Polarized solar activity at mm-waves

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dc.contributor.authorHidalgo R.R.F.
dc.contributor.authorKaufmann P.
dc.contributor.authorMorosi A.
dc.date.accessioned2024-03-13T00:00:43Z
dc.date.available2024-03-13T00:00:43Z
dc.date.issued2017
dc.description.abstract© 2017 URSI.The time development of active regions generates slow period variations in the solar flux, this is called the slowly varying component or S-component of radio emission. Thus, the study of structure and physical processes in active regions, estimation of plasma parameters referring to layer in solar atmosphere are accessible by radio methods [1]. Although the S-component is best known at centimeter wavelengths, their observations at millimeter wavelengths shall improve the understanding of the emission mechanisms involved in solar active regions. We show that emission from a quiescent solar active region observed by solar radio polarimeters at 45 and 90 GHz exhibits fluxes increasing with frequencies.
dc.description.firstpage1
dc.description.lastpage3
dc.description.volume2017-January
dc.identifier.doi10.23919/URSIGASS.2017.8105264
dc.identifier.urihttps://dspace.mackenzie.br/handle/10899/35692
dc.relation.ispartof2017 32nd General Assembly and Scientific Symposium of the International Union of Radio Science, URSI GASS 2017
dc.rightsAcesso Restrito
dc.titlePolarized solar activity at mm-waves
dc.typeArtigo de evento
local.scopus.citations1
local.scopus.eid2-s2.0-85046124088
local.scopus.subjectEmission mechanism
local.scopus.subjectMillimeter wavelength
local.scopus.subjectPhysical process
local.scopus.subjectPlasma parameter
local.scopus.subjectSolar active regions
local.scopus.subjectSolar activity
local.scopus.subjectSolar atmosphere
local.scopus.subjectTime development
local.scopus.updated2024-05-01
local.scopus.urlhttps://www.scopus.com/inward/record.uri?partnerID=HzOxMe3b&scp=85046124088&origin=inward
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