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6.5. Hydrodynamical simulations as probes for the structure of the galactic center

The Central Region of NGC 4321

Published online by Cambridge University Press:  25 May 2016

K. Wada ,
T. Minezaki ,
K. Sakamoto  and
H. Fukuda
K. Wada
Affiliation:
National Astronomical Observatory, Mitaka, Tokyo 181, Japan
T. Minezaki
Affiliation:
National Astronomical Observatory, Mitaka, Tokyo 181, Japan
K. Sakamoto
Affiliation:
Caltech, Radio Astronomy Department, 105-24, Pasadena, CA 91125
H. Fukuda
Affiliation:
Department of Physics, Hokkaido University, Sapporo 060, Japan

Extract

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Numerical modeling of the interstellar gas in galaxies is an effective approach to infer galactic gravitational structure. This is because the dynamical behavior of gas is very sensitive to the background gravitational potential. Since the dynamical resonances depend closely on the mass distribution and the pattern speed of the non-axisymmetric component, it is possible to determine these dynamical parameters by comparison of numerical simulations and gas observations.

Type
Part II. Nuclear Interstellar Medium
Information
Symposium - International Astronomical Union , Volume 184: The Central Regions of the Galaxy and Galaxies , 1998 , pp. 271 - 272
Copyright
Copyright © Kluwer 1998 

References

Knapen, J. H., Beckman, J. E., Heller, C. H., Shlosman, I., de Jong, R. S., 1995b, ApJ, 454. 623.Google Scholar
Sakamoto, K., Okumura, S., Minezaki, T., Kobayash, Y., Wada, K. 1995, AJ, 110, 2075.CrossRefGoogle Scholar
Sempere, M. J., Garcia-Burillo, S., Combes, F., Knapen, J. H. 1995, A&Ap, 296, 45.Google Scholar