Final Report
INTAS Open Call 2000 Project 00-0181:
Solar Coronal Magnetography
Period : July 1st 2001 – June 30th 2003
Project Co-ordinator : Dr. Boris Ryabov
Ventspils International Radio Astronomy Center
Akademijas laukums 1,
Riga LV-1050
e-mail : ryabov@latnet.lv
phone : +371-7-228321
fax
: +371-7-821153
SUMMARY OF RESULTS AND KEY REFERENCES
We have developed the technique of the coronal magnetography based on the inversion of the
circular polarization sign in a local microwave source on the Sun. The inversion has been treated
as the result of the quasi-transverse propagation of microwaves in the solar corona. The radio maps
of the solar active regions made with the Siberian Solar Radio Telescope (SSRT) and the
Nobeyama Radio Heliograph (NoRH) both in intensity and circular polarization have been used to
provide two-dimensional measurements of the coronal magnetic fields in the range of 10 – 110 G.
1) Coronal magnetograms of 10 – 30 Gauss
For the first time a series of coronal magnetograms of a set of the solar active regions (NOAA
9068, 9097, 9339, and 9415) has been measured. The active regions with a polarization inversion
in both eastern and western solar hemispheres are confirmed to provide the greatest number of the
magnetograms. The coronal magnetograms 60 – 120 wide, 10 – 35 G cover central portion of an
active region magnetosphere for 5 – 7 days around the time of the central meridian passage.
2) Consistency of coronal magnetograms
The coronal magnetograms as consistent with the intrinsic features of the coronal magnetic fields
give us some strong evidence of the validity of the coronal magnetography technique. The coronal
magnetograms of active region NOAA 8365 by using the radio maps taken with the SSRT and the
NoRH reproduce the general features of the coronal magnetic fields extrapolated in linear forcefree field model from the photosphere. The 2D coronal magnetograms of 50 – 110 G observed
with the NoRH at the heights of (1.5 – 3.8)  109 cm can be smoothly combined with the 10 – 30
G magnetogram measured with the SSRT at the coronal height of about (5 – 9)  109 cm. The
measured coronal fields behave in a predictable way: the strength distribution becomes more
regular with height. The derived characteristic of coronal currents, the constant  = 4.9  1011
cm1 of force-free field model, is just the result of the radio measurements in the magnetosphere of
NOAA 8365.
3) Technique improvements
The technique of coronal magnetography has been improved and made complete by the
verification of the validity and acceptable accuracy of coronal magnetography by means of
independent spectral polarization observations with the radio telescope RATAN-600. The new
method of the determination of the coronal height of each point in the plane of coronal
magnetogram is developed and compared with the existing semi-empirical methods. It is found
that the inaccuracy of several tens percent is inherent to all the methods of the height evaluation.
2
The investigations on the nature and the position of the involved microwave source are needed to
solve the problem of the more accurate height determination by means of radio observations.
4) Oscillations
The oscillations of the coronal magnetic fields of the active regions NOAA 6412, 6444, and 8230
with the characteristic time of 10 – 30 minutes have been revealed by means of the radio
measurements with the SSRT. It has been verified that the depolarization line is due to quasitransverse propagation of microwaves and that the points of the line under consideration oscillate
with the amplitude of 3 - 4. The longer time periods of the oscillations of 20 - 30 minutes are
found in the small compact active region NOAA 8230, whereas the matured active regions
NOAA 6412 and 6444 produce the oscillations with shorter time periods. It is supposed that, the
time periods of the oscillations are mainly determined not by the length of oscillating coronal
loops.
5) Plasma diagnostics anticipating the coronal magnetography
It is found that plasma in the post-eruptive arcades is controlled by the magnetic field and that the
coronal magnetography is highly desirable in the active regions producing eruptions. The spectral
polarization observations with the radio telescope RATAN-600 provide the electron density,
temperature, and the strength of the coronal magnetic field longitudinal component in the posteruptive arcades in the active regions NOAA 8108 and 9231 producing Coronal Mass Ejections.
The resulted gas-kinetic to magnetic pressure rations are much less than unity. The double
polarization inversion in a microwave source and the quick completion of each polarization
inversion are found to arise from the steep gradient of the coronal magnetic fields in the case of
flare-productive active region NOAA 9415.
Impact of the Results
 The results of the project gave an impetus to the efforts to elaborate new theoretical treatments
of the complicated polarization inversions at microwaves.
 The latest advances in coronal magnetography are taken into consideration in the science
requirements for the newly scheduled Frequency Agile Solar Radiotelescope (New Jersey
Institute of Technology, NRAO; http://www.ovsa.njit.edu/fasr/author_info.html).
 The collaboration is developed with the INTAS Open Call project 00-0543 entitled “Study of
MHD Oscillations in the Solar Active Regions Using Radio Observations”.
References
1. Ryabov B.I., Maksimov V.P., Lesovoi S.V., Shibasaki K., Nindos A., Pevtsov A.A. Coronal
magnetography of solar active region 8365 with the SSRT and NoRH radio heliographs.- Solar
Physics, 2003, (to be published).
2. Coronal magnetic field measurements through quasi-transverse propagation by Ryabov B.I..Chapter 6 in the book "Solar and Space Weather Radiophysics", ed.-s Dale E.Gary and
Christoph O. Keller, Astrophysics and Space Science Library series, Kluwer Academic
Publishers, 2003, (to be published); http://www.ovsa.njit.edu/fasr/author_info.html.
3. Coronal magnetic field measurements through bremsstrahlung emission by Gelfreikh G.B.Chapter 5 in the book "Solar and Space Weather Radiophysics", ed.-s Dale E.Gary and
Christoph O. Keller, Astrophysics and Space Science Library series, Kluwer Academic
Publishers, 2003, (to be published); http://www.ovsa.njit.edu/fasr/author_info.html.
4. 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. On the technique of coronal magnetography
through quasi-transverse propagation of microwaves.- Baltic Astronomy, 2003, (submitted).
5. Bogod V.M., Gelfreikh G.B., Drago F.Ch., Maksimov V.P., Nindos A., Kaltman T.I., Ryabov
B.I., Tokhchukova S.Kh. Study of polarized emission of the NOAA 9415 flare-productive
active region at microwaves.- “ASTROPAGE”, 2003, paper: astro-ph/03009444,
http://lanl.arxiv.org/abs/ astro-ph/?astro-ph%2F0309444; (submitted to Solar Physics).
3
6. Grechnev, V.V., Lesovoi, S.V., Smolkov, G.Ya., Krissinel, B.B., Zandanov, V.G., Altyntsev,
A.T., Kardapolova, N.N., Sergeev, R.Y., Uralov, A.M., Maksimov, V.P. , Lubyshev, B.I.,.
The Siberian Solar Radio Telescope: the current state of the instrument, observations, and
data. - Solar Physics, 2003, 216, N1-2, pp.239-272.
The progress of the project is presented at the Web site “ Solar Coronal Magnetography. INTAS
project #181” at http://borisphenus2.tripod.com/index.html
1. RESEARCH
1.1
Overview of Research Activities
1.1.1 Ventspils International Radio Astronomy Centre (VIRAC), Riga, Latvia
o Co-ordination of the project
o Radio mapping and selection of active regions in the course of polarization inversion in each
solar hemisphere (task T1.1)
o Long-sized and nearby sunspot coronal magnetic structures (task T1.2)
o The reconstruction of the active region magnetospheres (task T1.3)
o Diagnostics of plasma on the basis of the microwave spectrum and the coronal magnetography
of solar active regions (task T2.1)
o Nonthermal microwave sources in active regions (task T2.2)
1.1.2 University of Florence, Florence, Italy
o Long-sized and nearby sunspot coronal magnetic structures (task T1.2)
o The reconstruction of the active region magnetospheres (task T1.3)
o Diagnostics of plasma on the basis of the microwave spectrum and the coronal magnetography
of solar active regions (task T2.1)
o Nonthermal microwave sources in active regions (task T2.2)
1.1.3 Special Astrophysical Observatory (SAO), Nizhnij Arkhyz, Russia
o Radio mapping and selection of active regions in the course of polarization inversion in each
solar hemisphere (task T1.1)
o Long-sized and nearby sunspot coronal magnetic structures (task T1.2)
o The reconstruction of the active region magnetospheres (task T1.3)
o Diagnostics of plasma on the basis of the microwave spectrum and the coronal magnetography
of solar active regions (task T2.1)
o Nonthermal microwave sources in active regions (task T2.2)
1.1.4
Institute of Solar-Terrestrial Physics (ISTP), Irkutsk, Russia
o Radio mapping and selection of active regions in the course of polarization inversion in each
solar hemisphere (task T1.1)
o Long-sized and nearby sunspot coronal magnetic structures (task T1.2)
o The reconstruction of the active region magnetospheres (task T1.3)
o Diagnostics of plasma on the basis of the microwave spectrum and the coronal magnetography
of solar active regions (task T2.1)
o Nonthermal microwave sources in active regions (task T2.2)
1.1.5
Pulkovo Astronomical Observatory (Pulkovo), St-Petersburg, Russia
o Radio mapping and selection of active regions in the course of polarization inversion in each
solar hemisphere (task T1.1)
o Long-sized and nearby sunspot coronal magnetic structures (task T1.2)
o The reconstruction of the active region magnetospheres (task T1.3)
o Diagnostics of plasma on the basis of the microwave spectrum and the coronal magnetography
of solar active regions (task T2.1)
o Nonthermal microwave sources in active regions (task T2.2)
The research activities have been in accordance with the Work Programme. In addition to the
Work Programme, Florence team has participated T1.1, Pulkovo team has participated the task
T1.2, SAO and Pulkovo teams have participated T1.3.
4
1.2
Scientific Results
The main results and their scientific significance:
For the first time a series of coronal magnetograms of a set of the solar active regions
(NOAA 9068, 9097, 9339, and 9415) has been measured [3, 4, 12, 24]. The active regions with a
polarization inversion in both eastern and western solar hemispheres are confirmed to provide the
greatest number of the magnetograms. The coronal magnetograms 60 – 120 wide, 10 – 35 G
cover the central portion of an active region magnetosphere for 5 – 7 days around the time of the
central meridian passage.
The accumulated experience of the coronal magnetography [1, 3, 4, 6, 7, 12, 15, 23, 24] is of
practical significance both to complement two other techniques of radio magnetography (through
bremsstrahlung [33] and gyro emission) and to cover the coronal magnetic field strength range by
precise measurements.
1.2.1
The consistent coronal magnetograms give us some strong evidence of the validity of the
coronal magnetography technique. The coronal magnetograms of active region NOAA 8365 [1, 6,
12, 23, 24, 32] by using the radio maps taken with the SSRT [25] and the NoRH reproduce the
general features of the coronal magnetic fields extrapolated in linear force-free field model from
the photosphere. The 2D coronal magnetograms of 50 – 110 G observed with the NoRH at the
heights of (1.5 – 3.8)  109 cm can be smoothly combined with the 10 – 30 G magnetogram
measured with the SSRT at the coronal height of about (5 – 9)  109 cm. The measured coronal
fields behave in a predictable way: the strength distribution becomes more regular with height. The
derived characteristic of coronal currents, the constant  = 4.9  1011 cm1 of force-free field
model, is just the result of the radio measurements in the magnetosphere of NOAA 8365.
The project has indicated the way to the permanent coronal magnetography over a wide range of
the coronal magnetic field strength [32, 33]. The permanent radio magnetography is regarded as
being a magnetic energy measure, a prognostic tool of solar eruptions, and a interaction indicator
with solar plasma in the topologically peculiar regions.
1.2.2
The technique of coronal magnetography has been improved and made complete by the
verification of the validity and acceptable accuracy of coronal magnetography by means of
independent spectral polarization observations with the radio telescope RATAN-600 [3, 4, 6, 7, 9,
12, 15, 24, 27, 29]. The new method of the determination of the coronal height of each point in the
plane of coronal magnetogram is developed and compared with the existing semi-empirical
methods [3]. It is found that the inaccuracy of several tens percent is inherent to all the methods of
the height evaluation [1, 3]. The investigations on the nature and the position of the involved
microwave source are needed to solve the problem of the more accurate height determination by
means of radio observations.
It has been ascertained that all three techniques of radio magnetography (through QTpropagation [6], bremsstrahlung [7] and gyro emission) are complementary as regards the
sensitivity to and the position of the coronal fields to be measured. A combined program of the 2D
coronal magnetography of solar active regions is best suited for observations with such telescopes
as the forthcoming FASR [32, 33]. The efforts to elaborate new theoretical treatments and new
approaches to model simulations of the complicated polarization inversions at microwaves should
be mentioned [2, 11, 26, 28, 30, 31].
1.2.3
The oscillations of the coronal magnetic fields of the active regions NOAA 6412, 6444,
and 8230 with the characteristic time of 10 - 30 minutes have been revealed by means of the radio
measurements with the SSRT [8, 13, 16, 20 - 22]. It has been verified that the depolarization line is
due to quasi-transverse propagation of microwaves and that the points of the line under
consideration oscillate with the amplitude of 3 - 4. The longer time periods of the oscillations of
20 - 30 minutes are found in the small compact active region NOAA 8230, whereas the matured
active regions NOAA 6412 and 6444 produce the oscillations with shorter time periods [20]. It is
supposed that, the time periods of the oscillations are mainly determined not by the length of
oscillating coronal loops.
1.2.4
5
Contrary to the standard position measurements in the EUV or X-ray bright coronal loops, the
performed radio measurements are referred to the displacements of the coronal magnetic fields at a
fixed strength [16]. The direct radio measurements have a potential to an amplitude and phase
study of oscillations. These should give a possibility to recognize an oscillation type.
It is found that plasma in the post-eruptive arcades is controlled by the magnetic field and
that the coronal magnetography is highly desirable in the active regions producing eruptions [2, 5,
10, 11, 14, 17]. The spectral polarization observations with the radio telescope RATAN-600 [26,
27, 29, 30] provide the electron density, temperature, and the strength of the coronal magnetic field
longitudinal component in the post-eruptive arcades in the active regions NOAA 8108 [5] and
9231 [10] producing Coronal Mass Ejections. The resulted gas-kinetic to magnetic pressure ratios
are much less than unity.
The series of solar observations have been especially made with the help of the RATAN-600
throughout a month in 2001, 2002, and 2003. The observations were undertaken to provide the
diagnostics of solar plasma. The new regime was realized in the form of daily multi-azimuth and
multi-wavelength observations over a wide microwave range with 4 minutes cadence during 4
hours.
The double polarization inversion in a microwave source and the quick completion of each
polarization inversion are found to arise from the steep gradient of the coronal magnetic fields in
the case of flare-productive active region NOAA 9415 [2, 9, 11, 14, 15, 19, 26, 30].
The above measurements confirm the conjectures on the steep gradients of the coronal fields in
flare-productive active regions and the magnetic pressure dominance at the base of coronal
streamers [2, 5, 10]. After the coronal magnetography completion these results will become more
important as they clarify the interaction between explosive events and the active region
magnetosphere structure.
All the publications [1 - 33] resulted directly from the project. The works [1, 3 - 4, 23, 24, 27,
32, 33] on the subject have to be published. An additional comprehensive publication on the
coronal magnetography [4] is in preparation.
1.2.5

Joint Publications of INTAS and NIS project teams
International journals
1) Ryabov B.I., Maksimov V.P., Lesovoi S.V., Shibasaki K., Nindos A., Pevtsov A.A. “Coronal
magnetography of solar active region 8365 with the SSRT and NoRH radio heliographs”.Solar Physics, 2003, (to be published).
2) Bogod V.M., Gelfreikh G.B., Drago F.Ch., Maksimov V.P., Nindos A., Kaltman T.I., Ryabov
B.I.,Tokhchukova S.Kh.: 2003, “Study of polarized emission of the NOAA 9415 flareproductive active region at microwaves”.- “ASTROPAGE”, paper: astro-ph/03009444;
http://lanl.arxiv.org/abs/astro-ph/?astro-ph%2F0309444, (submitted to Solar Physics, 2003).
3) 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. “On the technique of coronal magnetography
through quasi-transverse propagation of microwaves”.- Baltic Astronomy, 2003, (submitted).
4) Ryabov B.I., Bogod V.M., Gelfreikh G.B., Maksimov V.P., Drago F., Lubyshev B.I., Peterova
N.G., Borisevich T.P., Bezrukov D.A.: 2003, “Magnetograms of solar active regions”.- Solar
Physics, 2003, (in preparation).

National journals
5) Peterova N.G., Ryabov B.I., Tokhchukova S.Kh. "A peculiar microwave source in the
structure of the NOAA 8108 AR from observations with RATAN-600".- Bulletin of Special
Astrophysical Observatory, 2001, v.51, p.106-111 (in English).

Abstracts in proceedings (indicate invited publications)
6) Ryabov B.I. "Coronal Magnetography from Quasi-Transverse Propagation".- (invited talk
presenting the progress of the INTAS project at the Green Bank Workshop "Solar
Radiophysics with the Frequency Agile Solar Radiotelescope, NRAO, Green Bank, WV, USA,
May 23-25, 2002.- Program and Abstracs, p.37. Both the abstract and the text of presentation
are published at the Web site http://www.ovsa.njit.edu/fasr/May_program.html).
7) Gelfreikh G.B. "Bremsstrahlung diagnostics of coronal magnetic fields".- (invited talk at the
Green Bank Workshop "Solar Radiophysics with the Frequency Agile Solar Radiotelescope,
6
NRAO, Green Bank, WV, USA, May 23-25, 2002.- Program and Abstracs, p25. Both the
abstract and the text of presentation are published at the Web site
http://www.ovsa.njit.edu/fasr/May_program.html).
8) Gelfreikh G.B., Ryabov B.I., Peterova N.G., Drago F., Agalakov B.V., Borisevich T.P.,
Lubyshev B.I., Maksimov V.P. "Oscillations of the zero-polarization region in the core of the
local source NOAA 6412".- Third Russian-Chinese Conference on Space Weather, 19-21 June
2002, Abstracts, Irkutsk, 2002, p.47.
9) Kaltman T.I, Agalakov B.V., Korzhavin A.N., Maksimov V.P., Ryabov B.I., Peterova N.G.
"The inversion of polarization sign in solar active regions with RATAN-600 and SSRT
observations".- Proc. 10th European Solar Physics Meeting, 'Solar Variability: From Core to
Outer Frontiers', Prague, Czech Republic, 9-14 September 2002, ESA SP-506, December
2002.
10) Borovik V.N, Gelfreikh G.B., Medar V.G., Grigorieva I.Y. “First registration of the posteruptive arcade formation during CME-event in wide microwave range”.- Proc. 10th European
Solar Physics Meeting, 'Solar Variability: From Core to Outer Frontiers', Prague, Czech
Republic, 9-14 September 2002, ESA SP-506, December 2002, p.431 - 434.
11) Bogod V.M., Gelfreikh G.B., Grechnev V.V., Nindos A., Kaltman T.I., Ryabov B.I.,
Tokhchkova S.Kh. "Analysis of flare-productive active region AR9415". - 10th European
Solar Physics Meeting, 9-14 September 2002, Prague, Abstracts, p.13.
12) Ryabov B.I., Bogod V.M., Gelfreikh G.B., Maximov V.P., Drago F., Lubychev B.I., Peterova
N.G., Borisevich T.P. "Coronal magnetography of solar active regions".- International
conference”.- "Active processes on the Sun", St. Petersburg University, July 1-6 2002,
Abstracts, p.29 (in Russian).
13) Gelfreikh G.B., Ryabov B.I., Peterova N.G., Drago F., Agalakov B.V. , Borisevich T.P.,
Lubychev B.I., Maximov V.P. "Oscillations of neutral line region in NOAA 6412".International conference.” -"Active processes on the Sun", St. Petersburg University, July 1-6
2002, Abstracts, p.17 (in Russian).
14) Bogod V.M., Gelfreikh G.B., Grechnev V.V., Nindos A., Kaltman T.I., Ryabov B.I.,
Tokhchkova S.Kh. "Analysis of flare-productive active region AR9415".- International
conference “.- “Active processes on the Sun", St. Petersburg University, July 1-6 2002,
Abstracts, p.13 (in Russian).
15) Kaltman T.I., Korzhavin A.N., Agalakov B.V., Maximov V.P., Ryabov B.I. "Active regions
with polarization inversion according RATAN-600 and SSRT observations".- "Active
processes on the Sun", St. Petersburg University, July 1-6 2002, Abstracts, p.23 (in Russian).
16) Agalakov B.V., Gelfreikh G.B., Ryabov B.I., Peterova N.G., Drago F., Borisevich T.P.,
Lubyshev B.I., Maksimov V.P. "Treatment of coronal magnetic field oscillations above solar
active regions using inversion screen technique".- Conference "Radiotelescopes RT-2002", 911 October 2002, Puschino, Russia (in Russian).
17) Ryabov B.I., Korzhavin A.N., Kaltman T,I., Peterova N.G., Borisevich T.P., Agalakov B.V.
“Coronal magnetic fields of "cusp-shaped" loops as observed at microwaves“. – International
conference of the NIS and Baltic countries "Current Problems of Solar and Stellar Activity",
June 02-07, 2003, Nizhny Novgorod, Russia. Proceedings of the conference, Nizhny
Novgorod, 2003, p.54-57 (in Russian).
18) Bogod V.M., Gelfreikh G.B., Tokhchukova S.Kh., Nindos A., Ryabov B.I.: 2003, “Spectral
and polarization analysis of quasi-periodical oscillations of solar microwave local sources
with RATAN-600”.- International conference of the NIS and Baltic countries "Current
Problems of Solar and Stellar Activity", June 02-07, 2003, Nizhny Novgorod, Russia.
Proceedings of the conference, Nizhny Novgorod, 2003, p.296-299 (in Russian).
19) Bogod V.M., Gelfreikh G.B., Kaltman T,I., Ryabov B.I., Tokhchukova S.Kh.: 2003, “A study
of flare-productive active region development using detail spectral and polarization
analysis”.- ”.- International conference of the NIS and Baltic countries "Current Problems of
Solar and Stellar Activity", June 02-07, 2003, Nizhny Novgorod, Russia. Proceedings of the
conference, Nizhny Novgorod, 2003, p.300-303 (in Russian).
20) Gelfreikh G.B., Ryabov B.I., Peterova N.G., Agalakov B.V., Borisevich T.P. “Oscillations of
coronal magnetic fields based on the analyses of quasi-transverse propagation of
7
microwaves.“ – International conference of the NIS and Baltic countries "Current Problems of
Solar and Stellar Activity", June 02-07, 2003, Nizhny Novgorod, Russia. Proceedings of the
conference, Nizhny Novgorod, 2003, p. 328-331 (in Russian).
21) Agalakov B.V., Borisevich T.P., Peterova N.G., Ryabov B.I. “Results and perspectives of
investigation of oscillations of the coronal magnetic field using the SSRT observations”.Russian conference devoted to memory of Prof. V.E. Stepanov “Magnetic fields and 3D
structure of the solar atmosphere”, August 25-29, 2003, Irkutsk, Russia. Abstracts, Irkutsk,
2003, p.29 (in Russian).
22) Agalakov B.V., Borisevich T.P., Peterova N.G., Ryabov B.I. “Study of the solar corona above
the active region NOAA 9591 using microwave observations”.- Russian conference devoted to
memory of Prof. V.E. Stepanov “Magnetic fields and 3D structure of the solar atmosphere”,
August 25-29, 2003, Irkutsk, Russia. Abstracts, Irkutsk, 2003, p.52 (in Russian).
23) Pevtsov A.A., Nindos A., Shibasaki K., Maksimov V.P., Lesovoi S.V., Ryabov B.I. “Coronal
Magnetography of Solar Active Region 8365 With the SSRT and NoRH Radio Heliographs”.American Geophysical Union, Fall 2003 AGU Meeting Session SH08: “Coronal Magnetic
Fields: From Models to Measurements”, December 2003, (submitted, 2003).
24) Ryabov B.I., Bogod V.M., Gelfreikh G.B., Maksimov V.P., Drago F., Lubyshev B.I., Peterova
N.G., Borisevich T.P., Bezrukov D.A. “Coronal magnetograms of solar active regions”.IAU Symposium No.223 “Multi-Wavelength Investigations of Solar Activity”, June 14-19
2004, St. Petersburg, Russia, (submitted, 2003).

 Publications without INTAS-NIS co-authorship of the project teams
International journals
25) Grechnev, V.V., Lesovoi, S.V., Smolkov, G.Ya., Krissinel, B.B., Zandanov, V.G., Altyntsev,
A.T., Kardapolova, N.N., Sergeev, R.Y., Uralov, A.M., Maksimov, V.P. , Lubyshev, B.I.,.
“The Siberian Solar Radio Telescope: the current state of the instrument, observations, and
data”. - Solar Physics, 2003, 216, N1-2, pp.239-272.

National journals
26) Bogod V.M., Tokhchukova S.Kh. Peculiarities of the Microwave Emission from Active
Regions Generating Intense Solar Flares, - Astronomy Letter, 2003, 29, p.263-273.
27) Bogod V.M., Zhekanis G.N., Mingaliev M.G., Tokhchukova S.Kh. Multi azimuth method of
observationswith South sector and Periscope RATAN-600, Radiophysics, 2003 (submitted).
 Abstracts in proceedings (indicate invited publications)
28) Kaltman T.I., Korzhavin A.N. "Polar radiance in solar active region magnetospheres and
their possible manifestations at microwaves".- International conference "Active processes on
the Sun".- St. Petersburg University, July 1-6 2002, Abstracts, p.22 (in Russian).
29) Bogod V.M., Zhekanis G.N., Mingaliev M.G., Tokhchukova S.Kh., Khaikin V.B.
"Multiathimuth regime of observations at South sector of RATAN-600 with periscope mirror".Conference "Radiotelescopes RT-2002", 9-11 October 2002, Puschino, Russia (in Russian).
30) Bogod V.M., Tokhchukova S. Spectral-polarization behavior of solar active region producing
powerful flares, - Proc. 10th European Solar Physics Meeting, 'Solar Variability: From Core to
Outer Frontiers', Prague, Czech Republic, 9-14 September 2002, ESA SP-506, December
2002, p.279- 282.
31) Kaltman T.I., Korzhavin A.N., Tsap Yu.T. "Polarization inversion in the frame of a model
with negative height gradient of temperature".- ”.- International conference of the NIS and
Baltic countries "Current Problems of Solar and Stellar Activity", June 02-07, 2003, Nizhny
Novgorod, Russia. Proceedings of the conference, Nizhny Novgorod, 2003, p.323-327 (in
Russian).
 Books, monographs, internal reports, thesis, patents
32) "Coronal magnetic field measurements through quasi-transverse propagation" by Ryabov
B.I..- Chapter 6 in the book "Solar and Space Weather Radiophysics", ed.-s Dale E.Gary and
Christoph O. Keller, Astrophysics and Space Science Library series, Kluwer Academic
Publishers, 2003, (to be published).
33) "Coronal magnetic field measurements through bremsstrahlung emission" by Gelfreikh G.B.Chapter 5 in the book "Solar and Space Weather Radiophysics", ed.-s Dale E.Gary and
8
Christoph O. Keller, Astrophysics and Space Science Library series, Kluwer Academic
Publishers, 2003, (to be published).
ONLY: Jointly by
INTAS and NIS
Project teams
ALL PUBLICATIONS
Scientific Output
Paper in an International
Journal
Paper in a National Journal *)
Published
In press/accepted
Submitted
2
1
2
3
1 (English)
-
2 (English)
1
21
-
2
19
-
-
2 (English)
-
2
-
-
-
-
-
Abstract in proceedings
(conferences, workshops)
Book, Monograph *)
Internal Report **)
Thesis (MSc, PhD, etc.) *)
Patent
*) Indicate the language **) Indicate if a report has not been published purely in order to protect intellectual property rights.
1.3
Impact and Applications
 The results of the project gave an impetus to the efforts to elaborate new theoretical treatments
of the complicated polarization inversions at microwaves.
 The latest advances in coronal magnetography are taken into consideration in the science
requirements for the newly scheduled Frequency Agile Solar Radiotelescope (New Jersey
Institute of Technology, NRAO; http://www.ovsa.njit.edu/fasr/author_info.html).
 The collaboration is developed with the INTAS Open Call project 00-0543 entitled “Study of
MHD Oscillations in the Solar Active Regions Using Radio Observations”.
 The solar plasma diagnostics complemented by coronal magnetography should provide the
adequate and comprehensive representation of solar plasma in flaring active regions,
improving the solar flare models and the solar flare and coronal mass ejection forecasts.
2. MANAGEMENT
2.1
Meetings and visits
Co-ordination meetings:
 the first co-ordination meeting held at Pulkovo Astronomical Observatory, Russia, March 25 29, 2002 (approval of the lists of targeted ARs, progress reports; VIRAC: Ryabov B.I.; SAO:
Bogod V.M., Korzhavin A.N., Peterova N.G., Tokhchukova S.Kh.; ISTP: Lubyshev B.I.;
Pulkovo: Gelfreikh G.B., Borovik V.N., Medar V.G., Borisevich T.P.);
 the second co-ordination meeting held at Pulkovo Astronomical Observatory, Russia, July 10 14, 2002 (discussion on the microwave polarization of flaring ARs; University of Florence:
F.Drago, M. Velli, invited C. Chiuderi; SAO: Bogod V.M., Korzhavin A.N., Peterova N.G.,
Tokhchukova S.Kh.; Pulkovo: Gelfreikh G.B., Borovik V.N., Medar V.G., Borisevich T.P.);
 the meeting held during Green Bank Workshop , USA, May 23-25, 2002 (discussions on the
progress of the project; VIRAC: Ryabov B.I.; University of Florence: F.Drago; SAO: Bogod
V.M.; Pulkovo: Gelfreikh G.B.);
 the meeting held at Pulkovo Astronomical Observatory, Russia, July 7-9, 2003 (discussions on
the completion of the project; SAO: Bogod V.M., Korzhavin A.N., Peterova N.G.,
Tokhchukova S.Kh.; Pulkovo: Gelfreikh G.B., Borovik V.N., Borisevich T.P.; VIARAC:
Ryabov B.I.; ISTP: Agalakov B.V.).
Exchange visits of scientists:
 Ryabov B.I., VIRAC visited Florence Universityб Italy, May 6-12, 2003 (preparation of a joint
paper on the coronal magnetography of the sampled solar active regions);
 Bogod V.M., SAO visited Florence University, Italy, June 30 - July 6, 2003 (collaboration
with Drago F. and Briard C. in joint radio and magnetographic observations; preparation of a
joint paper treating a flare-productive active region).
9
2.2
Visits
West ==> East
East ==> West
West ==> West
Number of scientists
4
3
3
Number of person days
13
9
9
East ==> East
10
77
Collaboration
Intensity of Collaboration
West <=> East
West <=> West
East <=> East
2.3
high
rather high
×
×
×
rather low
Low
Time Schedule
The time planning has been in accordance with the Work Programme.
2.4
Problems encountered
Problems encountered
Co-operation of team members
Transfer of funds
Telecommunication
Transfer of goods
Other
2.5
Major
Minor
None
×
×
×
×
×
not applicable
Actions required
No actions are required from INTAS.
2.6
Manpower invested
It is supposed that roughly 28 person-years went into the project. Some participants are involved in
one more INTAS Open Call project, that is, the project 00-0543 “Study of MHD Oscillations in
the Solar Active Regions Using Radio Observations”. The value of 28 person-years can be
considered as being about 100 % due to funding received from the grant of the project 00-0181.
3. FINANCES (in EURO)
4. ROLE AND IMPACT OF INTAS
Role of INTAS
Would the project have been started
without funding by INTAS?
Would the project have been carried out
without funding from INTAS?
Main achievement of the project
exciting science
new international contacts
additional prestige for my lab
additional funds for my lab
helping scientists in NIS
other (specify):
Definitely yes
rather yes
rather not
definitely not
√
√
very important
quite important
less important
not important
√
√
√
√
√
All teams participating this project are going to continue co-operation in the frame of a new
research project “Spectral Polarization Radio Survey for Physics of Solar Flares” (submitted to
INTAS Open Call 2003). The project is aimed to make the uniform and comprehensive
representation of a pre-flare state of solar plasma by means of microwave observations and coronal
magnetography.