Electron-, Mu-, and Tau-Number Conservation in a Supernova Core

Details Electron-, Mu-, and Tau-Number Conservation in a Supernova Core Electron-, Mu-, and Tau-Number Conservation in a Supernova Core

1999-12-11

arxiv.org/abs/astro-ph/9912242v2

Phys.Rev. D62 (2000) 093021

Astronomy and Astrophysics

Astrophysics

Slightly expanded version with improved presentation, no changes of substance

Scientific paper

10.1103/PhysRevD.62.093021

We study if the neutrino mixing parameters suggested by the atmospheric neutrino anomaly imply chemical equilibrium between mu- and tau-flavored leptons in a supernova (SN) core. The initial flavor-conversion rate would indeed be fast if the nu_mu-nu_tau-mixing angle were not suppressed by second-order refractive effects. The neutrino diffusion coefficients are different for nu_mu, anti-nu_mu, nu_tau and anti-nu_tau so that neutrino transport will create a net mu and tau lepton number density. This will typically lead to a situation where the usual first-order refractive effects dominate, further suppressing the rate of flavor conversion. Altogether, neutrino refraction has the nontrivial consequence of guaranteeing the separate conservation of e, mu, and tau lepton number in a SN core on the infall and cooling time scales, even when neutrino mixing angles are large.

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