High Temperatures, Low Metal Content: Atmospheric Model Results for 28 Magellanic Cloud O Stars.

Details High Temperatures, Low Metal Content: Atmospheric Model Results for 28 Magellanic Cloud O Stars. High Temperatures, Low Metal Content: Atmospheric Model Results for 28 Magellanic Cloud O Stars.

Dec 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...211.5902z&link_type=abstract

American Astronomical Society, AAS Meeting #211, #59.02; Bulletin of the American Astronomical Society, Vol. 39, p.841

Astronomy and Astrophysics

Astronomy

Scientific paper

This study is aimed at determining the physical properties of hot, massive stars as a function of metallicity. We obtained very high signal to noise (>300) optical spectra of a sample of 28 Magellanic Cloud O-type stars using the Clay 6.5-m Magellan telescope. This sample comprised the last 28 previously unanalyzed stars for which UV spectra had been obtained with HST. The optical spectra were modeled using the NLTE program FASTWIND. We fill in gaps in the spectral types and luminosity class from previous recent work (Massey et al 2004, Massey et al 2005), allowing us to compare the physical properties of SMC and LMC stars (Z/Z &sun;= 0.2 and Z/Z&sun; = 0.5 respectively) to their Galactic counterparts. Our results are consistent with previous findings that low metallicity O stars of a particular spectral type have higher effective temperatures than high metallicity stars of the same type. This is due to the increased importance of stellar winds and metal line-blanketing at higher metallicities. This work was supported by the NSF through AST-0453611 and NASA/HST through programs GO-09412 and AR-11270.

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