Double plasma resonance instability as a source of solar zebra emission

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A_____%2F18%3A00494615" target="_blank" >RIV/67985815:_____/18:00494615 - isvavai.cz</a>

Nalezeny alternativní kódy

RIV/00216224:14310/18:00106703

Výsledek na webu

<a href="http://dx.doi.org/10.1051/0004-6361/201731424" target="_blank" >http://dx.doi.org/10.1051/0004-6361/201731424</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1051/0004-6361/201731424" target="_blank" >10.1051/0004-6361/201731424</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Double plasma resonance instability as a source of solar zebra emission

Popis výsledku v původním jazyce

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.

Název v anglickém jazyce

Double plasma resonance instability as a source of solar zebra emission

Popis výsledku anglicky

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.

Druh

J_imp - Článek v periodiku v databázi Web of Science

CEP obor

—

OECD FORD obor

10308 - Astronomy (including astrophysics,space science)

Projekt

Výsledek vznikl pri realizaci vícero projektů. Více informací v záložce Projekty.

Návaznosti

P - Projekt vyzkumu a vyvoje financovany z verejnych zdroju (s odkazem do CEP)

Rok uplatnění

2018

Kód důvěrnosti údajů

S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů

Název periodika

Astronomy & Astrophysics

ISSN

1432-0746

e-ISSN

—

Svazek periodika

611

Číslo periodika v rámci svazku

March

Stát vydavatele periodika

FR - Francouzská republika

Počet stran výsledku

7

Strana od-do

—

Kód UT WoS článku

000428423300004

EID výsledku v databázi Scopus

2-s2.0-85044820860