Massive [tau] neutrino and SN 1987A

Journal Article · Wed Feb 15 04:00:00 EST 1995 · Physical Review, D (Particles Fields); (United States)

DOI:https://doi.org/10.1103/PhysRevD.51.1499· OSTI ID:6852739

Sigl, G ^[1]; Turner, M S ^[2]

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1. Department of Astronomy Astrophysics, Enrico Fermi Institute, The University of Chicago, Chicago, Illinois 60637-1433 (United States) NASA/Fermi Astrophysics Center, Fermi National Accelerator Laboratory, Batavia, Illinois 60510-0500 (United States)
2. Department of Astronomy Astrophysics, Enrico Fermi Institute, The University of Chicago, Chicago, Illinois 60637-1433 (United States) NASA/Fermilab Astrophysics Center, Fermi National Accelerator Laboratory, Batavia, Illinois 60510-0500 (United States) Department of Physics, Enrico Fermi Institute, The University of Chicago, Chicago, Illinois 60637-1433 (United States)

The emission of MeV-mass [tau] neutrinos from newly formed neutron stars is considered in a simple, but accurate, model based upon the diffusion approximation. The [tau]-neutrinosphere temperature is found to increase with mass so that the emission of massive [tau] neutrinos is not suppressed by the Boltzmann factor previously used, ([ital m][sub [nu]]/[ital T][sub [nu]])[sup 1.5]exp([minus][ital m][sub [nu]]/[ital T][sub [nu]]), where [ital T][sub [nu]][similar to]4 MeV--8 MeV. For short [tau] neutrino lifetimes ([tau][sub [nu]][approx lt]10[sup [minus]3] sec) decays and inverse decays lead to a reduction in the temperature of the [tau] neutrinosphere. Using our results, we revise limits to the mass and lifetime of an MeV-mass [tau] neutrino based upon SN 1987A. Our constraints, together with bounds based upon primordial nucleosynthesis and laboratory experiments, exclude the possibility of a [tau] neutrino more massive than 0.4 MeV if the dominant decay mode is radiative and [tau][sub [nu]][approx gt]2.5[times]10[sup [minus]12] sec ([ital m][sub [nu]]/MeV). The lifetime restriction does not apply for the modes [nu][sub [tau]][r arrow][nu][sub [ital e],[mu]]+[gamma]. Our technique and results are easily generalized to other hypothetical MeV-mass particles whose interactions are of roughly weak strength. Finally, we speculate on the possible role a 15 MeV--30 MeV [tau] neutrino might play in powering supernova explosions.

• OSTI ID: 6852739
• Journal Information: Physical Review, D (Particles Fields); (United States), Journal Name: Physical Review, D (Particles Fields); (United States) Vol. 51:4; ISSN PRVDAQ; ISSN 0556-2821
• Country of Publication: United States
• Language: English

Related Subjects

662430* -- Properties of Leptons-- (1992-)
72 PHYSICS OF ELEMENTARY PARTICLES AND FIELDS
DIFFUSION
ELEMENTARY PARTICLES
EMISSION
ENERGY RANGE
ERUPTIVE VARIABLE STARS
FERMIONS
HEAVY LEPTONS
LEPTONS
LIFETIME
MASSLESS PARTICLES
MEV RANGE
NEUTRINOS
NEUTRON STARS
NUCLEOSYNTHESIS
POSTULATED PARTICLES
STARS
SUPERNOVAE
SYNTHESIS
TAU NEUTRINOS
VARIABLE STARS