Sign on

SAO/NASA ADS Astronomy Abstract Service

· Find Similar Abstracts (with default settings below)
· Full Refereed Journal Article (PDF/Postscript)
· Full Refereed Scanned Article (GIF)
· References in the article
· Citations to the Article (39) (Citation History)
· Refereed Citations to the Article
· SIMBAD Objects (4)
· NED Objects (2)
· Reads History
·
· Translate This Page
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.

Printing Options

Print whole paper
Print Page(s) through

Return 600 dpi PDF to Acrobat/Browser. Different resolutions (200 or 600 dpi), formats (Postscript, PDF, etc), page sizes (US Letter, European A4, etc), and compression (gzip,compress,none) can be set through the Printing Preferences


More Article Retrieval Options

HELP for Article Retrieval
Bibtex entry for this abstract   Preferred format for this abstract (see Preferences)
   

Find Similar Abstracts:

Use: Authors
Title
Keywords (in text query field)
Abstract Text
Return: Query Results Return    items starting with number
Query Form
Database: Astronomy
Physics
arXiv e-prints
    


SAO/NASA ADS Homepage | ADS Sitemap | Query Form | Basic Search | Preferences | HELP | FAQ