Physics – Plasma Physics
Scientific paper
Oct 2000
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000aps..dppwo2005u&link_type=abstract
American Physical Society, 42nd Annual Meeting of the APS Division of Plasma Physics combined with the 10th International Congre
Physics
Plasma Physics
Scientific paper
Magnetic interaction between a star and an accretion disk can have a strong effect on the disk structure and on the angular momentum and mass transfer between the disk and the star. In this paper we study the time evolution of the magnetic field configuration caused by the relative rotation between the disk and the star. First, assuming ideal MHD everywhere, including both the stellar and the disk surfaces, we analyze the self-similar model for a uniformly rotating disk. In this model the magnetic field inflates on the rotation time scale and tends to open up in a finite time. We then consider additional physical processes that can remove the singularity, such as the finite disk resistivity and the inertial and reconnection effects in the magnetosphere. We also derive the condition for the existence of a steady state for a resistive disk. Finally, we generalize our analysis of the opening of magnetic field lines by using a non-self-similar numerical model that applies to an arbitrarily rotating (e.g. keplerian) disk.
Konigl Arieh
Litwin Christof
Uzdensky Dmitri
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