Winds of Massive Stars in Nearby Galaxies the WR Stars

Details Winds of Massive Stars in Nearby Galaxies the WR Stars Winds of Massive Stars in Nearby Galaxies the WR Stars

Jul 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995hst..prop.6038b&link_type=abstract

HST Proposal ID #6038

Computer Science

Hst Proposal Id #6038 Hot Stars

Scientific paper

In cycle 1 and cycle 4 we obtained the first FOS spectra of individual early type stars in M31, and M33 respectively. Combined with ground based data, these were used to study stellar atmospheres and winds and compare wind velocities, mass loss rates, and abundances with similar galactic stars. We used both the SEI method, and non-LTE model atmospheres to analyse the data, and made direct comparison with spectra and models of galactic stars. Detailed study of hot star population in galaxies outside the Milky Way provides a very important test to theories of stellar winds, star formation and evolution. This work extends the comparison beyond the Magellanic Clouds, to M31 and M33, which are more similar in structure, mass and chemical composition to the Milky Way. The work should sample different environments and galactocentric distances, to check for metallicity gradient, and different spectral types. Our sample to date still has less than 10 stars, mostly O9 to B2 supergiants. Our on-going ground-based program and analysis of the UIT images, provided excellent new targets: earlier O types, a main sequence O, a LBV star and new Wolf Rayet stars. For all the new targets we have complementary blue optical spectra for accurate spectral type determination, and accurate photometry to assure successful target acquisition.

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