Astronomy and Astrophysics – Astronomy
Scientific paper
May 2003
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003spd....34.1105g&link_type=abstract
American Astronomical Society, SPD meeting #34, #11.05; Bulletin of the American Astronomical Society, Vol. 35, p.827
Astronomy and Astrophysics
Astronomy
Scientific paper
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 τ 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 τ , and a monotonically decreasing function of D0. For values of D0 below the resolution limit, values of τ >> 1 correspond to strongly heated magnetic structures.
This work was supported by NSF grant ATM 9816335.
No associations
LandOfFree
Predictions of Heating Rates in Localized Magnetic Structures From The Photosphere To The Upper Chromosphere does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with Predictions of Heating Rates in Localized Magnetic Structures From The Photosphere To The Upper Chromosphere, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Predictions of Heating Rates in Localized Magnetic Structures From The Photosphere To The Upper Chromosphere will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-987195