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Dynamics of galactic nuclei: mass segregation and collisions

Published online by Cambridge University Press:  01 July 2007

Marc Freitag ,
James E. Dale ,
Ross P. Church  and
Melvyn B. Davies
Marc Freitag
Affiliation:
Institute of Astronomy, Madingley road, Cambridge, CB3 0HA, UK email: freitag@ast.cam.ac.uk
James E. Dale
Affiliation:
Lund Observatory, Box 43, SE 22100, Lund, Sweden
Ross P. Church
Affiliation:
Lund Observatory, Box 43, SE 22100, Lund, Sweden Centre for Stellar and Planetary Astrophysics, Monash University, Vic. 3800, Australia
Melvyn B. Davies
Affiliation:
Lund Observatory, Box 43, SE 22100, Lund, Sweden
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Abstract

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Massive black holes (MBHs) with a mass below ~ 107 M⊙ are likely to reside at the centre of dense stellar nuclei shaped by 2-body relaxation, close interactions with the MBH and direct collisions. In this contribution, we stress the role of mass segregation of stellar-mass black holes into the innermost tenths of a parsec and point to the importance of hydrodynamical collisions between stars. At the Galactic centre, collisions must affect giant stars and some of the S-stars.

Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 3 , Symposium S245: Formation and Evolution of Galaxy Bulges , July 2007 , pp. 211 - 214
Copyright
Copyright © International Astronomical Union 2008

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