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Bulge K and M giants

Published online by Cambridge University Press:  07 August 2017

Donald M. Terndrup
Donald M. Terndrup*
Affiliation:
Department of Astronomy, The Ohio State University, 174 W. 18th. Ave., Columbus, OH 43210 USA

Abstract

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Several independent studies of the abundances and kinematics of K and M giants in the inner Galaxy (R < 2 kpc) are assembled to trace out this region's global properties. The mean metal abundance is [M/H] ≈ +0.3 at R = 0.5 kpc, and declines by about 1.2 dex out to R = 2 kpc. The line-of-sight velocity dispersion at R = 0.5 kpc is σr ≈ 115 km sec—1 for all population tracers, and declines by d log σr /d log R = —0.4. It now seems fairly clear that only the most metal-poor K giants become RR Lyrae variables, while the more metal-rich ones become late M stars. There is some evidence that the most metal-rich stars are in a flatter, more rapidly rotating system. Metal abundance ratios for a few K giants suggest that the inner Galaxy may have formed rapidly.

Keywords

Galactic BulgeLate-type StarsMetallicity GradientsStellar Abundances
Type
Invited Reviews
Information
Symposium - International Astronomical Union , Volume 153: Galactic Bulges , 1993 , pp. 87 - 100
Copyright
Copyright © Kluwer 1993 

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