The Discordance of Mass-Loss Estimates for Galactic O-Type Stars

Details The Discordance of Mass-Loss Estimates for Galactic O-Type Stars The Discordance of Mass-Loss Estimates for Galactic O-Type Stars

Aug 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005jrasc..99v.137f&link_type=abstract

Journal of the Royal Astronomical Society of Canada, Vol. 99, No. 4, p.137

Astronomy and Astrophysics

Astronomy

Scientific paper

We have used new FUSE and archival Copernicus and Orfeus observations of the P v resonance doublet to estimate mass-loss rates for a standard sample of Galactic O-type stars. Since P4+ is expected to be the dominant ion in the winds of mid-O stars, its ion fraction is known a priori; and, since P is much less abundant than C or N, its resonance lines are rarely saturated and provide reliable measurements of the ionic column density. The mass-loss rates derived from P v wind profiles are typically 10 to 20 times smaller than those obtained from observations of H alpha line emission or radio continuum emission, both of which are "density squared" diagnostics. We interpret this discrepancy as an indication that the winds of O-type stars are strongly clumped.

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