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Double plasma resonance instability as a source of solar zebra emission
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SYSNO ASEP 0494615 Druh ASEP J - Článek v odborném periodiku Zařazení RIV J - Článek v odborném periodiku Poddruh J Článek ve WOS Název Double plasma resonance instability as a source of solar zebra emission Tvůrce(i) Benáček, J. (CZ)
Karlický, Marian (ASU-R) RID, ORCIDČíslo článku A60 Zdroj.dok. Astronomy & Astrophysics. - : EDP Sciences - ISSN 0004-6361
Roč. 611, March (2018)Poč.str. 7 s. Forma vydání Online - E Jazyk dok. eng - angličtina Země vyd. FR - Francie Klíč. slova instabilities ; numerical methods ; radio radiation Vědní obor RIV BN - Astronomie a nebeská mechanika, astrofyzika Obor OECD Astronomy (including astrophysics,space science) CEP GA16-13277S GA ČR - Grantová agentura ČR GA17-16447S GA ČR - Grantová agentura ČR Institucionální podpora ASU-R - RVO:67985815 UT WOS 000428423300004 EID SCOPUS 85044820860 DOI 10.1051/0004-6361/201731424 Anotace First using the multi-mode model, we study details of the double plasma resonance instability. We show how the distribution function of hot electrons changes during this instability. Then we show that there is a very good agreement between results obtained by the multi-mode and specific-mode models, which is caused by a dominance of the wave with the maximal growth rate. Therefore, for computations in a broad range of model parameters, we use the specific-mode model. We compute the maximal growth rates of the double plasma resonance instability with a dependence on the ratio between the upper-hybrid omega(UH) and electron-cyclotron omega(ce) frequency. We vary temperatures of both the hot and background plasma components and study their effects on the resulting growth rates. The results are compared with the analytical ones. We find a very good agreement between numerical and analytical growth rates. We also compute saturation energies of the upper-hybrid waves in a very broad range of parameters. We find that the saturation energies of the upper-hybrid waves show maxima and minima at almost the same values of omega(UH) =omega(ce) as the growth rates, but with a higher contrast between them than the growth rate maxima and minima. Pracoviště Astronomický ústav Kontakt Radka Svašková, bibl@asu.cas.cz, Tel.: 323 620 326 Rok sběru 2019
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