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The Bulge-disc connection in the Milky Way

Published online by Cambridge University Press:  01 June 2008

James Binney
James Binney*
Affiliation:
Rudolf Peierls Centre for Theoretical Physics, Keble Road, Oxford OX1 3NP, UK email: binney@thphys.ox.ac.uk
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Abstract

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Bulges come in two flavours – classical and pseudo. The principal characteristics of each flavour are summarised and their impact on discs is considered. Classical bulges probably inhibit the formation of stellar discs. Pseudobulges exchange angular momentum with stars and gas in their companion discs, and also with its embedding dark halo. Since the structure of a pseudobulge depends critically on its angular momentum, these exchanges are expected to modify the bulge. The consequences of this modification are not yet satisfactorily understood. The Galaxy has a pseudobulge. I review the manifestations of its interaction with the disc. More work is needed on the dynamics of gas near the bulge's corotation radius, and on tracing the stellar population in the inner few hundred parsecs of the Galaxy.

Keywords

Galaxy: kinematics and dynamicsGalaxy: bulgegalaxies: kinematics and dynamics
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 4 , Issue S254: The Galaxy Disk in Cosmological Context , June 2008 , pp. 145 - 152
Copyright
Copyright © International Astronomical Union 2009

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