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| Title: |
| Spectra of low-mass helium star models and the type IC supernova SN 1987M |
| Authors: |
| Swartz, Douglas A.; Filippenko, Alexei V.; Nomoto, Ken'ichi; Wheeler, J. C. |
| Affiliation: |
| AA(Texas Univ., Austin), AB(California Univ., Berkeley), AC(Tokyo Univ., Japan), AD(Texas Univ., Austin) |
| Publication: |
| Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 411, no. 1, p. 313-322. (ApJ Homepage) |
| Publication Date: |
| 07/1993 |
| Category: |
| Astrophysics |
| Origin: |
| STI |
| NASA/STI Keywords: |
| B STARS, STELLAR EVOLUTION, STELLAR INTERIORS, STELLAR MASS, STELLAR MODELS, STELLAR SPECTRA, SUPERNOVAE, ATMOSPHERIC MODELS, LIGHT CURVE, STELLAR ATMOSPHERES, VISIBLE SPECTRUM |
| DOI: |
| 10.1086/172831 |
| Bibliographic Code: |
| 1993ApJ...411..313S |
Abstract
The question of whether the low-mass helium star models reproduce the helium-poor Type
Ic spectrum of SN 1987M is investigated by comparing the theoretical spectrum from the 3.3-solar-mass model of Shigeyama et al. (1990) to observations of SN 1987M reported by Filippenko et al. (1990). The results indicate a number of positive correlations between the observed and the computed spectra. In both types of spectra, Ca II, O I, and Mg I emission lines dominate at late times, and, if extensive composition mixing is imposed, good fits can be made to the shapes of the emission features and good agreement can be found with the observed ratio of the forbidden and IR triplet blends of Ca II. The former indicates that the 3.3-solar-mass model predicts the proper density/velocity structure, and the latter indicates that the computed temperature structure is consistent with the observation though the lines are too strong relative to the continuum. This result is roughly independent of the He abundance. The computed and observed spectra are consistent with a small Ni-56 production in contrast to Type Ia thermonuclear events whose spectra are dominated by Fe-group lines at late times.
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