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RESULTS OF THE PROMINENCE OBSERVATIONS AT MICROWAVES DURING THE MAXIMAL PHASE OF THE TOTAL SOLAR ECLIPSE OF MARCH 2006
O.A. Golub china, V.M. Bogo d, A.N. Korzhavin, N.N. Bursov, S. Kh. Tokhchukova SPb branch of SAO RAS, St.Petersburg, Russia oag@OG4466.spb.edu Results of the prominence radio emission study according to observations of the solar eclipse on 2006 March 29 with the Northern sector and with the Southern sector with the Flat mirror of RATAN-600 are discussed. Investigation of the prominence lo cated in the NE solar limb is executed in the (1.03-5.0) cm wavelength range. These observations are unique b ecause the solar eclipse was observed with one telescop e simultaneously by two different metho ds. This enables to supplement mutually the data received by observations with two different sectors and gives an opp ortunity to control some obtained results. The angular resolution of the antenna in the horizontal direction is from 17.5 arcsec up to 47 arcsec in the (1.88-5.0) cm wavelength range with the Southern sector and the Flat mirror and from 0.44 arcmin to 1.68 arcmin in the (1.03-3.9) cm range with the Northern sector of the RATAN-600. An average angular size of the prominence source in the sp ecified wavelength range is ab out 30 arcsec. From observations with the Northern and Southern sectors, the p osition of maximum of the prominence radio source have b een found to coincide with the prominence top of the solar image in the He I I 304 line (SOHO, =45o , NE limb of the Sun). The radio fluxes of the prominence were obtained in the wavelength range from 1.03 to 5.0 cm. The fluxes in the range = 1.38 - 4.0(cm) are equal to F()=0.8-0.01(s.f.u.). These values coincide for observations with b oth sectors of RATAN-600, meanwhile the metho ds of the observations and the techniques of data pro cessing of the observations with two sectors were different. The obtained sp ectrum of the prominence defined a thermal mechanism of the prominence radio emission in the (1.03-5.0) cm range. There is a sharp decrease of the prominence radio flux down to value F = 0.02 s.f.u. in comparison with exp ected value for the 1.03 cm wavelength, according to received dep endence F (). Possibly it is caused by the Mo on closing the prominence at the moment of observation. A relative p osition of the Mo on and the Sun at the moment of the solar eclipse maximum phase allowed to estimate the height of the prominence ab ove the photosphere. The derived brightness temp eratures of the prominence are equal to Tb = (5450 - 17900)o K in the (1.84-4.21) cm wavelength range. It was registered a bip olar structure of the radio source asso ciated with the prominence. The degree of circular p olarization of the source is: p = (5 - 10)% for the (1.84-5.0) cm wavelengths. Acknow ledgements. This work is supp orted by the RFBR grant N05-02-16228.