Solar atmospheric model over a highly polarized 17 GHz active region

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dc.contributor.authorSelhorst C.L.
dc.contributor.authorSilva-Valio A.
dc.contributor.authorCosta J.E.R.
dc.date.accessioned2024-03-13T01:37:13Z
dc.date.available2024-03-13T01:37:13Z
dc.date.issued2008
dc.description.abstractAims. We construct a 3D solar atmospheric model to reproduce active region brightness temperature of radio observations.Methods. A 3D solar atmospheric model was developed to reproduce the radio observations at 17 and 34 GHz from the Nobeyama Radioheliograph. The model included bremsstrahlung and gyro-resonance emission mechanisms. Both potential and force-free magnetic field extrapolations from MDI magnetograms are considered, as well as the changes in the quiet Sun atmosphere (density and temperature distributions) due to the magnetic field interaction. We analyze a highly polarized active region at 17 GHz ( LHCP) observed 2002 June 25 (NOAA 10008).Results. Modeling of this region requires that the whole projected region between the magnetic field footpoints changes its atmospheric density and temperature constitution. The modeling at 17 GHz showed the following results: a) the intensity of the corrected MDI magnetograms is able to account for the emission as gyro-resonance, but, the problem with saturation points still persists; b) for a low number of saturation points, a simple linear correction can change the maximum brightness temperature results in the simulations completely; c) the brightness temperature maxima resulting from the linear correction in the magnetic field intensities reproduced all maxima observed during the day (1.14-1.76 K); and d) the spatial brightness distribution of the gyro-resonance emission of NOAA 10008 was well-reproduced either by a potential or force-free field extrapolation with low positive α (0.70- Mm). At 34 GHz, the emission was successfully modeled as completely free-free radiation with a brightness temperature maximum in agreement with the observations.Conclusions. In summary the model is able to account for the observations at both frequencies, which are, however, produced by distinct emission mechanisms. © 2008 ESO.
dc.description.firstpage1079
dc.description.issuenumber3
dc.description.lastpage1084
dc.description.volume488
dc.identifier.doi10.1051/0004-6361:20079217
dc.identifier.issn0004-6361
dc.identifier.urihttps://dspace.mackenzie.br/handle/10899/37502
dc.relation.ispartofAstronomy and Astrophysics
dc.rightsAcesso Aberto
dc.subject.otherlanguageSun: atmosphere
dc.subject.otherlanguageSun: magnetic fields
dc.subject.otherlanguageSun: radio radiation
dc.titleSolar atmospheric model over a highly polarized 17 GHz active region
dc.typeArtigo
local.scopus.citations35
local.scopus.eid2-s2.0-51949089965
local.scopus.subjectActive region
local.scopus.subjectBrightness temperature
local.scopus.subjectEmission mechanisms
local.scopus.subjectFree fields
local.scopus.subjectLinear corrections
local.scopus.subjectMagnetic field extrapolations
local.scopus.subjectMaximum brightness
local.scopus.subjectMDI magnetograms
local.scopus.subjectQuiet-Sun
local.scopus.subjectRadio observations
local.scopus.subjectResonance emission
local.scopus.subjectSaturation points
local.scopus.subjectSolar atmospheric model
local.scopus.subjectSpatial brightness
local.scopus.subjectSun: atmosphere
local.scopus.subjectSun: magnetic fields
local.scopus.subjectSun: radio radiation
local.scopus.updated2024-05-01
local.scopus.urlhttps://www.scopus.com/inward/record.uri?partnerID=HzOxMe3b&scp=51949089965&origin=inward
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