Polarization changes with time during solar microwave impulsive bursts

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dc.contributor.authorKaufmann P.
dc.contributor.authorMatsuura O.T.
dc.contributor.authorDos Santos P.M.
dc.date.accessioned2024-03-13T01:48:27Z
dc.date.available2024-03-13T01:48:27Z
dc.date.issued1970
dc.description.abstractThe evolution with time of circular polarization π(t) from solar bursts at 7 GHz presents, in the majority of cases, a polarization degree peak before the maximum flux time. The subsequent evolution of π(t) is continuous and usually increasing. The changes could be caused by superimposed polarization effects, due to the fast emissive electrons (dominant in the first phase), and to the propagation effects caused by the coronal condensation where the event occurred (dominant in the second phase). In an approximate approach, π(t) is connected to the movement of the source in the second phase, being qualitatively sound, but limited to the lack of knowledge on acceleration processes and on magnetic field topology in the active region where the flares take place. © 1970 D. Reidel Publishing Company.
dc.description.firstpage190
dc.description.issuenumber1
dc.description.lastpage195
dc.description.volume14
dc.identifier.doi10.1007/BF00240177
dc.identifier.issn0038-0938
dc.identifier.urihttps://dspace.mackenzie.br/handle/10899/38118
dc.relation.ispartofSolar Physics
dc.rightsAcesso Restrito
dc.titlePolarization changes with time during solar microwave impulsive bursts
dc.typeArtigo
local.scopus.citations5
local.scopus.eid2-s2.0-34250483769
local.scopus.updated2024-05-01
local.scopus.urlhttps://www.scopus.com/inward/record.uri?partnerID=HzOxMe3b&scp=34250483769&origin=inward
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