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v22	v23
12	12	[[latex($\frac{1}{2} m v_{ff}^2 = \frac{GmM_{}}{R_{}}$)]]
13	13
14		As material passes through the accretion shocks at the surface of the star, kinetic energy will be converted into heat that is then radiated away. For an accretion rate [[latex($\dot{m}$)]], the rate at which this heat is produced, or the ~~luminosity~~ L, is given by:
	14	As material passes through the accretion shocks at the surface of the star, kinetic energy will be converted into heat that is then radiated away. For an accretion rate [[latex($\dot{m}$)]], the rate at which this heat is produced, or the ''accretion luminosity'', L, is given by:
15	15
16	16	[[latex($ L = \frac{1}{2}\dot{m} v_{ff}^2 = \frac{G\dot{m}M_{}}{R_{}}$)]]