Measurements of Magnetic Reconnection Rates and Inferred Coronal Electric Fields in Solar Active Regions from Simultaneous SOHO/MDI and TRACE observations

Details Measurements of Magnetic Reconnection Rates and Inferred Coronal Electric Fields in Solar Active Regions from Simultaneous SOHO/MDI and TRACE observations Measurements of Magnetic Reconnection Rates and Inferred Coronal Electric Fields in Solar Active Regions from Simultaneous SOHO/MDI and TRACE observations

May 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agusm..sh41a08g&link_type=abstract

American Geophysical Union, Spring Meeting 2001, abstract #SH41A-08

Astronomy and Astrophysics

Astrophysics

7500 Solar Physics, Astrophysics, And Astronomy

Scientific paper

One of the long-standing issues in coronal physics is the lack of solid constraints on parameters that are fundamental to realistic models of magnetic reconnection. For example, the electric field strength above solar active regions is generally unknown, although it has been estimated to about a factor of two (Forbes and Lin 2000) in a specific large flare (Poletto and Kopp 1986). Recently, high resolution high cadence UV and EUV observations from the Transition Region and Coronal Explorer (TRACE) together with high quality magnetograms from the Michelson Doppler Imager (MDI) on SOHO provide an opportunity to approach this problem. These observations allow measuremenents of the rate of magnetic reconnection, which may be converted (using simple geometric models of the coronal fields) to electric fields in the reconnection region. We use the MDI and TRACE data archives to choose simultaneous TRACE observations and MDI high-resolution magnetograms of active regions near disk center. We create movies with these data to investigate reconnection rates in various coronal transient events. Some earlier La Palma high resolution observations in H-alpha showing reconnection rates may also be presented. This work was supported by NASA contracts NAG5-8878 (MDI) and NAS5-38099 (TRACE).

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