How Does Low Metallicity Affect the Rotational Velocities of Very Massive Stars?

Statistics – Methodology

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Scientific paper

Are the rotational velocities of massive stars the same in all galaxies despite their metallicities? We lack the key measurements of projected rotational velocity, V sin i, to answer this important question. There is no study of the V sin i distribution for stars in any galaxy other than the Milky Way. Here we present preliminary V sin i values of these low metallicity, high mass stars from Space Telescope Imaging Spectrograph (STIS) and International Ultraviolet Explorer (IUE) UV observations of 21 Large Magellanic Cloud (LMC, ZLMC =0.007) and 23 Small Magellanic Cloud (SMC, ZSMC =0.002) O-type stars with well determined spectral classifications. Our methodology is based on a previous study of the projected rotational velocities of Galactic O-type stars using IUE Short Wavelength Prime (SWP) Camera high dispersion spectra. Our final results will be the first study of projected rotational velocities of O-type stars outside our own Galaxy. They are a critical first step in constraining several areas in the theoretical study of massive stars and their evolution, notably the predictions that massive stars in a low metallicity environment (1) may form with higher rotational velocities and (2) will have decreased angular momentum loss as the evolve. Support for proposal #09945 was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc. under NASA contract NAS5-26555.

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