Changes between Version 14 and Version 15 of u/erica/RadFeedback
- Timestamp:
- 11/19/15 14:02:32 (9 years ago)
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u/erica/RadFeedback
v14 v15 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. Th us, [[latex($r=ir_{acc}$)]] in the code. 2. We take [[latex($v(r)$)]] to be the velocity of the ith cell 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. 5. [[latex($R_{*}=\frac{1}{4}\Delta X_{min}$)]].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).