A Lifetime of Influence: Abstracts, Talks, and Posters
 

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van den Heuvel

  

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The Effects of Metallicity on the Rotation Rates of Massive Stars

Laura R. Penny
College of Charleston

Douglas R. Gies
CHARA, Georgia State University

Stellar interior models that include the effects of angular momentum in low metallicity massive stars predict that these stars should have drastically reduced equatorial winds (mass loss) while on the main sequence, and as such should retain most of their angular momentum. This is supported by indirect observations of both the Be/(B+Be) ratio and the blue-to-red supergiant ratio which appear to have a metallicity dependence that may be caused by high rotational velocities. Several studies have attempted to directly measure the rotation rates of massive stars in the Small and Large Magellenic Clouds to determine whether they do in fact rotate faster than their Galactic counterparts. Unfortunately a large sample size is needed in order to correct for the random distribution of inclination on the sky. The Multimission Archive at Space Telescope (MAST) contains FUSE archival spectra of 161 O-type stars in the Magellanic Clouds. Here we present the results of our project to test the treatment of angular momentum in the new stellar interior models through a large scale survey of projected rotational velocities of O-type stars in three metallicity environments: the Milky Way (Z = 0.020), LMC (Z = 0.007), and the SMC (Z=0.004).