Changes between Version 5 and Version 6 of u/erica/scratch4

Timestamp:

02/16/16 14:15:13 (9 years ago)

Author:

Erica Kaminski

Comment:

—

u/erica/scratch4

@@ -9 +9 @@
 = Accretion Luminosity = 
 
-As I discuss in this [https://astrobear.pas.rochester.edu/trac/blog/erica01262016 blog post], using the approximation for accretion luminosity as:
+As discussed [https://astrobear.pas.rochester.edu/trac/blog/erica01262016 here], the following equation for the accretion luminosity:
 
-[[latex($L=\frac{G*M*dm}{r_* dt}$)]]
+[[latex($L=\frac{G M dm}{R dt}$)]]
 
-ddw
+should be a very good approximation for Astrobear to use.  
 
 = Tracking accretion luminosity in the code = 
+
+At each time-step i, the luminosity is computed as:
+
+[[latex($L_i=\frac{G M_i dm_i}{R ~dt}$)]]
+
+where [[latex($M_i$)]] is the mass of the sink particle at i, [[latex($dm_i$)]] is the total accreted mass for that time-step, [[latex($G$)]] is the gravitational constant in computational units, [[latex($R$)]] is the radius of the star, taken to be 1 solar radius by default, but modifiable by the user at run-time, and [[latex($dt$)]] is the hydro time-step. This luminosity is only computed after the sink particle has grown to have non-zero mass, and then will only be a source of luminosity after surrounding material has been deemed unstable and collapsing inward to the sink particle (i.e. is accreted).  
 
 == Kernel ==