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Article: Solar rotation stereoscopy in microwaves

TitleSolar rotation stereoscopy in microwaves
Authors
KeywordsSun: Activity
Sun: Corona
Sun: Radio Radiation
Sun: Rotation
Issue Date1995
PublisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/2041-8205
Citation
Astrophysical Journal Letters, 1995, v. 454 n. 1, p. 512-521 How to Cite?
AbstractWe present here the first stereoscopic altitude measurements of active region sources observed at microwave frequencies (10-14 GHz). The active region NOAA 7128 was observed with the Owens Valley Radio Observatory (OVRO) on 1992 April 13, 14, 15, and 16 as it passed through the central meridian. From white-light data of the underlying sunspot we determined the rotation rate of the active region, which was found to have a relative motion of dL/dt = +0°.240 day -1 with respect to the standard photospheric differential rotation rate. Based on this rotation rate we determine for the microwave sources stereoscopic altitudes of 3.3-11.0 Mm above the photosphere. The altitude spectrum h(vν) of the right circular polarization (RCP) main source shows a discontinuity at 12 GHz and can be satisfactorily fitted with a dipole model with a transition from the second to the third harmonic level at 12 GHz. The dominance of the third harmonic for frequencies above 12 GHz occurs because the second harmonic level drops below the transition region, at a height of 2.6 ± 0.6 Mm according to the microwave data. The altitude spectrum h(ν) serves also to invert the temperature profile T(h) from the optically thick parts of the radio brightness temperature spectrum T B(ν[h]). The microwave emission in both circular polarizations can be modeled with gyroresonance emission, with x-mode for RCP and o-mode in LCP, with the same harmonics at each frequency, but different emission angles in both modes. The contributions from free-free emission are negligible in both polarizations, based on the peak emission measure of EM ≈ 6 × 10 28 cm -5 observed in soft X-rays by Yohkoh/SXT. This study demonstrates that the height dependence of the coronal magnetic field B(h) and the plasma temperature T(h) in an active region can be inverted from the stereoscopic altitude spectra h(ν) and the observed brightness temperature spectra T B(V).
Persistent Identifierhttp://hdl.handle.net/10722/174904
ISSN
2015 Impact Factor: 5.487
2015 SCImago Journal Rankings: 3.369

 

DC FieldValueLanguage
dc.contributor.authorAschwanden, MJen_US
dc.contributor.authorLim, Jen_US
dc.contributor.authorGary, DEen_US
dc.contributor.authorKlimchuk, JAen_US
dc.date.accessioned2012-11-26T08:48:03Z-
dc.date.available2012-11-26T08:48:03Z-
dc.date.issued1995en_US
dc.identifier.citationAstrophysical Journal Letters, 1995, v. 454 n. 1, p. 512-521en_US
dc.identifier.issn2041-8205en_US
dc.identifier.urihttp://hdl.handle.net/10722/174904-
dc.description.abstractWe present here the first stereoscopic altitude measurements of active region sources observed at microwave frequencies (10-14 GHz). The active region NOAA 7128 was observed with the Owens Valley Radio Observatory (OVRO) on 1992 April 13, 14, 15, and 16 as it passed through the central meridian. From white-light data of the underlying sunspot we determined the rotation rate of the active region, which was found to have a relative motion of dL/dt = +0°.240 day -1 with respect to the standard photospheric differential rotation rate. Based on this rotation rate we determine for the microwave sources stereoscopic altitudes of 3.3-11.0 Mm above the photosphere. The altitude spectrum h(vν) of the right circular polarization (RCP) main source shows a discontinuity at 12 GHz and can be satisfactorily fitted with a dipole model with a transition from the second to the third harmonic level at 12 GHz. The dominance of the third harmonic for frequencies above 12 GHz occurs because the second harmonic level drops below the transition region, at a height of 2.6 ± 0.6 Mm according to the microwave data. The altitude spectrum h(ν) serves also to invert the temperature profile T(h) from the optically thick parts of the radio brightness temperature spectrum T B(ν[h]). The microwave emission in both circular polarizations can be modeled with gyroresonance emission, with x-mode for RCP and o-mode in LCP, with the same harmonics at each frequency, but different emission angles in both modes. The contributions from free-free emission are negligible in both polarizations, based on the peak emission measure of EM ≈ 6 × 10 28 cm -5 observed in soft X-rays by Yohkoh/SXT. This study demonstrates that the height dependence of the coronal magnetic field B(h) and the plasma temperature T(h) in an active region can be inverted from the stereoscopic altitude spectra h(ν) and the observed brightness temperature spectra T B(V).en_US
dc.languageengen_US
dc.publisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/2041-8205en_US
dc.relation.ispartofAstrophysical Journal Lettersen_US
dc.subjectSun: Activityen_US
dc.subjectSun: Coronaen_US
dc.subjectSun: Radio Radiationen_US
dc.subjectSun: Rotationen_US
dc.titleSolar rotation stereoscopy in microwavesen_US
dc.typeArticleen_US
dc.identifier.emailLim, J: jjlim@hku.hken_US
dc.identifier.authorityLim, J=rp00745en_US
dc.description.naturelink_to_subscribed_fulltexten_US
dc.identifier.scopuseid_2-s2.0-11944271600en_US
dc.identifier.volume454en_US
dc.identifier.issue1en_US
dc.identifier.spage512en_US
dc.identifier.epage521en_US
dc.publisher.placeUnited Kingdomen_US
dc.identifier.scopusauthoridAschwanden, MJ=7005411838en_US
dc.identifier.scopusauthoridLim, J=7403453870en_US
dc.identifier.scopusauthoridGary, DE=7005231589en_US
dc.identifier.scopusauthoridKlimchuk, JA=7004081884en_US

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