The physical conditions in the shells of type I supernovae

Details The physical conditions in the shells of type I supernovae The physical conditions in the shells of type I supernovae

Jan 1975

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975ap%26ss..32...39m&link_type=abstract

Astrophysics and Space Science, vol. 32, Jan. 1975, p. 39-53.

Astronomy and Astrophysics

Astrophysics

6

Astronomical Models, Stellar Envelopes, Stellar Spectra, Supernovae, Absorption Spectra, Calcium, Continuous Spectra, Hydrogen, Light Curve, Opacity, Photosphere, Silicon

Scientific paper

Two models of the origin of the spectrum of type I supernovae are analyzed: (1) the photosphere of the central remnant and the expanding shell are separated by a density cavity; (2) the photosphere is the inner part of the expansing shell. Opacity of the shell close to light maximum for 4000 A is mostly due to Thomson scattering; soon after light maximum the shell becomes completely transparent in this region of the spectrum. A very noticeable dispersion in the velocities of the radial gas motions in the shell is the principal cause of the large equivalent width of the absorption lines in the spectra of these supernovae. The role played by the inhomogeneities in the shell is also discussed. The depth of the strong absorption lines produced by a very inhomogeneous shell may be equal to the filling factor of the medium. From the analysis of the spectra of supernova 1972e, a lower limit for the mass of the shell is obtained. Then from the fact of absence of a detectable H-absorption line and a simultaneous presence of strong Si II absorption lines in the spectrum of supernova 1972e, it follows that the ratio Si/H is at least two or three orders greater than that for the 'normal' stars.

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