DOI QR코드

DOI QR Code

EVOLUTION OF SELF-GRAVITATING GAS DISKS UNDER THE INFLUENCE OF A ROTATING BAR POTENTIAL

  • YUAN CHI (Institute of Astronomy & Astrophysics, Academia Sinica, Physics Department, National Taiwan University) ;
  • YEN DAVID C. C. (Institute of Astronomy & Astrophysics, Academia Sinica, Mathematics Department, Fu Jen Catholic University)
  • Published : 2005.06.01

Abstract

It is well known that a rotating bar potential can transport angular momentum to the disk and hence cause the evolution of the disk. Such a process is particularly important in disk galaxies since it can result in fuelling AGNs and starburst ring activities. In this paper, we will present the numerical simulations to show how this mechanism works. The problem, however, is quite complicated. We classify our simulations according to the type of Lindbald resonances and try to single out the individual roles they play in the disk evolution. Among many interesting results, we emphasize the identification of the origin of the starburst rings and the dense circumnuclear molecular disks to the instability of the disk. Unlike most of the other simulations, the self-gravitation of the disk is emphasized in this study.

Keywords

Lindblad resonance;bar-driven density waves;Toomre instability

References

  1. Bruhweiler, F. C., Miskey, C. L.; Smith, A. M., Landsman, W., & Malumuth, E., 2001 ApJ, 546, 866 https://doi.org/10.1086/318302
  2. Elmegreen, B. G., & Elmegreen, D. M., 1990, ApJ, 355,52 https://doi.org/10.1086/168740
  3. Jackson, J. M., Heyer, M. H., Paglione, T. A. D., & Bolatto, A, D., 1996, ApJ, 456, L91
  4. Jin, S., & Xin, Z. P., 1995, Commun. Pure Appl. Math., 58, 235
  5. Lin, C. C., & Lau, Y. Y., 1975, SJAM, 29, 352
  6. Yuan, C., & Cheng, Y., 1991, ApJ, 376, 104 https://doi.org/10.1086/170259
  7. Yuan, C., & Kuo, C. L., 1997, ApJ, 486, 750 https://doi.org/10.1086/304568
  8. Yuan, C., & Chao-lin Kuo, 1998, ApJ, 497, 689 https://doi.org/10.1086/305482

Cited by

  1. ON THE ORBITAL EVOLUTION OF A GIANT PLANET PAIR EMBEDDED IN A GASEOUS DISK. I. JUPITER-SATURN CONFIGURATION vol.714, pp.1, 2010, https://doi.org/10.1088/0004-637X/714/1/532
  2. On the Orbital Evolution of a Jovian Planet Embedded in a Self‐Gravitating Disk vol.676, pp.1, 2008, https://doi.org/10.1086/528707
  3. FORMATION OF ISOTHERMAL DISKS AROUND PROTOPLANETS. I. INTRODUCTORY THREE-DIMENSIONAL GLOBAL SIMULATIONS FOR SUB-NEPTUNE-MASS PROTOPLANETS vol.790, pp.1, 2014, https://doi.org/10.1088/0004-637X/790/1/32
  4. SPIRAL DENSITY WAVES IN M81. II. HYDRODYNAMIC SIMULATIONS OF THE GAS RESPONSE TO STELLAR SPIRAL DENSITY WAVES vol.800, pp.2, 2015, https://doi.org/10.1088/0004-637X/800/2/106
  5. Hydrodynamical Simulations of the Barred Spiral Galaxy NGC 6782 vol.684, pp.2, 2008, https://doi.org/10.1086/590247
  6. HYDRODYNAMICAL SIMULATIONS OF THE BARRED SPIRAL GALAXY NGC 1097 vol.771, pp.1, 2013, https://doi.org/10.1088/0004-637X/771/1/8
  7. ULTRAHARMONICS AND SECONDARY SPIRAL WAKES INDUCED BY A PLANET vol.832, pp.2, 2016, https://doi.org/10.3847/0004-637X/832/2/166
  8. THE CENTRAL REGION OF THE NEARBY SEYFERT 2 GALAXY NGC 4945: A PAIR OF SPIRALS vol.731, pp.1, 2011, https://doi.org/10.1088/0004-637X/731/1/15
  9. CENTRAL REGIONS OF BARRED GALAXIES: TWO-DIMENSIONAL NON-SELF-GRAVITATING HYDRODYNAMIC SIMULATIONS vol.747, pp.1, 2012, https://doi.org/10.1088/0004-637X/747/1/60
  10. A Numerical Convolution Representation of Potential for a Disk Surface Density in 3D vol.2014, 2014, https://doi.org/10.1155/2014/693537