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Late-Type Giants in the Bulge, at High Galactic Latitudes and in the Plane

Published online by Cambridge University Press:  25 May 2016

Patricia Whitelock
Patricia Whitelock*
Affiliation:
South African Astronomical Observatory, P O Box 9, Observatory, 7935 Cape, South Africa

Abstract

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Mira and non-Mira M stars are easily distinguished by means of their near-infrared colours. The Miras show a large range of mass-loss rates, and the actual rates are a strong function of the K-[12] colour. The kinematics and scale heights of these Miras are a function of their pulsation periods. The period distribution of Miras in the South Galactic Cap is similar to that of Miras in the Bulge. Non-Mira M stars in the South Galactic Cap have similar colours to their counterparts in the Bulge but differ from bright M-giants in the solar neighbourhood. The galactic distribution and scale height of the M giants is a function of colour and it is suggested that differences in composition influence the colours.

Information

Type
Chapter 5: How Did the Milky Way Form?
Information
Symposium - International Astronomical Union , Volume 169: Unsolved Problems of the Milky Way , 1996 , pp. 411 - 417
Copyright
Copyright © Kluwer 1996 

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