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3.16. Bar-driven spiral density waves and accretion of gas-dominated central disks

Published online by Cambridge University Press:  25 May 2016

Chi Yuan
Chi Yuan*
Affiliation:
Institute of Astronomy and Astrophysics, Academia Sinica Box 1-87, Nankang, Taipei, Taiwan, ROC e-mail: yuan@biaa7.biaa.sinica.edu.tw

Extract

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In this short paper, we report the main results of a comprehensive theory of bar-driven spiral density waves. The theory offers explanations of the morphological difference of the spirals observed in the gas-dominated central disks as well as the different patterns of isovelocity curves distorted by the waves. It also gives reliable estimates of the induced mass flux to fuel the AGNs and starburst ring activities and hence the lifespan of the central disks. In particular, we compare our results with the CO and HCN observations of NGC1068 and M100. Based on these results, we can speculate the possible origin of the central bars and will propose two critical observational tests of the theory.

Type
Part I. Stellar Cluster, Star Formation
Information
Symposium - International Astronomical Union , Volume 184: The Central Regions of the Galaxy and Galaxies , 1998 , pp. 121 - 122
Copyright
Copyright © Kluwer 1998 

References

Helfer, T. and Blitz, L. (1995), ApJ, 450, 90.CrossRefGoogle Scholar
Planesas, P., Scoville, N. and Myers, S.T., (1991), ApJ 369, 364.CrossRefGoogle Scholar
Sakamoto, K., et al, (1995), AJ, 110, 2075.Google Scholar
Yuan, C. and Kuo, C.L. (1997), ApJ, 486, 750.CrossRefGoogle Scholar
Yuan, C. and Kuo, C.L. (1997a), Submitted to ApJ.Google Scholar