Hostname: page-component-745bb68f8f-kw2vx Total loading time: 0 Render date: 2025-01-13T11:01:03.000Z Has data issue: false hasContentIssue false
  • English
  • Français

A Simple Treatment of the Problem of Radiative Transfer in Supernova-Like Envelopes

Published online by Cambridge University Press:  12 April 2016

J. Isern ,
R. López  and
E. Simonneau
J. Isern
Affiliation:
Instituto de Astrofisica de Andalucia(C.S.I.C.) Apdo.2144, 18080 Granada, (Spain) Grup d’Astrofisica, (Institut d’Estudis Catalans)
R. López
Affiliation:
Grup d’Astrofisica, (Institut d’Estudis Catalans) Departament de Fisica de l’Atmosfera, Astronomia i Astrofisica, (Universitat de Barcelona) Diagonal 647. 08028 Garcelona, (Spain)
E. Simonneau
Affiliation:
Institut d’Astroohysiaue de Paris 98bis Bd. Aragó. 75014 Paris, (France)

Extract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

Since the only direct information, on the physics of supernova explosions comes from spectrophotometry of their light curves, it is wortwhile to put considerable effort on understanding the properties of supernova atmospheres. Two problems appear, however, in doing so. First, the mean free path of a photon in the region where the Spectrum forms (the atmosphere) is an important fraction of the supernova size and the plane parallel approximation breaks down. Second, the roles of scattering and absorption in the formation of the continuum are not clearly determined.

The complications introduced by spherical geometry arise from the angular derivative terms in the transfer equation and from the high degree of anisotropy introduced by the geometry. The complications introduced by scattering arise from the presence of the mean intensity in the source term of the transfer equation. As an outcome, its numerical solution is time consuming, and classical simplifications are not possible due to the strong anisotropy of the radiation field. In hydrodynamical calculations it is better to calculate the moments of the radiation field, but the success of this method depends on the possibility of replacing the infinite set of differential equations by the equations of low order moments plus a closure relationship that keeps all the properties of the higher moments.

Type
Part III. Chemical and Dynamical Structures of Exploding Stars
Information
International Astronomical Union Colloquium , Volume 108: Atmospherics Diagnostics of Stellar Evolution: Chemical Peculiarity, Mass Loss, and Explosion , 1988 , pp. 436 - 437
Copyright
Copyright © Springer-Verlag 1988

References

Castor, J.I., 1972, Astrophys. J., 178, 779.Google Scholar
Isern, J., López, R., and Simonneau, E., 1987, Rev. Mex. Astron. Astrof., 14 in press.Google Scholar
López, R., Simonneau, E., and Isern, J., 1987, Astr. Astroph., 184 in press.Google Scholar
Simonneau, E., Isern, J., and López, R., 1987, preprint.Google Scholar
Simonneau, E., 1980, Bull. Soc. Roy. des Sci. de Liège. n9-10, p. 281.Google Scholar