Center-to-Limb Variation of Solar Bursts Polarization at Millimeter Wavelengths

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dc.contributor.authorHidalgoRamirez R.F.
dc.contributor.authorMorosi A.
dc.contributor.authorSilva D.
dc.contributor.authorSimoes P.J.A.
dc.contributor.authorValio A.
dc.date.accessioned2024-03-12T23:52:18Z
dc.date.available2024-03-12T23:52:18Z
dc.date.issued2019
dc.description.abstract© 2019, Springer Nature B.V.Polarization of radio emission from solar flares provides essential information about plasma regimes confined to magnetic field in quiescent, pre-explosion, sudden energy release and decay phases. Observations of polarization are carried out continuously by the first time at two millimeter wavelengths of 6.67 and 3.34 mm (45 and 90 GHz, respectively) by two solar radio polarimeters named POEMAS operating at El Leoncito Observatory, Argentinian Andes. A total of 30 solar flares observed by the radio polarimeters, between 2012 and 2013, were analyzed. The degree of polarization was observed to increase and then decrease as the heliocentric angle increased. We found a weak correlation between the bursts’ flux density and their heliocentric angle, i.e. solar bursts with higher flux density slightly tend to occur near the limb.
dc.description.issuenumber8
dc.description.volume294
dc.identifier.doi10.1007/s11207-019-1503-x
dc.identifier.issn0038-0938
dc.identifier.urihttps://dspace.mackenzie.br/handle/10899/35221
dc.relation.ispartofSolar Physics
dc.rightsAcesso Restrito
dc.subject.otherlanguagemm Radio-Astronomy
dc.subject.otherlanguagePolarization
dc.subject.otherlanguageSolar radio bursts
dc.titleCenter-to-Limb Variation of Solar Bursts Polarization at Millimeter Wavelengths
dc.typeArtigo
local.scopus.citations3
local.scopus.eid2-s2.0-85071156903
local.scopus.updated2024-05-01
local.scopus.urlhttps://www.scopus.com/inward/record.uri?partnerID=HzOxMe3b&scp=85071156903&origin=inward
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