Coronal Sunspot Magnetic Fields: Extrapolation vs. Direct Observation

Details Coronal Sunspot Magnetic Fields: Extrapolation vs. Direct Observation Coronal Sunspot Magnetic Fields: Extrapolation vs. Direct Observation

May 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agusm..sh31d03l&link_type=abstract

American Geophysical Union, Spring Meeting 2001, abstract #SH31D-03

Physics

7509 Corona, 7524 Magnetic Fields, 7529 Photosphere, 7534 Radio Emissions, 7594 Instruments And Techniques

Scientific paper

Direct observations of the coronal magnetic field strength is presently only available using radio wavelengths. It is, however, common to infer the morphology of coronal magnetic fields by extrapolating in height from observations of photospheric magnetic fields. Both methods have sources of uncertainty, and neither presently results in the quantitative coronal vector magnetic field measurements required to understand coronal dynamics. In this paper we combine radio (VLA) observations of a region containing a large spot with simultaneous highly accurate photospheric vector magnetic field measurements obtained with the NSO/HAO Advanced Stokes Polarimeter and investigate the coronal response to changes in the photospheric magnetic field as NOAA AR8535 (May 1999) crossed the solar disk.

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