Non-equilibrium beta processes in neutron stars: a relationship between the net reaction rate and the total emissivity of neutrinos
Several different processes could be changing the density in the core of a neutron star, leading to a departure from Î² equilibrium, quantified by the chemical potential difference Î´Î¼ â‰¡ Î¼n -Î¼ p - Î¼e. The evolution of this quantity is coupled to that of the star's interior temperature T by two functions that quantify the rate at which neutrino-emitting reactions proceed: the net reaction rate (difference between Î² decay and capture rates), Î“netT, Î´Î¼). and the total emissivity (total energy-emission rate in the form of neutrinos and antineutrinos), âˆˆtot(T, Î´Î¼). Here, we present a simple and general relationship between these variables, âˆ‚âˆˆtot/âˆ‚Î´Î¼ = 3Î“net, and show that it holds even in the case of superfluid nucleons. This relation may simplify the numerical calculation of these quantities, including superfluid reduction factors. Â© 2006 RAS.
|Título según WOS:||Non-equilibrium beta processes in neutron stars: a relationship between the net reaction rate and the total emissivity of neutrinos|
|Título según SCOPUS:||Non-equilibrium beta processes in neutron stars: A relationship between the net reaction rate and the total emissivity of neutrinos|
|Título de la Revista:||MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY|
|Fecha de publicación:||2006|
|Página de inicio:||276|