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Massive variable stars at very low metallicity?

Published online by Cambridge University Press:  12 July 2011

Dominik J. Bomans  and
Kerstin Weis
Dominik J. Bomans
Affiliation:
Astronomical Institute, Ruhr-University Bochum, Universitätsstr. 150, 44801, Bochum, Germany email: bomans@astro.rub.de, kweis@astro.rub.de
Kerstin Weis
Affiliation:
Astronomical Institute, Ruhr-University Bochum, Universitätsstr. 150, 44801, Bochum, Germany email: bomans@astro.rub.de, kweis@astro.rub.de
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Abstract

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Observational contraints on the evolution and instabilities of massive stars at very low metallicities are limited. Most of the information come from HST observations of one target, I Zw 18. Recent distance estimates of I Zw 18 put it at 17 Mpc, moving detailed studies of single stars clearly beyond the range of current ground based telescopes. Since massive stars with metallcities of 1/10 of solar and below are our best proxies for massive stars in (proto-) galaxies around the time of reionization, finding them and studying their evolution and instabilities is of premium importance for our understanding of galaxy formation, feedback, and the IGM reionization. Here we present pilot study results of variable stars in two more nearby extremely low metallicity galaxies, UGC 5340 and UGCA 292, and comment on the possibilities of more detailed studies of variable massive stars with new ground-based instrumentation.

Keywords

stars: variables: otherstars: evolutionstars: early-type(stars:) supergiantsstars: windsoutflowsgalaxies: stellar contentgalaxies: irregularinstrumentation: spectrographs
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S272: Active OB stars: structure, evolution, mass loss, and critical limits , July 2010 , pp. 265 - 270
Copyright
Copyright © International Astronomical Union 2011

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