Origin of the submillimeter radio emission during the time-extended phase of a solar flare

Página do item simplificado
dc.contributor.authorTrottet G.
dc.contributor.authorRaulin J.-P.
dc.contributor.authorGimenez De Castro G.
dc.contributor.authorLuthi T.
dc.contributor.authorCaspi A.
dc.contributor.authorMandrini C.H.
dc.contributor.authorLuoni M.L.
dc.contributor.authorKaufmann P.
dc.date.accessioned2024-03-13T01:08:06Z
dc.date.available2024-03-13T01:08:06Z
dc.date.issued2012
dc.description.abstract© Springer Science+Business Media New York 2012. All rights are reserved.Solar flares observed in the 200∈-∈400 GHz radio domain may exhibit a slowly varying and time-extended component which follows a short (few minutes) impulsive phase and can last for a few tens of minutes to more than one hour. The few examples discussed in the literature indicate that such long-lasting submillimeter emission is most likely thermal bremsstrahlung. We present a detailed analysis of the time-extended phase of the 27 October 2003 (M6.7) flare, combining 1∈-∈345 GHz total-flux radio measurements with X-ray, EUV, and Hα observations. We find that the time-extended radio emission is, as expected, radiated by thermal bremsstrahlung. Up to 230 GHz, it is entirely produced in the corona by hot and cool materials at 7∈-∈16 MK and 1∈-∈3 MK, respectively. At 345 GHz, there is an additional contribution from chromospheric material at a few 104 K. These results, which may also apply to other millimeter-submillimeter radio events, are not consistent with the expectations from standard semiempirical models of the chromosphere and transition region during flares, which predict observable radio emission from the chromosphere at all frequencies where the corona is transparent.
dc.description.firstpage33
dc.description.lastpage55
dc.description.volume9781461444039
dc.identifier.doi10.1007/978-1-4614-4403-9_3
dc.identifier.urihttps://dspace.mackenzie.br/handle/10899/36810
dc.relation.ispartofEnergy Storage and Release through the Solar Activity Cycle: Models Meet Radio Observations
dc.rightsAcesso Restrito
dc.subject.otherlanguageactive
dc.subject.otherlanguageassociation with flares
dc.subject.otherlanguageassociation with flares
dc.subject.otherlanguageChromosphere
dc.subject.otherlanguageFlares
dc.subject.otherlanguagemicrowave
dc.subject.otherlanguageRadio bursts
dc.subject.otherlanguageRadio bursts
dc.subject.otherlanguagerelation to magnetic field
dc.subject.otherlanguageX-ray bursts
dc.titleOrigin of the submillimeter radio emission during the time-extended phase of a solar flare
dc.typeCapítulo de livro
local.scopus.citations1
local.scopus.eid2-s2.0-84949179986
local.scopus.subjectactive
local.scopus.subjectChromosphere
local.scopus.subjectFlares
local.scopus.subjectRadio bursts
local.scopus.subjectX-ray bursts
local.scopus.updated2024-05-01
local.scopus.urlhttps://www.scopus.com/inward/record.uri?partnerID=HzOxMe3b&scp=84949179986&origin=inward
Arquivos
Coleções
Livro e Capítulo de livro