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scratch4

-              v23
+              v24
 The accretion energy ([[latex($L*dt$)]]) will then be distributed smoothly in a kernel surrounding the sink every time step. From there it will diffuse away from the sink via FLD radiative transfer. In this way, sinks will act as additional sources of radiation within the grid.
 = Tracking accretion luminosity in the code =
+= Tracking accretion energy 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 time 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.
+where [[latex($M_i$)]] is the mass of the sink particle at time 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.
 == Kernel ==