HR: 1330h
AN: SH42B-0507    [PDF]
TI: Coronal Magnetic Fields in a Sunspot Plume at the Limb
AU: * Brosius, J W
EM: brosius@comstoc.gsfc.nasa.gov
AF: Catholic University of America, Code 682 NASA's GSFC, Greenbelt, MD 20771 United States
AU: White, S M
EM: white@astro.umd.edu
AF: University of Maryland, Department of Astronomy, College Park, MD 20742 United States
AB: 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.
DE: 7509 Corona
DE: 7524 Magnetic fields
DE: 7534 Radio emissions
DE: 7549 Ultraviolet emissions
SC: SPA - Solar and Heliospheric Physics [SH]
MN: 2003 Fall Meeting