Rotational Velocities of B Stars in the Outer Galactic Disk

Details Rotational Velocities of B Stars in the Outer Galactic Disk Rotational Velocities of B Stars in the Outer Galactic Disk

Jan 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21541318g&link_type=abstract

American Astronomical Society, AAS Meeting #215, #413.18; Bulletin of the American Astronomical Society, Vol. 42, p.253

Astronomy and Astrophysics

Astronomy

Scientific paper

Metallicity gradients in the Milky Way disk are important constraints to models of chemical evolution and galaxy formation. As part of a long term project to better constrain the galactic metallicity gradient (Daflon & Cunha) we have obtained spectra of early B stars in the outer disk with the Magellan 6.5m (Clay) and MIKE double echelle spectrograph. We present herein a preliminary analysis of the projected rotational velocities (v sin i), for 150 early B stars in the third galactic quadrant. The stars were selected from the Case-Hamburg Catalog of Luminous Stars (Reed, 2005). Distances have been computed from the reddening-free Q parameter and published Mv values. We use the spectral type information in the catalog to further refine distances of the non-main sequence B stars in our sample. We have followed the method described by Daflon et al (2007) to estimate v sin i for these stars from their He I lines. These stars are primarily field B stars, with galactocentric distances between 8 and 16 kpc, and most of them lie outside dense clusters and associations. Our analysis will address two questions: 1) Is there any evidence for a difference in mean rotation rate as a function of galactocentric distance and/or metallicity; and 2) Do these stars have on average low rotation rates, as seem to characterize stars in the field and in expanding associations near the Sun (Wolff, et al. 2007).

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