TY - JOUR

T1 - The mu and tau number of supernovae

AU - Horowitz, C. J.

AU - Li, Gang

PY - 1998/12/10

Y1 - 1998/12/10

N2 - The neutrino-nucleon cross section is slightly larger than that for ν̄ - N. Therefore, ν̄ will escape more quickly from core collapse supernovae leaving the star ν rich. A diffusion formalism is used to calculate the time evolution of the mu and tau lepton number densities. These quickly reach steady state equilibria. We estimate that a protoneutron star with a maximum temperature near 50 MeV will contain over 50% more νμ and ντ than ν̄μ and ν̄τ. Supernovae may be the only known systems with large mu and or tau lepton numbers.

AB - The neutrino-nucleon cross section is slightly larger than that for ν̄ - N. Therefore, ν̄ will escape more quickly from core collapse supernovae leaving the star ν rich. A diffusion formalism is used to calculate the time evolution of the mu and tau lepton number densities. These quickly reach steady state equilibria. We estimate that a protoneutron star with a maximum temperature near 50 MeV will contain over 50% more νμ and ντ than ν̄μ and ν̄τ. Supernovae may be the only known systems with large mu and or tau lepton numbers.

UR - http://www.scopus.com/inward/record.url?scp=0345918866&partnerID=8YFLogxK

U2 - 10.1016/S0370-2693(98)01293-3

DO - 10.1016/S0370-2693(98)01293-3

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AN - SCOPUS:0345918866

SN - 0370-2693

VL - 443

SP - 58

EP - 62

JO - Physics Letters, Section B: Nuclear, Elementary Particle and High-Energy Physics

JF - Physics Letters, Section B: Nuclear, Elementary Particle and High-Energy Physics

IS - 1-4

ER -