Microwave emission and polarization of a flaring loop

Details Microwave emission and polarization of a flaring loop Microwave emission and polarization of a flaring loop

Oct 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984a%26a...139..507a&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 139, no. 2, Oct. 1984, p. 507-511.

Astronomy and Astrophysics

Astrophysics

38

Coronal Loops, Microwave Emission, Polarization Characteristics, Solar Flares, Solar Radio Bursts, Brightness Temperature, Solar Activity Effects, Stellar Models

Scientific paper

The authors present computations of the microwave emission from a loop filled with accelerated electrons. At short wavelengths the loop is optically thin and the emission comes predominantly from the feet of the loop, while at long wavelengths the emission comes from the entire loop with a maximum near the top. If the loop is not located at the center of the solar disk the observed polarization is greatly affected by propagation effects in the corona which may change the sense of the circular polarization (V). For the adopted model and for a loop located 30° away from the center of the disk the sense of V corresponds to the direction of the magnetic field in the region of emission only for wavelengths much shorter than 1.4 cm; for wavelengths much longer than 7.5 cm the sense of V corresponds to the polarity of the field at the diskward foot of the loop.

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