[Previous] | [Session 39] | [Next]

[39.06] Magnetic Topology, Flux Emergence/Reconnection and Velocities from a Magnetic Charge Topology Model for Solar Active Regions

G. Barnes (NWRA/CoRA), D.W. Longcope (MSU), K.D. Leka (NWRA/CoRA)

Magnetic Charge Topology (MCT) models represent the field in the solar corona as being due to collection of point magnetic charges located at or below the photosphere. These models have the advantage of providing a simple quantitative description of the field topology. We apply MCT to time series of magnetograms from the U. Hawai`i/Mees Solar Observatory Imaging Vector Magnetograph (IVM). We first describe the evolution of the magnetic topology of the region, by calculating such quantities as the magnetic flux connecting each pair of point sources, and the number and locations of magnetic separators, which are likely to be the location of reconnection in the solar corona. Using the changes in the magnitudes of the point sources, and in the connectivity matrix, we estimate the rate at which flux is emerging and submerging through the photosphere, and the rate at which reconnection is happening in the corona. By tracking the changes in the locations of the sources, we are also able to estimate the horizontal velocities.

This work was performed under Air Force Office of Scientific Research contracts F49620-03-C-0019 and F49620-02-C-0191.

[Previous] | [Session 39] | [Next]

Bulletin of the American Astronomical Society, 36 #2
© YEAR. The American Astronomical Soceity.