The microwave structure of quiescent solar filaments at high resolution.

Details The microwave structure of quiescent solar filaments at high resolution. The microwave structure of quiescent solar filaments at high resolution.

Dec 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986nascp2442..121g&link_type=abstract

NASA Conf. Publ., NASA CP-2442, p. 121 - 125

Physics

1

Solar Filaments:Vla Observations

Scientific paper

The author presents high resolution VLA maps of a quiescent filament at three frequencies. At each frequency, the filament appears as a depression in the quiet Sun background. The depression is measurably wider and longer in extent than the corresponding Hα filament at 1.45 GHz and 4.9 GHz, indicating that the depression is due in large part to a deficit in coronal density associated with the filament channel. In contrast, the shape of the radio depression at 15 GHz closely matches that of the Hα filament. In addition, the 15 GHz map shows enhanced emission along both sides of the radio depression. A similar enhancement is seen in an observation of a second filament obtained 4 days later, which suggests that the enhancement is a general feature of filaments. Possible causes of the enhanced emission are explored.

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