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Chains of type-I radio bursts and drifting pulsation structures
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SYSNO ASEP 0479161 Document Type J - Journal Article R&D Document Type Journal Article Subsidiary J Článek ve WOS Title Chains of type-I radio bursts and drifting pulsation structures Author(s) Karlický, Marian (ASU-R) RID, ORCID Source Title Astronomy & Astrophysics. - : EDP Sciences - ISSN 0004-6361
Roč. 602, June (2017), A122/1-A122/7Number of pages 7 s. Publication form Online - E Language eng - English Country FR - France Keywords Sun activity ; radio radiation ; flares Subject RIV BN - Astronomy, Celestial Mechanics, Astrophysics OECD category Astronomy (including astrophysics,space science) R&D Projects GA16-13277S GA ČR - Czech Science Foundation (CSF) GA17-16447S GA ČR - Czech Science Foundation (CSF) Institutional support ASU-R - RVO:67985815 UT WOS 000404648300039 EID SCOPUS 85021637928 DOI 10.1051/0004-6361/201629652 Annotation Owing to similarities of chains of type-I radio bursts and drifting pulsation structures the question arises as to whether both these radio bursts are generated by similar processes. Characteristics and parameters of both these radio bursts are compared. We present examples of both types of bursts and show their similarities and di ff erences. Then, for chains of type-I bursts, a similar model as for drifting pulsation structures (DPSs) is proposed. We show that, similar to the DPS model, the chains of type-I bursts can be generated by the fragmented magnetic reconnection associated with plasmoid interactions. To support this new model of chains of type-I bursts, we present an e ff ect of merging two plasmoids to form one larger plasmoid on the radio spectrum of DPS. This process can also explain the ` wavy' appearance of some chains of type-I bursts. Further, we show that the chains of type-I bursts with the wavy appearance can be used for estimation of the magnetic field strength in their sources. We think that di ff erences of chains of type-I bursts and DPSs are mainly owing to di ff erent regimes of the magnetic field reconnection. While in the case of chains of type-I bursts, the magnetic reconnection and plasmoid interactions are in the quasi-separatrix layer of the active region in more or less quasi-saturated regime, in the case of DPSs, observed in the impulsive phase of eruptive flares, the magnetic reconnection and plasmoid interactions are in the current sheet formed under the flare magnetic rope, which moves upwards and forces this magnetic reconnection. Workplace Astronomical Institute Contact Radka Svašková, bibl@asu.cas.cz, Tel.: 323 620 326 Year of Publishing 2018
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