Hostname: page-component-78c5997874-v9fdk Total loading time: 0 Render date: 2024-11-13T12:13:55.762Z Has data issue: false hasContentIssue false
  • English
  • Français

Galactic scale star formation: Interplay between stellar spirals and the ISM

Published online by Cambridge University Press:  27 April 2011

Keiichi Wada ,
Junichi Baba ,
Michiko Fujii  and
Takayuki R. Saitoh
Keiichi Wada
Affiliation:
Graduate School of Science and Engeering, Kagoshima University, Kagoshima, Japan email: wada@cfca.jp
Junichi Baba
Affiliation:
National Astronomical Observatory of Japan
Michiko Fujii
Affiliation:
Graduate School of Science and Engeering, Kagoshima University, Kagoshima, Japan email: wada@cfca.jp
Takayuki R. Saitoh
Affiliation:
National Astronomical Observatory of Japan
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

Spiral structures in the disk galaxies have been extensively studied by many theoretical papers, but conventional steady-state models are not consistent with what we observe in time-dependent, multi-dimensional numerical simulations and also in real galaxies. Here we review recent progress in numerical modeling of stellar and gas spirals in disk galaxies. The spiral arms excited in a stellar disk can last for 10 Gyrs without the ISM, but each spiral arm is short-lived and is recurrently formed. The stellar spirals are not waves propagating with a single pattern speed. The ISM is concentrated in local potential minima, which roughly follow the galactic rotation together with the stellar arms, therefore galactic dust lanes are not the classic ‘galactic shocks’.

Keywords

N-body simulationSPHhydrodynamics
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S270: Computational Star Formation , May 2010 , pp. 363 - 370
Copyright
Copyright © International Astronomical Union 2011

References

Baba, J., Asaki, Y., Makino, J., Miyoshi, M., Saitoh, T. R., & Wada, K. 2010, ApJ, 706, 471CrossRefGoogle Scholar
Dobbs, C. L. 2008, 391, 844CrossRefGoogle Scholar
Dobbs, C. L. & Bonnell, I. A. 2008, MNRAS, 385, 1893CrossRefGoogle Scholar
Fujii, M. S., Baba, J., Saitoh, T.R., Makino, J., Kokubo, E., Wada, K., 2010, arXiv:1006.1228Google Scholar
Fujimoto, M. 1968, Non-stable Phenomena in Galaxies, proceedings of IAU Symposium No. 29, Byurakan, May 4-12, 1966. Published by "The Pubblishing House of the Academy of Sciences of Armenian SSR Yerevan, 1968 (translated from Russian)., p.453Google Scholar
Hartmann, L., Ballesteros-Paredes, J., & Bergin, E. A. 2001, ApJ, 562, 852Google Scholar
Heitsch, F. & Hartmann, L. 2008, ApJ, 689, 290Google Scholar
Kim, C.-G., Kim, W.-T., & Ostriker, E. C. 2010, arXiv:1006.4691Google Scholar
Meidt, S. E., Rand, R. J., Merrifield, M. R., Shetty, R., & Vogel, S. N. 2008, ApJ, 688, 224Google Scholar
Merrifield, M. R., Rand, R. J., & Meidt, S. E. 2006, MNRAS, 366, L17Google Scholar
Roberts, W. W. 1969, ApJ, 158, 123CrossRefGoogle Scholar
Saitoh, T. R., Daisaka, H., Kokubo, E., Makino, J., Okamoto, T., Tomisaka, K., Wada, K., & Yoshida, N. 2008, PASJ, 60, 667Google Scholar
Saitoh, T. R., Daisaka, H., Kokubo, E., Makino, J., Okamoto, T., Tomisaka, K., Wada, K., & Yoshida, N. 2009, PASJ, 61, 481CrossRefGoogle Scholar
Sellwood, J. A. & Carlberg, R. G. 1984, ApJ, 282, 61Google Scholar
Sellwood, J. A. 2010, arXiv:1008.2737Google Scholar
Shetty, R. & Ostriker, E. C. 2006, ApJ, 647, 997CrossRefGoogle Scholar
Shu, F. H., Milione, V., & Roberts, W. W. Jr. 1973, ApJ, 183, 819Google Scholar
Tomisaka, K. 1986, PASJ, 38, 95Google Scholar
Vázquez-Semadeni, E., Ryu, D., Passot, T., González, R. F., & Gazol, A. 2006, ApJ, 643, 245CrossRefGoogle Scholar
Wada, K. 2008, ApJ, 675, 188Google Scholar
Wada, K. & Koda, J. 2004, MNRAS, 349, 270CrossRefGoogle Scholar