Počet záznamů: 1
Interplanetary Type III Bursts and Electron Density Fluctuations in the Solar Wind
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SYSNO ASEP 0489280 Druh ASEP J - Článek v odborném periodiku Zařazení RIV J - Článek v odborném periodiku Poddruh J Článek ve WOS Název Interplanetary Type III Bursts and Electron Density Fluctuations in the Solar Wind Tvůrce(i) Krupař, Vratislav (UFA-U) RID, ORCID
Maksimovic, M. (FR)
Kontar, E. P. (GB)
Zaslavsky, A. (FR)
Santolík, Ondřej (UFA-U) RID, ORCID
Souček, Jan (UFA-U) RID, ORCID
Krupařová, Oksana (UFA-U) RID, ORCID
Eastwood, J. P. (GB)
Szabo, A. (US)Celkový počet autorů 9 Číslo článku 82 Zdroj.dok. Astrophysical Journal - ISSN 0004-637X
Roč. 857, č. 2 (2018)Poč.str. 7 s. Forma vydání Online - E Jazyk dok. eng - angličtina Země vyd. US - Spojené státy americké Klíč. slova scattering ; Sun: radio radiation ; solar wind ; radio-burst Vědní obor RIV BL - Fyzika plazmatu a výboje v plynech Obor OECD Fluids and plasma physics (including surface physics) CEP GJ17-06818Y GA ČR - Grantová agentura ČR GA17-08772S GA ČR - Grantová agentura ČR GA17-06065S GA ČR - Grantová agentura ČR Institucionální podpora UFA-U - RVO:68378289 UT WOS 000430336500005 EID SCOPUS 85046377082 DOI 10.3847/1538-4357/aab60f Anotace Type III bursts are generated by fast electron beams originated from magnetic reconnection sites of solar flares. As propagation of radio waves in the interplanetary medium is strongly affected by random electron density fluctuations, type III bursts provide us with a unique diagnostic tool for solar wind remote plasma measurements. Here, we performed a statistical survey of 152 simple and isolated type III bursts observed by the twin-spacecraft Solar TErrestrial RElations Observatory mission. We investigated their time-frequency profiles in order to retrieve decay times as a function of frequency. Next, we performed Monte Carlo simulations to study the role of scattering due to random electron density fluctuations on time-frequency profiles of radio emissions generated in the interplanetary medium. For simplification, we assumed the presence of isotropic electron density fluctuations described by a power law with the Kolmogorov spectral index. Decay times obtained from observations and simulations were compared. We found that the characteristic exponential decay profile of type III bursts can be explained by the scattering of the fundamental component between the source and the observer despite restrictive assumptions included in the Monte Carlo simulation algorithm. Our results suggest that relative electron density fluctuations <delta n(e)>/n(e) in the solar wind are 0.06-0.07 over wide range of heliospheric distances. Pracoviště Ústav fyziky atmosféry Kontakt Kateřina Adamovičová, adamovicova@ufa.cas.cz, Tel.: 272 016 012 ; Kateřina Potužníková, kaca@ufa.cas.cz, Tel.: 272 016 019 Rok sběru 2019
Počet záznamů: 1