K H A S S M. Abstracts...

	Multi-wave station of solar monitoring
	Abstracts of principal works

1. CCD-observations of the Sun at the Balmer and Pashen continua. // AApTr v.18, 1999 - in press

Kurochka L.N. (AO of Kiev University, Ukraine),Astronomical Observatory of Kiev University, Astronomicheskaya st.3, Kiev 254053, Ukraine;
Belkina I.L., Beletsky S.A., Korokhin V.V., and Marchenko G.P. Astronomical Observatory of Kharkov St. University, Sumskaya st. 35, Kharkov 310022, Ukraine.

A preliminary results are presented of the solar CCD observations at the Balmer and Pashen continua and at the Balmer precontinuum. The Balmer precontinuum intensity distribution for the emission features of a.r. 7890 NOAA/USAF are obtained. A limits of electron density in the plasma volume along the line of sight are evaluated for a emission feature from this a.r. Solar monitoring at the hygrogen series continua and precontinua appears to have considerable promise.

2. Observations and Analysis of Emission from Solar Active Regions at the Edge of Balmer Continuum. //Astronomicheskiy Zhurnal., 1997, v(t)74, N3,p(s)460-465.

Kurochka L.N. (AO of Kiev University, Ukraine),Astronomical Observatory of Kiev University, Astronomicheskaya st.3, Kiev 254053, Ukraine;
Belkina I.L., Beletsky S.A., Korokhin V.V., and Marchenko G.P. Astronomical Observatory of Kharkov St. University, Sumskaya st. 35, Kharkov 310022, Ukraine

The first results of CCD observations of the Sun in Balmer and Pashen continua and in the Balmer precontinuum are presented. The intensity distribution in the Balmer precontinuum in a knot of the active region NOAA/USAF 7890 provides information about inhomogeneities in the electron density of the plasma along the sight line. The value of conductiong monitoring observations of this kind is argued.

3. Equatorial coronal holes from the observations at HeI 1083nm wings//conference at crimean astrophysical observatory, by Belkina I.L., Beletsky S.A., Korokchin V.V., Marchenko G.P.,-Astronomical Observatory of Kharkov St. University, Sumskaya st. 35, Kharkov 310022, Ukraine

The mean ratio of the HeI line intensity (image) blue wing ( Ib ) to that of the red wing ( Ir ) for ten equatorial coronal holes and the unipolar quiet regions has been found from the solar CCD-images taken at l = 10827A and l = 10837A for ten dates of 1995. The main intensity ratio is Ib/Ir = 0.73±0.02 for the coronal holes and Ib/Ir=0.81 ± 0.03 for the unipolar regions of the quiet chromosphere. For the coronal holes and the unipolar parts of the quiet Sun these ratios correspond to the Doppler shift of 0.04A and 0.027A towards the blue, and also to the area averaged outflow velocities of 1.3kms-1 and 0.7kms-1 respectively. Accounting the existense of the fine structure elements in coronal holes with the radial outflow speed of 8kms-1 it has been found these elements to be covered about 10% of the whole coronal holes surface.

4. Solar Flare from the HeI 1083nm CCD Observations on August 27, 1995// UAA_IV
Belkina I.L., Beletsky S.A., Korokhin V.V., Marchenko G.P.
Astronomical Observatory of the Kharkov State University

As soon the HeI 1083nm chromospheric emission is largely determined by the coronal shortwave radiation, dynamics and morphology of phenomena occuring on the solar disk at He line during the hard solar emission burst are very interesting. In this work the results of the HeI 1083nm observations of event related with August 27, 1995 X-ray burst and chromospheric H-alpha flare have been analized. The observations have been carried out using the Kharkov St. Univ. AO spectroheliograph with CCD-photometer. The instrument, means of observational data reduction and constructing maps of HeI 1083nm line depth distribution over solar disk have been described in "Kinemat. and Phys..." 1996, v.12, N2, p.65.
During an hour, from 08h16m to 09h15m UT, nine digitized images of the full solar disk have been taken at this line with spatial resolution about 8 arcsec. According to SGD (N618 pt.II) the X-ray burst has been registered by GOES (B4.6 beg. 08h35m, max 08h52m, end 10h10m) and patrol observations at the SVTO station marked H-alpha flare (SF, beg. before 08h52m, max 08h53m). From our helium images only two first have been registered before the X-burst onset. Our studies of the temporary HeI 1083nm line depth variations in active region 7901 NOAA /USAF show: 1. The He-line depth variation at the H-alpha flare place starts before the H-alpha flare. At 08h40m UT the line depth begin to decrese and goes on until the value about 1% of continuum intensity is reached in a moment near the burst maximum. The later (from 09h01m UT) images show the increasing line depth. It is suggested a subflare may be observed in emission at a time of the burst maximum. 2. Before a burst maximum the increasing of the line depth was substational (up to 10%) almost throughout the whole a.r. The temporary line depth variation is obtained for different parts of a.r.
3. The comparison of the He-line observations with the photospheric magnetic field structure from the Kitt-Peak data has been shown the H-alpha flare to be located near neutral magnetic field line. For period nearby the burst maximum (08h46m-08h51m) the directions along which the He line depth variation was the most have been clearly manifested. These are near the neutral line of photospheric magnetic field. It seems the directions are determined by the magnetic field of the coronal excited loops

The work is carried out in the frames preporation of the Russian-Ukrainan sattelite project "Photon" and is supported by Ukrainan National Cosmic Agency, contract N6-117/96, UNCA-KhStU.

5. CCD-observations of the Sun HeI 1083nm, Ha and K Ca II lines// Kinematika i fizika nebesnyh tel., 1996, v(t)12, N2,p(s)65-76.
by Belkina I.L., Beletsky S.A., Gretskij A.M., Marchenko G.P.
Astronomical Observatory of Kharkov St. University, Sumskaya st. 35, Kharkov 310022, Ukraine.

The digitized monochromatic images of the Sun in HeI 1083nm, Ha and K CaII are obtained on the spectroheliograph with the CCD photometer of the Kharkov University Astronomical Observatory. Optical characteristics of the CCD receiver operating in the monochromatic regime are studied from optical to the near IR spectral range. We present the algorithms and software to remove the drawbacks inherent in this class devices. The Ha and K CaII images obtained during 1993 July-Avgust and 1994 June-October seasons (when chromospheric flares and other nonsteady processes occurred) were used to determine heliographic positions and intensities for the solar activity patrol program. The HeI 1083nm image sets were used to study line depth changes during the development of two chromospheric subflares and accompanying filaments. These flares were observed in absorption only. The tangential velocity of propagation of the perturbation in one of the filaments is evaluated.

6. Observations of jupiter, the moon and the sun with the one-dimensional ccd detector, by V.V.Korokhin, L.A.Akimov, G.P.Martchenko, O.M.Starodubtseva - Astronomicheskii Vestnic, 1993, v.25, No 3, pp.56-64 [Solar System Research (Engl. transl.), 1993, v.25, No 3, pp.252-259]

The photopolarimetric complex, which was made on the basis of a one-dimensional CCD, is described. It was used for the following astrophysical investigations: polarization observations of Jupiter, mapping the Lunar surfase physical characteristics, making the Solar images in the K CA II, H and He I 10830 A spectral lines.

7. Software system <IRIS> as prototype of data processor for the Ukrainian solar service
//conference at crimean astrophysical observatory, by Beletsky S.A., Korokhin V.V., Velikodsky Yu.I.,-Astronomical Observatory of Kharkov St. University, Sumskaya st. 35, Kharkov 310022, Ukraine, e-mail:wk@astron.kharkov.ua