Radiative efficiency
= Radiative efficiency
{title2=$\eta=L/(\dot Mc^2)$}
The <radiative efficiency> is the escaping radiative power divided by an adopted accreted rest-mass <energy> rate. Its meaning depends on where the <mass> rate is measured and which emission is counted. For efficient Newtonian <accretion> onto a stellar surface it scales as $GM/(R_*c^2)$, whereas advection or outflows can reduce luminosity for the same supplied <mass>.