A study of eruptive solar events with negative radio bursts

• Published in: Astronomy reports Vol. 53; no. 11; pp. 1039 - 1049
• Main Authors: Kuz’menko, I. V., Grechnev, V. V., Uralov, A. M.
• Format: Journal Article
• Language: English
• Published: Dordrecht SP MAIK Nauka/Interperiodica 01-11-2009; Springer Nature B.V
• Subjects: Absorption; Astronomy; Background radiation; Corona; Emissions; Magnetic fields; Observations and Techniques; Physics; Physics and Astronomy; Radio astronomy; Sun; 96.60.qf
• ISSN: 1063-7729; 1562-6881
• DOI: 10.1134/S1063772909110092

Solar events of June 15/16, 2000, June 1/2, 2002, February 6, 2002, and February 7, 2002, have been studied. These events probably belong to a poorly studied class of explosive eruptions. In such events disintegration of the magnetic structure of an eruptive filament and dispersing of its fragments as a cloud over a considerable part of the solar surface are possible. The analysis of SOHO/EIT extreme ultraviolet images obtained in the 195 Å and 304 Å channels has revealed the appearance of dimmings of various shapes and propagation of a coronal wave for June 1/2, 2002. In all the events the Nobeyama, Learmonth, and Ussuriysk observatories recorded negative radio bursts at several frequencies in the 1–10 GHz range. Most likely, these bursts were due to absorption of solar radio emission in clouds produced by fragments of filaments. Absorption of the solar background radiation can be observed as a depression of the emission in the 304 Å channel. A model has been developed, which permits one to estimate parameters of absorbing plasma such as temperature, optical thickness, area of the absorbing cloud, and its height above the chromosphere from the radio absorption observed at several frequencies. The obtained values of the temperature, 8000–9000 K, demonstrate that the absorber was the material of an erupted cool filament. The model estimate of the masses of the ejecta in the considered events were ∼10
15
g, which is comparable to masses of typical filaments and coronal mass ejections.