Quasi-periodic Fast-mode Magnetosonic Wave Trains Within Coronal Waveguides Associated with Flares and CMEs

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A_____%2F16%3A00472820" target="_blank" >RIV/67985815:_____/16:00472820 - isvavai.cz</a>

Výsledek na webu

<a href="http://dx.doi.org/10.1063/1.4943821" target="_blank" >http://dx.doi.org/10.1063/1.4943821</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1063/1.4943821" target="_blank" >10.1063/1.4943821</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Quasi-periodic Fast-mode Magnetosonic Wave Trains Within Coronal Waveguides Associated with Flares and CMEs

Popis výsledku v původním jazyce

Quasi-periodic, fast-mode, propagating wave trains (QFPs) are a new observational phenomenon recently discovered in the solar corona by the Solar 11)ynamics Observatory with extreme ultraviolet (EUV) imaging observations. They originate from flares and propagate at speeds up to similar to 2000 km s(-1) within funnel-shaped waveguides in the wakes of coronal mass ejections (CMEs). QFPs can carry sufficient energy fluxes required for coronal heating during their occurrences. They can provide new diagnostics for the solar corona and their associated flares. We present recent observations of QFPs focusing on their spatio-temporal properties, temperature dependence, and statistical correlation with flares and CMEs. Of particular interest is the 2010-Aug-01 C3.2 flare with correlated QFPs and drifting zebra and fiber radio bursts, which might be different manifestations of the same fast-mode wave trains. We also discuss the potential roles of QFPs in accelerating and/or modulating the solar wind.

Název v anglickém jazyce

Quasi-periodic Fast-mode Magnetosonic Wave Trains Within Coronal Waveguides Associated with Flares and CMEs

Popis výsledku anglicky

Quasi-periodic, fast-mode, propagating wave trains (QFPs) are a new observational phenomenon recently discovered in the solar corona by the Solar 11)ynamics Observatory with extreme ultraviolet (EUV) imaging observations. They originate from flares and propagate at speeds up to similar to 2000 km s(-1) within funnel-shaped waveguides in the wakes of coronal mass ejections (CMEs). QFPs can carry sufficient energy fluxes required for coronal heating during their occurrences. They can provide new diagnostics for the solar corona and their associated flares. We present recent observations of QFPs focusing on their spatio-temporal properties, temperature dependence, and statistical correlation with flares and CMEs. Of particular interest is the 2010-Aug-01 C3.2 flare with correlated QFPs and drifting zebra and fiber radio bursts, which might be different manifestations of the same fast-mode wave trains. We also discuss the potential roles of QFPs in accelerating and/or modulating the solar wind.

Druh

D - Stať ve sborníku

CEP obor

BN - Astronomie a nebeská mechanika, astrofyzika

OECD FORD obor

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Projekt

<a href="/cs/project/GAP209%2F12%2F0103" target="_blank" >GAP209/12/0103: Rádiová a rentgenová diagnostika procesů primárního uvolňování energie ve slunečních erupcích a jejich numerické simulace</a><br>

Návaznosti

I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace

Rok uplatnění

2016

Kód důvěrnosti údajů

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

Název statě ve sborníku

Solar Wind 14: Proceedings of the Fourteenth International Solar Wind Conference

ISBN

9780735413672

ISSN

0094-243X

e-ISSN

—

Počet stran výsledku

4

Strana od-do

"040010/1"-"040010/4"

Název nakladatele

American Institute of Physics

Místo vydání

Melville

Místo konání akce

Weihai

Datum konání akce

22. 6. 2015

Typ akce podle státní příslušnosti

WRD - Celosvětová akce

Kód UT WoS článku

000392692000021