Cooling of neutrons stars proceeds mainly via neutrino emission; As an example we study the modified neutrino bremsstrahlung process $nn \to nn\nu\bar{ \nu}.$ The radiated energy is small compared to other scales in the system. Hence one can use low-energy theorems to compute the neutrino emissivity in terms of the non-radiative process, ie the on-shell $T$ matrix. We find that the use of the $T-$matrix as compared to previous estimates based upon one pion exchange leads a substantial reduction of the predicted emissivity.
Categories: nucl-th astro-ph