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Numerical simulations of magnetized winds of solar-like stars

Published online by Cambridge University Press:  01 November 2008

Aline A. Vidotto ,
M. Opher ,
V. Jatenco-Pereira  and
T. I. Gombosi
Aline A. Vidotto
Affiliation:
University of São Paulo, Rua do Matão 1226, São Paulo, SP, Brazil, 05508-090 email: [email protected] George Mason University, 4400 University Drive, Fairfax, VA, USA, 22030-4444
M. Opher
Affiliation:
George Mason University, 4400 University Drive, Fairfax, VA, USA, 22030-4444
V. Jatenco-Pereira
Affiliation:
University of São Paulo, Rua do Matão 1226, São Paulo, SP, Brazil, 05508-090 email: [email protected]
T. I. Gombosi
Affiliation:
University of Michigan, 1517 Space Research Building, Ann Arbor, MI, USA, 48109-2143
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Abstract

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We investigate magnetized solar-like stellar winds by means of self-consistent three-dimensional (3D) magnetohydrodynamics (MHD) numerical simulations. We analyze winds with different magnetic field intensities and densities as to explore the dependence on the plasma-β parameter. By solving the fully ideal 3D MHD equations, we show that the plasma-β parameter is the crucial parameter in the configuration of the steady-state wind. Therefore, there is a group of magnetized flows that would present the same terminal velocity despite of its thermal and magnetic energy densities, as long as the plasma-β parameter is the same.

Keywords

Stars: coronae – stars: late-type – stars: magnetic fields – stars: mass loss
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 4 , Symposium S259: Cosmic Magnetic Fields: From Planets, to Stars and Galaxies , November 2008 , pp. 415 - 416
Copyright
Copyright © International Astronomical Union 2009

References

Low, B. C., & Tsinganos, K. 1986, ApJ 302, 163CrossRefGoogle Scholar
Pneuman, G. W. & Kopp, R. A. 1971, SP 18, 258, PK71Google Scholar
Powell, K. G. et al. 1999, J. of Comp. Phys. 154, 284CrossRefGoogle Scholar
Washimi, H. & Shibata, S. 1993, MNRAS 262, 936CrossRefGoogle Scholar
Wood, B. E. et al. 2005, ApJ 628, L143CrossRefGoogle Scholar