Hostname: page-component-78c5997874-g7gxr Total loading time: 0 Render date: 2024-11-11T09:47:52.109Z Has data issue: false hasContentIssue false
  • English
  • Français

Vertical flows and structures excited by magnetic activity in the Galactic center region

Published online by Cambridge University Press:  09 February 2017

Kensuke Kakiuchi ,
Takeru K. Suzuki ,
Yasuo Fukui ,
Kazufumi Torii ,
Mami Machida  and
Ryoji Matsumoto
Kensuke Kakiuchi
Affiliation:
Dept. of Physics, Nagoya University, Furo-cho, Chikusa, Nagoya, Aichi, 464-8602, Japan email: kakiuchi@nagoya-u.jp
Takeru K. Suzuki
Affiliation:
Dept. of Physics, Nagoya University, Furo-cho, Chikusa, Nagoya, Aichi, 464-8602, Japan email: kakiuchi@nagoya-u.jp School of Arts & Sciences, The University of Tokyo, 3-8-1, Komaba, Meguro, Tokyo, 153-8902, Japan
Yasuo Fukui
Affiliation:
Dept. of Physics, Nagoya University, Furo-cho, Chikusa, Nagoya, Aichi, 464-8602, Japan email: kakiuchi@nagoya-u.jp
Kazufumi Torii
Affiliation:
Dept. of Physics, Nagoya University, Furo-cho, Chikusa, Nagoya, Aichi, 464-8602, Japan email: kakiuchi@nagoya-u.jp National Radio Observatory, National Astronomical Observatory of Japan, 462-2, Nobeyama, Minamimaki, Minamisaku, Nagano, 384-1305, Japan
Mami Machida
Affiliation:
Dept. of Physics, Faculty of Sciences, Kyushu University, 6-10-1 Hakozaki, Higashi-ku, Fukuoka 812-8581, Japan
Ryoji Matsumoto
Affiliation:
Dept. of Physics, Graduate School of Science, Chiba University, 1-33 Yayoi-cho, Inage-ku, Chiba 263-8522, 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.

Various observations show peculiar features in the Galactic Center region, such as loops and filamentary structure. It is still unclear how such characteristic features are formed. Magnetic field is believed to play very important roles in the dynamics of gas in the Galaxy Center. Suzuki et al. (2015) performed a global magneto-hydrodynamical simulation focusing on the Galactic Center with an axisymmetric gravitational potential and claimed that non-radial motion is excited by magnetic activity. We further analyzed their simulation data and found that vertical motion is also excited by magnetic activity. In particular, fast down flows with speed of ~100 km/s are triggered near the footpoint of magnetic loops that are buoyantly risen by Parker instability. These downward flows are accelerated by the vertical component of the gravity, falling along inclined field lines. As a result, the azimuthal and radial components of the velocity are also excited, which are observed as high velocity features in a simulated position-velocity diagram. Depending on the viewing angle, these fast flows will show a huge variety of characteristic features in the position-velocity diagram.

Keywords

accretionaccretion discsGalaxy: bulgeGalaxy: centre–Galaxy: kinematics and dynamicsmagnetohydrodynamics (MHD)–turbulence
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 11 , Symposium S322: The Multi-Messenger Astrophysics of the Galactic Centre , July 2016 , pp. 220 - 221
Copyright
Copyright © International Astronomical Union 2017 

References

Fukui, Y., Yamamoto, H., Fujishita, M., et al. 2006, Science, 314, 106 Google Scholar
Machida, M., Matsumoto, R., Nozawa, S., et al. 2009, PASJ, 61, 411 Google Scholar
Parker, E. N. 1966, ApJ, 145, 811 Google Scholar
Suzuki, T. K., Fukui, Y., Torii, K., Machida, M., & Matsumoto, R. 2015, MNRAS, 454, 3049 CrossRefGoogle Scholar
Torii, K., Kudo, N., Fujishita, M., et al. 2010a, PASJ, 62, 1307 Google Scholar
Torii, K., Kudo, N., Fujishita, M., et al. 2010b, PASJ, 62, 675 Google Scholar