Physics
Scientific paper
Jan 1999
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999soph..184..103h&link_type=abstract
Solar Physics, v. 184, Issue 1, p. 103-111 (1999).
Physics
9
Scientific paper
Magnetic dips are generally assumed to be basic equilibrium configurations in quiescent solar prominences. Here we discuss two types of the magnetic dips which were considered in the literature: (1)dips resulting from a force-free magnetic equilibrium in the corona, and (2)magnetic dips which are formed in situations where the Lorentz force balances the weight of the prominence plasma. An important parameter which decides between these two cases is the plasma beta. For beta<<<1, the effect of the prominence material on the equilibrium structure is quite negligible and the case (1)holds. If, however, beta is larger, say between 0.1 and 1 or even higher, magnetic dips of the second kind are formed and they can be characterized by the angle psi1 between the vertical and the direction of the field lines at the surface of the prominence structure. A simple and illustratory formula is derived to relate this angle to the plasma beta at the prominence center, namely betac~=cot2psi1. betac=1 thus corresponds to psi1=45 deg. Finally, we discuss the range of values of both betac and psi1 as deduced from various observations and conclude that the dips of the second kind are important for the prominence equilibria. We also suggest a new method for determination of the field-line inclination.
Anzer Ulrich
Heinzel Petr
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