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The Distribution of Bar Strengths in Disk Galaxies

Published online by Cambridge University Press:  01 August 2006

R. Buta ,
E. Laurikainen ,
H. Salo ,
J. H. Knapen  and
D. L. Block
R. Buta
Affiliation:
Dept. of Physics & Astronomy, University of Alabama, Tuscaloosa, AL 35487, USA
E. Laurikainen
Affiliation:
Division of Astronomy, Dept. of Physical Sciences, University of Oulu, FIN-90014, Finland
H. Salo
Affiliation:
Division of Astronomy, Dept. of Physical Sciences, University of Oulu, FIN-90014, Finland
J. H. Knapen
Affiliation:
University of Hertfordshire, Centre for Astrophysics Research, Hatfield, Herts AL10, 9AB, UK
D. L. Block
Affiliation:
School of Computational & Applied Mathematics, University of the Witwatersrand, Johannesburg, South Africa
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Abstract

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Bars are the most important features that redistribute angular momentum and drive secular evolution in disk galaxies. We have derived the distribution of bar strengths in spirals and the Fourier properties of early-type galaxy bars in order to evaluate recent models of bar-halo angular momentum transfer and external gas accretion. A few results are presented here.

Keywords

galaxies: barsgalaxies: evolution
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S235: Galaxy Evolution Across the Hubble Time , August 2006 , pp. 81
Copyright
Copyright © International Astronomical Union 2007