Neutrino and photon emission from a dense, high temperature atmosphere

Details Neutrino and photon emission from a dense, high temperature atmosphere Neutrino and photon emission from a dense, high temperature atmosphere

Dec 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981apj...251..311s&link_type=abstract

Astrophysical Journal, Part 1, vol. 251, Dec. 1, 1981, p. 311-324.

Statistics

Computation

18

Dense Plasmas, High Temperature Gases, Neutrinos, Particle Emission, Photons, Stellar Atmospheres, Atmospheric Density, Computational Fluid Dynamics, Hot Stars, Neutron Stars, Opacity, Optical Thickness, Particle Diffusion, Particle Flux Density, Stellar Temperature

Scientific paper

The thermal evolution of a hot, dense medium cooling through neutrino and photon emission is analyzed. It is assumed that the medium is a plane-parallel, semi-infinite atmosphere in hydrostatic equilibrium and that it is initially isothermal. It is noted that the thermal history of the neutrino photosphere is governed by a nonlinear diffusion equation and that at late times the solution of the equation acquires a self-similar form. Since the photon opacity everywhere exceeds the neutrino opacity, the photon flux is markedly below the neutrino flux and can be treated as a small perturbation. The temperature profile, together with the neutrino and photon fluxes, is obtained as a function of depth and time by a combination of numerical and analytic calculations. The main results are summarized by a convenient set of compact, closed-form similarity formulas. These formulas are then used in examining the cooling of a young neutron star during approximately the first 15 sec of its lifetime, when the star is hot, optically thick to photons and neutrinos, and quasi-static out to the neutrino photosphere.

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