The Wind - Relationship for SMC a- and B-Supergiants

Details The Wind - Relationship for SMC a- and B-Supergiants The Wind - Relationship for SMC a- and B-Supergiants

Jul 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995hst..prop.6078l&link_type=abstract

HST Proposal ID #6078

Astronomy and Astrophysics

Astronomy

Hst Proposal Id #6078 Hot Stars

Scientific paper

Very recently a tight empirical relation between the windmomentum and luminosity has been found forgalactic supergiants of spectral type O,B and A. This windmomentum-luminosity relationship provides the means ofdetermining the distances of blue supergiants in othergalaxies much more accurately than traditional methods.However using HST observations of O-stars in the MagellanicClouds it has been demonstrated that this method is dependenton metallicity with large departures from the Milky Wayresults occurring for the SMC. We propose observing a sampleof A- and B-supergiants in the SMC to derive wind terminalvelocities which will be used together with visual data, including HAlpha profiles, to derive stellar parameters andmass-loss rates. These results for the low metallicityenvironment of the SMC, and analogous results for Milky Wayand LMC, will be used to calibrate and verify this techniquefor blue supergiants such that it can be applied to stars ineven more distant galaxies. An important corollary to thiswork is that the calibration of mass-loss rates as a functionof metallicity is important for many other aspects ofastronomy involving massive stars; stellar evolution,starburst regions/galaxies, dynamics/energetics of HIIregions and chemical evolution of galaxies.

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