34th Solar Physics Division Meeting, June 2003
Session 11 Photosphere and Chormosphere II
Oral, Tuesday, June 17, 2003, 1:30-3:30pm, Auditorium

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[11.05] Predictions of Heating Rates in Localized Magnetic Structures From The Photosphere To The Upper Chromosphere

M. L. Goodman (Institute for Scientific Research, Fairmont, WV)

The heating rates due to resistive dissipation of magnetic field aligned currents and of Pedersen currents are computed as functions of height and horizontal radius in a specified 2.5 D magnetic field from the photosphere to the upper chromosphere. The model uses the VAL C height dependent profiles of temperature, and electron, proton, hydrogen, helium, and heavy ion densities together with the magnetic field to compute the anisotropic electrical conductivity tensor for each charged particle species. The magnetic field is parameterized by its maximum magnitude B0, scale height L, characteristic diameter D0, and twist \tau which is the ratio of the azimuthal field component to the radial field component. The objective is to determine the ranges of values of these parameters that yield heating rates that are within observational constraints for values of D0 that are above and below the resolution limit of ~150 km. This provides a test of the proposition that Pedersen current dissipation is a major source of chromopsheric heating in magnetic structures throughout the chromosphere, and that it is the rapid increase of charged particle magnetization with height in the lower chromosphere that causes the chromospheric temperature inversion and the rapid increase of the heating rate per unit mass with height in this region. It is found that the heating rate is a monotonically increasing function of B0, L, and \tau, and a monotonically decreasing function of D0. For values of D0 below the resolution limit, values of \tau >> 1 correspond to strongly heated magnetic structures.

This work was supported by NSF grant ATM 9816335.


The author(s) of this abstract have provided an email address for comments about the abstract: mgoodman@isr.us

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