Physics
Scientific paper
May 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21812507n&link_type=abstract
American Astronomical Society, AAS Meeting #218, #125.07; Bulletin of the American Astronomical Society, Vol. 43, 2011
Physics
Scientific paper
The physics behind hot, massive stars is complicated, making the stars' properties difficult to model. For this reason, we rely on observational tests to see how well stellar evolutionary theory predicts the relative numbers of various types of massive stars. The star-forming galaxies of the Local Group, with their varying metallicities, provide an excellent laboratory for such studies, as massive star evolution is strongly influenced by mass-loss rates, which in turn depend upon metallicity, at least on the main sequence. We've recently begun a far deeper, and more complete survey of the Wolf-Rayet (WR) content of Local Group galaxies compared to what has been done in the past. Here we discuss our candidate selection process, as well as the results from our most recent study of M33 which yielded 56 new WR stars. The relative number of WCs to WNs would support there being a strong metallicity gradient. This work was supported by the National Science Foundation under AST-1008020.
Massey Pedro
Neugent Kathryn
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