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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. Golubchina, V.M. Bogod, 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 RATAN­600 are discussed. Investigation of the prominence located in the NE
solar limb is executed in the (1.03­5.0) cm wavelength range. These observations are unique
because the solar eclipse was observed with one telescope simultaneously by two di#erent
methods. This enables to supplement mutually the data received by observations with two
di#erent sectors and gives an opportunity 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 (1.88­5.0) cm wavelength range with the Southern sector and the Flat mirror and
from 0.44 arcmin to 1.68 arcmin in the (1.03­3.9) cm range with the Northern sector of the
RATAN­600. An average angular size of the prominence source in the specified wavelength
range is about 30 arcsec. From observations with the Northern and Southern sectors, the
position of maximum of the prominence radio source have been found to coincide with the
prominence top of the solar image in the He II 304 line (SOHO, #=45 o , 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(#)=0.8­0.01(s.f.u.).
These values coincide for observations with both sectors of RATAN­600, meanwhile the
methods of the observations and the techniques of data processing of the observations with
two sectors were di#erent.
The obtained spectrum of the prominence defined a thermal mechanism of the promi­
nence radio emission in the (1.03­5.0) cm range. There is a sharp decrease of the prominence
radio flux down to value F = 0.02 s.f.u. in comparison with expected value for the 1.03 cm
wavelength, according to received dependence F (#). Possibly it is caused by the Moon
closing the prominence at the moment of observation. A relative position of the Moon and
the Sun at the moment of the solar eclipse maximum phase allowed to estimate the height
of the prominence above the photosphere. The derived brightness temperatures of the
prominence are equal to T b = (5450 - 17900) o K in the (1.84­4.21) cm wavelength range.
It was registered a bipolar structure of the radio source associated with the prominence.
The degree of circular polarization of the source is: p = (5 - 10)% for the (1.84­5.0) cm
wavelengths.
Acknowledgements. This work is supported by the RFBR grant N05­02­16228.