Pulsations and Mass-loss in Massive Wolf - Rayet Stars: M O S T Observations of W R 123 and W R 103

Details Pulsations and Mass-loss in Massive Wolf - Rayet Stars: M O S T Observations of W R 123 and W R 103 Pulsations and Mass-loss in Massive Wolf - Rayet Stars: M O S T Observations of W R 123 and W R 103

Jun 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006aas...208.4601m&link_type=abstract

American Astronomical Society Meeting 208, #46.01; Bulletin of the American Astronomical Society, Vol. 38, p.121

Astronomy and Astrophysics

Astrophysics

2

Scientific paper

The massive, luminous Population I Wolf-Rayet stars drive fast, dense winds.Their sustained (on evolutionary time scales) mass-loss rates exceed theoretical predictions by an order of magnitude. Looking for an alternative mechanism which may help to boost the mass-loss rate, we obtained long-term (5.5 weeks), high-quality, non-stop photometry of two presumably single WR stars, WR 123 (WN8) and WR103 (WC8), using the unique capabilities of the MOST (Microvariability and Oscillations of Stars), a specialized astrophysical micro-satellite. Our targets belong to the cool end of each of the two different evolutionary branches of the WR family: WR123 is ascribed to the WN (Nitrogen-rich) class, while WR103 represents the WC group (Carbon-rich; perceived to be a more advanced evolutionary stage following WN). Despite the difference in evolutionary paths, both stars show dynamic, complex power spectra, with multiple components in the range f (0.1-10) d-1, coherency times not exceeding 10d, and typical amplitudes 5-20 mmag. The photometry provides very strict upper limits on short-term pulsations: amplitudes less than 0.2 mmag for any frequencies higher than 10 d-1. Simultaneous spectroscopy, by probing conditions in the stellar winds, allowed us to link, quite unequivocally, the observed photometric variability to pulsations of the stellar cores.

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