Stellar winds and mass loss from extreme helium stars

Details Stellar winds and mass loss from extreme helium stars Stellar winds and mass loss from extreme helium stars

Jun 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010mnras.404.1698j&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Volume 404, Issue 4, pp. 1698-1710.

Astronomy and Astrophysics

Astronomy

2

Stars: Chemically Peculiar, Stars: Evolution, Stars: Mass-Loss

Scientific paper

Extreme helium stars are very rare low-mass supergiants in a late stage of evolution. They are probably contracting to become white dwarfs following a violent phase of evolution which caused them to become hydrogen-deficient giants, possibly R CrB stars. Using the latest generation of models for spherically expanding stellar atmospheres, we set out to measure mass-loss rates for a representative fraction of these stars. We have used high-resolution ultraviolet and optical spectra, and ultraviolet, optical and near-infrared photometry from a variety of archives. Overall atmospheric parameters have mostly been taken from previous analyses and checked for consistency. Mass-loss rates were measured by fitting the P Cygni and asymmetric profiles of C, N and Si ultraviolet resonance lines and lie in the range of 10-10-10-7 Msolar yr-1. These rates follow a Castor-type () relation marking a lower limit for the mass loss from hot stars of all kinds. The mass-loss rates of the stars studied also show a strong correlation with their proximity to the Eddington limit. There is no firm evidence for variability in the stellar wind, although photospheric pulsations have been reported in many cases.

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