A model for active region emission at centimeter wavelengths |
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| Authors: | A Nindos C E Alissandrakis G B Gelfreikh M R Kundu K P Dere A N Korzhavin V M Bogod |
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| Institution: | (1) Section of of Astrophysics, Astronomy and Mechanics, Department of Physics, University of Athens, GR-15784 Athens, Greece;(2) Section of Astrogeophysics, Department of Physics, University of Ioannina, GR-45110 Ioannina, Greece;(3) Main Astronomical Observatory of the Russian Academy of Sciences, 196140 Pulkovo, St. Petersburg, Russia;(4) Astronomy Department, University of Maryland, 20742 College Park, MD, U.S.A.;(5) E. O. Hulburt Center for Space Research, U.S. Naval Research Laboratory, 20375-5000 Washington, DC, U.S.A.;(6) St. Petersburg Branch of the Special Astrophysical Observatory of the Russian Academy of Sciences, St. Petersburg, 196140 Pulkovo, Russia |
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| Abstract: | We present multi-frequency observations and model computations of the microwave emission of a solar active region. The radio observations were obtained with the RATAN-600 at several wavelengths between 0.8 and 31.6 cm and with the VLA at 6 and 20 cm. The active region was also observed in the EUV O Iv lines by the HRTS instrument aboard the Space Shuttle Spacelab-2 mission. These lines are formed in the chromosphere-corona transition region and their intensity ratio is sensitive to pressure. Photospheric magnetograms provided both the longitudinal and the transverse component of the magnetic field. The microwave observations were checked against model computations taking into account both the free-free and the gyro-resonance emission mechanisms and using the pressure data from the O IV lines. The magnetic field was computed through constant- force-free extrapolations of the longitudinal photospheric field. We computed both the flux from 2 to 20 cm and the spatial structure of the microwave emission at 6 and 20 cm. The comparison of the computed and observed flux spectra allowed us to estimate the magnetic field strength at the base of the transition region and in the low corona, as well as the values of the conductive flux and the height of the base of the transition region. The model maps at 6 cm and 20 cm showed that was not constant above the active region; the same conclusion was reached on the basis of the photospheric observations. The use of pressure measurements allowed us to identify microwave structures which were determined by pressure enhancements. At 6 cm the computations confirmed the fact that the magnetic field is the principal factor that determines the structure of sunspot-associated sources and showed that the effect of pressure variations was small. Pressure variations were more important at 20 cm, where the peak of the emission was associated with the sunspot and a diffuse component was associated with the plage which had an average pressure higher by a factor of 1.54 than the sunspot. |
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