Coronal Magnetic Fields in a Sunspot Plume at the Limb

Details Coronal Magnetic Fields in a Sunspot Plume at the Limb Coronal Magnetic Fields in a Sunspot Plume at the Limb

Dec 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003agufmsh42b0507b&link_type=abstract

American Geophysical Union, Fall Meeting 2003, abstract #SH42B-0507

Physics

7509 Corona, 7524 Magnetic Fields, 7534 Radio Emissions, 7549 Ultraviolet Emissions

Scientific paper

We obtained coordinated EUV and radio observations of NOAA Active Region 10139 on 2002 October 14 when the region was on the west limb of the Sun. Observations were obtained with the Very Large Array (VLA) and three instruments aboard the Solar and Heliospheric Observatory (SOHO) satellite, including the Coronal Diagnostic Spectrometer (CDS), the Extreme-ultraviolet Imaging Telescope (EIT), and the Michelson Doppler Imager (MDI). A sunspot plume is clearly seen in EUV emission lines formed at temperatures between about 0.2 and 0.5 MK. Polarized 8 GHz radio emission from the plume suggests 4th harmonic gyroemission (from 760 Gauss fields) above the limb, and 3rd harmonic gyroemission (from 960 Gauss fields) on the disk.

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