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The Stellar Disk–Halo Connection

Published online by Cambridge University Press:  03 August 2017

Rosemary F. G. Wyse  and
Gerard Gilmore
Rosemary F. G. Wyse
Affiliation:
The Johns Hopkins University, Baltimore, MD 21218, USA
Gerard Gilmore
Affiliation:
Institute of Astronomy, Cambridge CB3 0HA, England

Abstract

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The thick disk is the stellar disk-halo connection. At least near the solar circle, this component is on average as old as the system of disk globular clusters, or ~ 12 Gyr. This implies that it most probably formed early in the process of Galaxy formation, so that its properties – chemical abundances, stellar kinematics and spatial distribution – contain clues to the physics of these stages of Galaxy evolution. Its present-day importance for the interstellar disk-halo connection lies in the evolution of its constituent stars – gas loss through winds on the red giant and asymptotic giant branches, through planetary nebulae prior to white dwarf formation, and through supernovae. This gas loss results in mass injection, momentum injection and energy injection into the interstellar medium from a stellar population with a scale height of ~ 1kpc.

Type
I. The Disk-Halo Interface in Our Galaxy
Information
Symposium - International Astronomical Union , Volume 144: The Interstellar Disk-Halo Connection in Galaxies , 1991 , pp. 97 - 108
Copyright
Copyright © Kluwer 1991 

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