Centimeter-wave radio emission of a high-latitude prominence

Details Centimeter-wave radio emission of a high-latitude prominence Centimeter-wave radio emission of a high-latitude prominence

Mar 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008astbu..63...34g&link_type=abstract

Astrophysical Bulletin, Volume 63, Issue 1, pp.34-42

Astronomy and Astrophysics

Astrophysics

1

95.85.-E, 96.60.Qf

Scientific paper

The results of observations of the radio emission of a high-latitude prominence located in the NE part of the solar limb are discussed. Observations were performed on the radio telescope RATAN-600 using its Northeastern sector and Southern sector with a periscope during the maximum phase (0.998) of the solar eclipse of March 29, 2006. The prominence was studied in the wavelength interval 1.03 ÷ 5.0 cm. The absence of the background illumination from the solar disk allowed us to study the parameters of the radio emission of the high-latitude prominence ( ϕ = 45°, NE limb of the Sun). Observations of the solar limb at the time of the maximum phase made it possible to record very small radio fluxes from the prominence, which amounted to 0.05 ÷ 0.01 s.f.u. in the wavelength interval from 1.84 to 5.0 cm. The position of the maximum of the radio emission of the prominence coincides, according to the results of observations performed on both sectors, with the summit of the prominence as seen on the solar image taken in the He II 304 Å line (SOHO, ϕ = 45°, NE limb of the Sun). The degree of polarization is P ≈ 7 ÷ 16% at 1.88 ÷ 5.0 cm. If interpreted in terms of the thermal mechanism considered here, polarized emission corresponds to a magnetic-field strength of H ≅ (550 ÷ 100) G in the prominence region.

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