Hostname: page-component-cd9895bd7-jkksz Total loading time: 0 Render date: 2024-12-23T07:44:06.581Z Has data issue: false hasContentIssue false
  • English
  • Français

Stationary and axisymmetric magnetized equilibria of stars and winds

Published online by Cambridge University Press:  08 June 2011

Shin Yoshida ,
Kotaro Fujisawa ,
Yoshiharu Eriguchi ,
Shijun Yoshida  and
Rohta Takahashi
Shin Yoshida
Affiliation:
Department of Earth Science and Astronomy, Graduate School of Arts and Sciences, University of TokyoKomaba, Meguro-ku, Tokyo 153-8902, Japan email: [email protected]
Kotaro Fujisawa
Affiliation:
Department of Earth Science and Astronomy, Graduate School of Arts and Sciences, University of TokyoKomaba, Meguro-ku, Tokyo 153-8902, Japan email: [email protected]
Yoshiharu Eriguchi
Affiliation:
Department of Earth Science and Astronomy, Graduate School of Arts and Sciences, University of TokyoKomaba, Meguro-ku, Tokyo 153-8902, Japan email: [email protected]
Shijun Yoshida
Affiliation:
Astronomical Institute, Tohoku University6-3 Aramaki, Aoba-ku, Sendai 980-8578, Japan
Rohta Takahashi
Affiliation:
Cosmic Radiation Laboratory, The Institute of Physical and Chemical Research, RIKEN, 2-1 Hirosawa, Wako, Saitama 351-0198, 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.

We present a new formulation to compute numerically stationary and axisymmetric equilibria of magnetized and self-gravitating astrophysical fluids. Under the assumption of ideal MHD, the stream function for the flow can be chosen as a basic variable with which the Euler-Maxwell equations are cast into a set of basic equations, i.e. a generalized Bernoulli equation and a Grad-Shafranov-like equation by employing various integral conditions. A novel feature of this formulation is that systems with stars, disks and winds are treated in a simple unified picture and the magnetic field structures can contain both poloidal and toroidal components.

Keywords

stars: magnetic fieldsstars: rotationstars: windsoutflows
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S274: Advances in Plasma Astrophysics , September 2010 , pp. 437 - 440
Copyright
Copyright © International Astronomical Union 2011

References

Fujisawa, K., Yoshida, S., & Eriguchi, Y. 2010, MNRAS, submittedGoogle Scholar
Keppens, R. & Goedbloed, J. P. 1999, A & A, 343, 251Google Scholar
Lovelace, R. V. E., Mehanian, C., Mobarry, C. M., & Sulkanen, M. E. 1986, ApJS, 62, 1CrossRefGoogle Scholar
Parker, E. N. 1958, ApJ, 128, 664CrossRefGoogle Scholar
Pneuman, G. W. & Kopp, R. A. 1971, Solar Phys., 18, 258CrossRefGoogle Scholar
Sakurai, T. 1985, A & A, 152, 121Google Scholar
Sakurai, T. 1987, PASJ, 39, 821Google Scholar
Weber, E. J. & Davis, L. 1967, ApJ, 148, 217CrossRefGoogle Scholar