Wolf-Rayet stars of high and low mass

W.-R. Hamann

Lehrstuhl Astrophysik der Universität Potsdam, Postfach 601553, D-14415 Potsdam, Germany

The quantitative analysis of Wolf-Rayet type spectra requires non-LTE models for expanding atmospheres which are available now. They were extensively applied to study the "classical", massive Wolf-Rayet stars of Population I. The obtained results are briefly reviewed and discussed. Wolf-Rayet type spectra are also shown by a subgroup of central stars of planetary nebulae. Recent spectral analyses of these low-mass stars yielded their parameters and atmospheric abundances, providing the empirical basis for discussing their evolutionary status. Hydrogen deficiency and strong mass-loss are the common features of both, high- and low-mass stars showing Wolf-Rayet type spectra.

In: Hydrogen-Deficient Stars. Proceedings of the 2nd International Colloquium held in Bamberg, Germany, September 1995, U. Heber and C.S. Jeffery (eds.), ASP Conference Series (in press)


The full article is available as PostScript file via anonymous ftp.
Server: ftp.astro.physik.uni-potsdam.de
user: anonymous or ftp; Password: your e-mail address;
file: pub/wrhamann/bamberg_95.ps (1.0MB uncompressed) or bamberg_95.ps.gz (0.23MB compressed).

Display full article with ghostview (local users only!)

Fetch PostScript-File (bamberg_95.ps, 1.0MB, uncompressed)

Fetch PostScript-File (bamberg_95.ps.gz, 0.23MB, compressed)

Zurück zur Übersicht