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v19	v20
16	16	[[latex($ L = \frac{1}{2}\dot{m} v_{ff}^2 = \frac{G\dot{m}M_{}}{R_{}}$)]]
17	17
18		Since we do not track energy accretion onto the sink, we are left to assume that the gas that is accreted from the surrounding zones contribute to this accretion luminosity directly. Thus, the best we can do for tracking the energy released from infall is to calculate the RHS of this equation in the code and use it as an estimate of the true accretion luminosity. (By the way, this form of the accretion luminosity was shown to be a good approximation for our purposes [https://astrobear.pas.rochester.edu/trac/blog/erica01262016 here]).
	18	Since we do not track energy accretion onto the sink, we are left to assume that the gas that is accreted from the surrounding zones contributes to this accretion luminosity directly. Thus, the best we can do for tracking the energy released from infall is to calculate the RHS of this equation in the code and use it as an estimate of the true accretion luminosity. (By the way, this form of the accretion luminosity was shown to be a good approximation for our purposes [https://astrobear.pas.rochester.edu/trac/blog/erica01262016 here]).
19	19
20	20	The accretion energy ([[latex($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.