Clumping in Galactic WN stars: a comparison of mass loss rates from UV/optical & radio diagnostics

A. Liermann & W.-R. Hamann

Universität Potsdam, Institut für Physik, Astrophysik

The mass loss rates and other parameters for a large sample of Galactic WN stars have been revised by Hamann et al. (2006), using the most up-to date Potsdam Wolf-Rayet (PoWR) model atmospheres. For a sub-sample of these stars exist measurements of their radio free-free emission. After harmonizing the adopted distance and terminal wind velocities, we compare the mass loss rates obtained from the two diagnostics. The differences are discussed as a possible consequence of different clumping contrast in the line-forming and radio-emitting regions.

The full article is available as PostScript file via anonymous ftp.
user: anonymous or ftp; Password: your e-mail address;
file: /usr/aftp/pub/wrhamann/workshop/ (200kB PostScript uncompressed)
or (80kB PostScript compressed)
or liermann.pdf (53kB)

Display full article with ghostview (local users only!)

Fetch PostScript-File (, 200kB, uncompressed)

Fetch PostScript-File (, 80kB, compressed)

Fetch Pdf-File (liermann.pdf, 53kB, uncompressed)

Zurück zur Übersicht