Young, high-velocity a stars. II - Misidentified, ejected, or unique?

Details Young, high-velocity a stars. II - Misidentified, ejected, or unique? Young, high-velocity a stars. II - Misidentified, ejected, or unique?

Nov 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988apj...334..927l&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 334, Nov. 15, 1988, p. 927-946.

Other

56

A Stars, Early Stars, Milky Way Galaxy, Stellar Evolution, Stellar Motions, Accretion Disks, Galactic Evolution, Main Sequence Stars, Metallic Stars

Scientific paper

Rodgers, Harding, and Sadler identified a group of A stars at the south Galactic (SGP) pole with properties unlike those of any stellar population. They found the stars to be at distances from the disk of 1 kpc to more than 4 kpc, with a velocity dispersion perpendicular to the plane of 66 km s-1, yet they appear to be young stars. In this study, the ages, abundances, and kinematics of a large number of early-type stars at the SGP have been derived in order to examine the properties and augment the sample of high-velocity stars. In striking contrast to a comparative group of normal A stars near the disk the high-velocity A stars were all formed within the last 6.5×108yr. Their calcium abundances range from -0.5 dex to 0.0 dex, and their W velocity dispersion is 62 km s-1. It is shown that the stars are not misidentified horizontal-branch stars. It is suggested that at around 6.5×108yr ago, a major source of relatively low abundance hydrogen was accreted by the Galactic disk, forming young high-velocity stars that do not partake of the age-abundance-kinematics relationships shown by other stellar groupings.

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