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Separation of solar radio bursts in a complex spectrum

Published online by Cambridge University Press:  08 June 2011

Hana Mészárosová ,
Ján Rybák ,
Marian Karlický  and
Karel Jiřička
Hana Mészárosová
Affiliation:
Astronomical Institute of the Academy of Sciences, CZ-25165 Ondřejov, Czech Republic email: hana@asu.cas.cz
Ján Rybák
Affiliation:
Astronomical Institute, Slovak Academy of Sciences, SK-05960 Tatranská Lomnica, Slovak Republic email: choc@ta3.sk
Marian Karlický
Affiliation:
Astronomical Institute of the Academy of Sciences, CZ-25165 Ondřejov, Czech Republic email: hana@asu.cas.cz
Karel Jiřička
Affiliation:
Astronomical Institute of the Academy of Sciences, CZ-25165 Ondřejov, Czech Republic email: hana@asu.cas.cz
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Abstract

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Radio spectra, observed during solar flares, are usually very complex (many bursts and fine structures). We have developed a new method to separate them into individual bursts and analyze them separately. The method is used in the analysis of the 0.8–2.0 GHz radio spectrum of the April 11, 2001 event, which was rich in drifting pulsating structures (DPSs). Using this method we showed that the complex radio spectrum consists of at least four DPSs separated with respect to their different frequency drifts (−115, −36, −23, and −11 MHz s−1). These DPSs indicate a presence of at least four plasmoids expected to be formed in a flaring current sheet. These plasmoids produce the radio emission on close frequencies giving thus a mixture of superimposed DPSs observed in the radio spectrum.

Keywords

Sun: coronaSun: flaresSun: radio radiationSun: oscillations
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S274: Advances in Plasma Astrophysics , September 2010 , pp. 150 - 152
Copyright
Copyright © International Astronomical Union 2011

References

Bárta, M., Karlický, M. & Žemlička, R. 2008, Solar Phys., 253, 173CrossRefGoogle Scholar
Jiřička, K., Karlický, M., Kepka, O., & Tlamicha, A. 1993, Solar Phys., 147, 203CrossRefGoogle Scholar
Karlický, M. & Odstrčil, D. 1994, Solar Phys., 155, 171CrossRefGoogle Scholar
Karlický, M., Fárník, F., & Mészárosová, H. 2002, A&A, 395, 677Google Scholar
Karlický, M. 2004, A&A, 417, 325Google Scholar
Karlický, M. & Bárta, M. 2007, A&A, 464, 735Google Scholar
Karlický, M., Bárta, M., & Rybák, J. 2010, A&A, 514, A28Google Scholar
Kliem, B., Karlický, M., & Benz, A. O. 2000, A&A, 360, 715Google Scholar
Mészárosová, H., Rybák, J., & Karlický, M. 2010, A&A, submittedGoogle Scholar
Ohyama, M. & Shibata, K. 1998, ApJ, 499, 934CrossRefGoogle Scholar
Reiner, M. J., Klein, K. L., Karlický, M., et al. . 2008, Solar Phys., 249, 337CrossRefGoogle Scholar
Shibata, K. & Tanuma, S. 2001, Earth, Planets and Space, 53, 473CrossRefGoogle Scholar