1. “Coronal Magnetograms of Solar Active Regions Derived from Polarization Inversion in Microwaves” Boris Ryabov Latvian University, Latvia MSFC Photospheric Magnetogram of NOAA 7260 NoRH Coronal Magnetogram of NOAA 7260 (from Ryabov B.I., Pilyeva N.A., Alissandrakis C.E., Shibasaki K., Bogod V.M., Garaimov V.I., Gelfreikh G.B.: 1999, Solar Physics, 185,157)

2. QTR Time dependence of polarization inversion fits the model properties of QT-region. NOAA 9068 NoRH maps & KPNO magnetograms Model prediction of QT-region

3. Technique of coronal magnetography. NOAA 9068 B(G)  205. 4/3 (cm) [- ln(0.5  o + 0.5)] /1/3, where the product of electron density N and the scale L d of coronal magnetic field divergence is assumed to be constant, N L d = 10 18 cm -2, is observing wavelength. = 5.2 cm (from Bezrukov D.A., Ryabov B.I., Bogod V.M., Gelfreikh G.B., Maksimov V.P., Drago F., Lubyshev B.I., Peterova N.G., Borisevich T.P.: 2004, to be published in Baltic Astronomy)

4. Frequency dependence of polarization inversion fits the QT - propagation. NOAA 8365 NoRH maps V/I observed at 1.76cm on (a) October 22, (b) 23, (c) 24, 1998 SSRT maps V/I observed at 5.2 cm on (d) October 21, (e) 22, (f) 23, 1998 - DL is found to be closer to the NL at a shorter wavelength, as DL is formed at stronger coronal magnetic fields for a shorter wavelength. - The closer an AR to the solar limb is the shorter is the wavelength required to detect the polarization inversion.

5. Coronal magnetography is a 3D magnetography. NOAA 8365 (1) As the shape and the height of any QT-surface are not known in radio observations revealing the strengths of coronal magnetic fields, they should be evaluated from 3D model simulations. (2) To provide credible coronal magnetograms the lo- cation and the directivity V(  ) of the microwave source should be made clear by 3D model simulations. The coronal magnetograms measured in the plane of view should be restored in 3D space.

6. The coronal magnetograms in the range of 10  30 G at 5.2 cm (SSRT) and 50  110 G at 1.76 cm (NoRH) are evaluated. The height of the QT-region is estimated from the force-free field extrapolations as 6.2  10 9 cm for the 20 G and 2.3  10 9 cm for 85 G levels. Model evaluation of coronal heights for 2-D magnetograms. NOAA 8365 FFF Model Simulations: m.f. & height (from Ryabov B.I., Maksimov V.P., Lesovoi S.V., Shibasaki K., Nindos A., Pevtsov A.: 2004, to be published in Solar Physics) SSRT: coronal magnetograms

7. NoRH and SSRT: coronal magnetograms of October 23, 1998 Consistency of results. Radio observations of the active region NOAA 8365 The features of the measured coronal magnetograms: The measured values (28  150 G from the NoRH maps at 1.76 cm and 6.7  35 G from the SSRT maps at 5.2 cm) overlap and can be compared. - DL tends to move toward the western solar limb; - DL is found to be closer to the NL at a shorter wavelength; - the gradient is in the W-E direction for a bipolar AR located in the western hemisphere.

8. Difficulties of coronal magnetography: NOAA 9415 NoRH observations on April 12-13, 2001. A sketch of polarization changes produced by 2 coronal regions of QT-propagation and observed with the RATAN-600 (from Bogod V.M., Gelfreikh G.B., Drago F.Ch., Maksimov V.P., Nindos A., Kaltman T.I., Ryabov B.I., Tokhchukova S.Kh.: 2003, ASTROPAGE, astro-ph/03009444). Not all mechanisms of polarization inversion in the microwave range have been investigated. This coronal magnetography should be conducted with a caution to avoid the confusion of QT and non QT-propagations. The technique needs further improvements concerning the evaluation of the coronal height, directivity, and the evolution of a microwave source.

9. Oscillations Depolarization line oscillations show evidence of the oscillations of QT-region and/or the oscillations of iso-gauss surface (1) Stable coronal magnetogram results from radio maps averaged over 30 – 60 minute time intervals (NoRH). (2) The coronal magnetic field oscillations with the charac- teristic time of 10 – 20 minutes have been reported (SSRT). (from Gelfreikh G.B., Ryabov B.I., Agalakov B.V., Borisevich T.P., Peterova N.G.: 2004, submitted to Baltic Astronomy) Alternative ways to get results

10. Summary  Microwave measurements have the potential to determine magnetic fields in solar active regions in the range of 10 – 110 G taking advantage of radio mapping with the NoRH and the SSRT.  Obtaining the values of the QT-region heights makes the coronal magnetography three-dimensional.  Existing interpretations of possible polarization inversions in microwaves have to be supplemented with new ones in an effort to discriminate the polarization inversions due to QT-propagation.  An advance in this coronal magnetography application is ex- pected to be in the field of coronal field oscillations (the intensities of coronal fields and their spatial and temporal variations).