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Issue A&A
Volume 507, Number 2, November IV 2009
Page(s) 611 - 616
Section Astrophysical processes
DOI http://dx.doi.org/10.1051/0004-6361/200912432
Published online 15 September 2009

A&A 507, 611-616 (2009)
DOI: 10.1051/0004-6361/200912432

Characteristics of magnetised plasma flow around stationary and expanding magnetic clouds

G. Dalakishvili1, S. Poedts1, H. Fichtner2, and E. Romashets3

1  Centre for Plasma Astrophysics, K.U.Leuven, Celestijnenlaan 200B, 3001 Leuven, Belgium
    e-mail: Giorgi.Dalakishvili@wis.kuleuven.be
2  Institut für Weltraum und Astrophysik, Ruhr-Universität Bochum, Universitätsstrasse 150, 44780 Bochum, Germany
3  Solar Observatory of Prairie View A & M University, Prairie View, TX 77446, USA

Received 6 May 2009 / Accepted 4 September 2009

Abstract
Aims. Studies of interplanetary magnetic clouds have shown that the characteristics of the region ahead of these objects, which are moving away from the Sun in the solar wind, play a role in determining their geo-efficiency, i.e. the kind and the degree of their effects on the Earth environment. Therefore, our main goal is to model and study the plasma parameters in the vicinity of interplanetary magnetic clouds.
Methods. To this end we present a model in which the magnetic clouds are immersed in a magnetised plasma flow with a homogeneous magnetic field. We first calculate the resulting distortion of the external magnetic field and then determine the plasma velocity by employing the frozen-in condition.
Results. Subsequently, the plasma density and pressure are expressed as functions of the magnetic field and the velocity field.
Conclusions. The plasma flow parameters are determined by solving the time-independent ideal MHD equations for both the stationary regime and for the case of an expanding cylindrical magnetic cloud, thus extending previous results that appeared in the literature.


Key words: magnetohydrodynamics (MHD) -- magnetic fields -- plasmas -- Sun: solar wind



© ESO 2009


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