= Stellar neutrino energy loss
{title2=$\epsilon_\nu\ge0$}
Escaping <neutrinos> remove energy produced by nuclear reactions or drawn from thermal reservoirs. Pair annihilation, plasma excitations, photoneutrino emission and electron-ion bremsstrahlung provide thermal losses. This reduces photon <luminosity> or increases the required nuclear and gravothermal supply. At sufficiently extreme collapse densities, <neutrino> transport must replace a free-escape loss approximation.
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