Close Association of an Extreme-Ultraviolet Sunspot Plume with Depressions in the Sunspot Radio Emission

Details Close Association of an Extreme-Ultraviolet Sunspot Plume with Depressions in the Sunspot Radio Emission Close Association of an Extreme-Ultraviolet Sunspot Plume with Depressions in the Sunspot Radio Emission

Jan 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004apj...601..546b&link_type=abstract

The Astrophysical Journal, Volume 601, Issue 1, pp. 546-558.

Astronomy and Astrophysics

Astronomy

8

Sun: Corona, Sun: Magnetic Fields, Sun: Radio Radiation, Sun: Transition Region, Sun: Uv Radiation, Sun: Sunspots

Scientific paper

We obtained coordinated observations of the large sunspot in NOAA Region 8539 on 1999 May 9 and 13 with the Very Large Array and three instruments (CDS, EIT, MDI) aboard the Solar and Heliospheric Observatory satellite. The EUV observations reveal a plume in the sunspot umbra on both observing dates. The plume appears brightest in emission lines formed at temperatures between 1.6×105 and 5.0×105 K. Radio emission from the sunspot umbra is dominated by thermal gyroemission from the plume, which accounts for radio brightness temperatures <1×106 K in the umbra on both dates, as well as umbral brightness temperature depressions in the 4.535 and 8.065 GHz observations on May 13. A compact 14.665 GHz source persists near the umbra/penumbra boundary during our observing period, indicating a long-lived, compact flux tube with coronal magnetic field strength of at least 1748 G. It occurs in a portion of the sunspot that appears very dark in EUV emission.

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