ith cell at a distance r away from the sink (for r within the accretion volume). 3. We take [[latex($\dot m$)]] to be the 'Bondi Accretion Rate' already calculated in the code. 4. [[latex($M_{*}$)]] is the mass of the sink particle. Thus, radiative feedback only possible after sinks have performed first accretion. 5. [[latex($R_{*}=\frac{1}{4}\Delta X_{min}$)]]. 6. [[latex($M_r$)]] is the total mass within the accretion volume (sum of all [[latex($q_i(1)$)]] + mass of sink).25 To first order, we make the following approximations. 1. Only mass within the accretion volume will contribute to the accretion luminosity. This is reasonable because only mass within this volume is accreted. 2. We take [[latex($v(r)$)]] to be the velocity of the ith cell at a distance r away from the sink (for r within the accretion volume). 3. We take [[latex($\dot m$)]] to be the 'Bondi Accretion Rate' already calculated in the code. 4. [[latex($M_{*}$)]] is the mass of the sink particle. Thus, radiative feedback only possible after sinks have performed first accretion. 5. [[latex($R_{*}=\frac{1}{4}\Delta X_{min}$)]]. 6. [[latex($M_r$)]] is the total mass within the accretion volume (sum of all [[latex($q_i(1)$)]] + mass of sink).