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Supernova 1972e in NGC 5253
Kirshner, R. P.; Oke, J. B.
AA(Hale Observatoires, Pasadena, Calif.), AB(Hale Observatoires, Pasadena, Calif.)
Astrophysical Journal, vol. 200, Sept. 15, 1975, pt. 1, p. 574-581. (ApJ Homepage)
Publication Date:
NASA/STI Keywords:
Astronomical Models, Stellar Evolution, Supernovae, D Lines, Metal Ions, Plasma Spectra, Stellar Envelopes, Stellar Luminosity
Bibliographic Code:


Absolute energy distributions of the Type I supernova 1972e in NGC 5253 extending to about 700 days after maximum light have been obtained. A physical model of the expanding envelope, based on the identification of the feature at 6550 A with H-alpha is proposed. It consists of a differentially expanding atmosphere, with electron density ranging from 10 billion near maximum light to about 10 million 340 days later, illuminated by a photosphere with temperature in the range from 10,000 K to 7000 K. Under these conditions, the identifications of Ca II 8600-A, H, and K lines, the Na D lines, and the Mg I b lines forming P Cygni lines are quite plausible. More than 200 days after maximum, the spectrum is dominated by four features between 4200 and 5500 A. Three of these four features match the blended emissions from over 100 Fe II forbidden lines. If this identification is correct, the envelope requires about 0.01 solar mass of iron, which corresponds to an Fe/H ratio about 20 times higher than the cosmic abundance. Possible identifications of the fourth feature with the Mg I 4571-A line or permitted lines of Fe II are also discussed.

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