Coronal signatures of flare generated fast-mode wave at EUV and radio wavelengths

2024
journal article
article
dc.abstract.enThis paper presents a detailed study of the type II solar radio burst that occurred on 06 March 2014 using combined data analysis. It is a classical radio event consisting of type III radio burst and a following type II radio burst in the dynamic spectrum. The type II radio burst is observed between 235 – 130 MHz (120 – 60 MHz) in harmonic (fundamental) bands with the life time of 5 minutes between 09:26 – 09:31 UT. The estimated speed of type II burst by applying two-fold Saito model is ∼ 650 km s$^{−1}$. An extreme ultraviolet (EUV) wave is observed with Atmospheric Imaging Assembly (AIA) onboard the Solar Dynamics Observatory (SDO). The very close temporal onset association of the EUV wave and flare energy release indicates that the EUV wave is likely produced by a flare pressure pulse. The eruption is also accompanied by a weak coronal mass ejection (CME) observed with the coronagraphs onboard the Solar and Heliospheric Observatory (SOHO) and the twin Solar Terrestrial Relations Observatory (STEREO). The plane of sky speed of the CME was ∼ 252 km s$^{−1}$ in the SOHO/LASCO-C2 and ∼ 280 km s$^{−1}$ in the STEREO-B/SECCHI-COR1 images. The EUV wave has two wave fronts, one expanding radially outward and the other one moving along the flare loop arcade. The source position of the type II burst imaged by the Nançay Radio Heliograph (NRH) shows that it was associated with the outward moving EUV wave. The CME is independent of the shock wave as confirmed by the location of NRH radio sources below the CME’s leading edge. Therefore the type II radio burst is probably ignited by the flare. This study shows the possibility of EUV wave and coronal shock triggered by flare pressure pulse, generating the observed type II radio burst.
dc.affiliationWydział Fizyki, Astronomii i Informatyki Stosowanej : Instytut – Obserwatorium Astronomiczne
dc.contributor.authorVeluchamy, Vasanth - 464067
dc.date.accessioned2024-05-24T14:45:17Z
dc.date.available2024-05-24T14:45:17Z
dc.date.issued2024
dc.date.openaccess0
dc.description.accesstimew momencie opublikowania
dc.description.number5
dc.description.versionostateczna wersja wydawcy
dc.description.volume299
dc.identifier.articleid63
dc.identifier.doi10.1007/s11207-024-02293-z
dc.identifier.issn0038-0938
dc.identifier.urihttps://ruj.uj.edu.pl/handle/item/342899
dc.languageeng
dc.language.containereng
dc.rightsUdzielam licencji. Uznanie autorstwa 4.0 Międzynarodowa
dc.rights.licenceCC-BY
dc.rights.urihttp://creativecommons.org/licenses/by/4.0/legalcode.pl
dc.share.typeinne
dc.subject.entype II radio bursts
dc.subject.enflares
dc.subject.encoronal mass ejections (CMEs)
dc.subject.enshocks
dc.subtypeArticle
dc.titleCoronal signatures of flare generated fast-mode wave at EUV and radio wavelengths
dc.title.journalSolar Physics
dc.typeJournalArticle
dspace.entity.typePublicationen
dc.abstract.en
This paper presents a detailed study of the type II solar radio burst that occurred on 06 March 2014 using combined data analysis. It is a classical radio event consisting of type III radio burst and a following type II radio burst in the dynamic spectrum. The type II radio burst is observed between 235 – 130 MHz (120 – 60 MHz) in harmonic (fundamental) bands with the life time of 5 minutes between 09:26 – 09:31 UT. The estimated speed of type II burst by applying two-fold Saito model is ∼ 650 km s$^{−1}$. An extreme ultraviolet (EUV) wave is observed with Atmospheric Imaging Assembly (AIA) onboard the Solar Dynamics Observatory (SDO). The very close temporal onset association of the EUV wave and flare energy release indicates that the EUV wave is likely produced by a flare pressure pulse. The eruption is also accompanied by a weak coronal mass ejection (CME) observed with the coronagraphs onboard the Solar and Heliospheric Observatory (SOHO) and the twin Solar Terrestrial Relations Observatory (STEREO). The plane of sky speed of the CME was ∼ 252 km s$^{−1}$ in the SOHO/LASCO-C2 and ∼ 280 km s$^{−1}$ in the STEREO-B/SECCHI-COR1 images. The EUV wave has two wave fronts, one expanding radially outward and the other one moving along the flare loop arcade. The source position of the type II burst imaged by the Nançay Radio Heliograph (NRH) shows that it was associated with the outward moving EUV wave. The CME is independent of the shock wave as confirmed by the location of NRH radio sources below the CME’s leading edge. Therefore the type II radio burst is probably ignited by the flare. This study shows the possibility of EUV wave and coronal shock triggered by flare pressure pulse, generating the observed type II radio burst.
dc.affiliation
Wydział Fizyki, Astronomii i Informatyki Stosowanej : Instytut – Obserwatorium Astronomiczne
dc.contributor.author
Veluchamy, Vasanth - 464067
dc.date.accessioned
2024-05-24T14:45:17Z
dc.date.available
2024-05-24T14:45:17Z
dc.date.issued
2024
dc.date.openaccess
0
dc.description.accesstime
w momencie opublikowania
dc.description.number
5
dc.description.version
ostateczna wersja wydawcy
dc.description.volume
299
dc.identifier.articleid
63
dc.identifier.doi
10.1007/s11207-024-02293-z
dc.identifier.issn
0038-0938
dc.identifier.uri
https://ruj.uj.edu.pl/handle/item/342899
dc.language
eng
dc.language.container
eng
dc.rights
Udzielam licencji. Uznanie autorstwa 4.0 Międzynarodowa
dc.rights.licence
CC-BY
dc.rights.uri
http://creativecommons.org/licenses/by/4.0/legalcode.pl
dc.share.type
inne
dc.subject.en
type II radio bursts
dc.subject.en
flares
dc.subject.en
coronal mass ejections (CMEs)
dc.subject.en
shocks
dc.subtype
Article
dc.title
Coronal signatures of flare generated fast-mode wave at EUV and radio wavelengths
dc.title.journal
Solar Physics
dc.type
JournalArticle
dspace.entity.typeen
Publication
Affiliations

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