Since its launch on 2 December 1995, the joint ESA/NASA SOHO mission has provided a wealth of information about the Sun, from its interior, through the hot and dynamic atmosphere, to the solar wind and its interaction with the interstellar medium. At the same time, SOHO's easily accessible images and movies have captured the imagination of the science community and the general public alike. This article summarizes some of the key findings from 8 years of SOHO.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

The Dutch Open Telescope (DOT) on La Palma is an innovative solar telescope combining open telescope structure and an open support tower with a multi-wavelength imaging assembly and with synchronous speckle cameras to generate high-resolution movies which sample different layers of the solar atmosphere simultaneously and co-spatially at high resolution over long durations. The DOT test and development phase is nearly concluded. The installation of an advanced speckle processor enables full science utilization including “Open-DOT” time allocation to the international community. Co-pointing with spectropolarimeters at other Canary Island telescopes and with TRACE furnishes valuable Solar-B precursor capabilities.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

Observations of the Sun are always complicated by the thermal influence of the integral flux of its radiation on the optical-mechanical and photo-detecting units of the telescope. This influence manifests itself especially strong and can be even amplified while observing the Sun from the space, and mostly while observing its full disk. However, the existing optical solar telescopes produce an image of either full disk of the Sun or only one individual region. In the latter case, the radiation of almost full disk of the Sun is cut off from the telescope, and emission from a small region on its surface propagate through a small aperture on the optical axis of the telescope (see, for example, Popov (1988); Stix (1991). The third variant is a solar coronagraph, which constructs an image of the solar corona, cutting off radiation of the whole disk of the Sun, thus imitating a total solar eclipse (Lyott, 1939; Nikolsky 1966; Smartt 1998). This solution determines success of the solar experiment in the space, particularly, if it is connected with long-term high-precision photometric and coordinate measurements of temporal variations of the diameter and shape of the solar disk limb.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

Valuable large archive of solar radio observations has been accumulated by the Pulkovo solar radio group. But big part of data is recorded on paper. We describe a method and software for transferring data recorded on paper to FITS format.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

The paper presents study of the influence of coronal inhomogeneities on the average temporal pulse profile of radio emission from a compact solar pulse source located near the photosphere of the Sun. To consider both scattering and refraction of the radio emission propagating through the solar corona an integral representation of the wave field in the form of the interference integral is used. Thus formation of regular and random caustics and focuses as well as multipath structure of the radio emission received on the ground are taken into account. A numerical simulation of the average pulse profile, carried out for different parameters of the solar corona turbulence has shown that near-solar plasma can distort the emitted pulse significantly to form several pulses.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

More than 300000 images of the Sun have been acquired during the SPIRIT experiment with 10 telescopic and spectroheliographic EUV and X-ray instruments aboard the CORONAS-F satellite. We have developed methods and routines for the first-level data processing to make the SPIRIT data easy for use in a way similar to that one for SOHO/EIT images.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

The wide range frequency observations at microwaves with high spatial resolution open new ways in developing the solar physics today. They may result in most sensitive diagnostics of the upper chromosphere, TR, and corona in respect to the following parameters: - magnetic fields strength and structure; - plasma density; - periodic oscillations of plasma structures; - plasma oscillations; - temperature. The situation has been demonstrated by using a number of modern radio telescopes of interferometer type: radio heliographs at Nobeyama and Badary (SSRT), multi-element interferometer VLA. Each of them has its own important parameters, but in limited sphere of applications. In this presentation we discuss some results obtained with the reflector type instrument RATAN-600 anf possible directions in developing its parameters. The parameters of the RATAN-600, used now at the solar observations are summarized below. The most important are:

1. - high collecting area (about 1000 m2) and high flux sensitivity;

2. - wide wavelength range (1.7÷30 cm);

3. - high spectral resolution (∼5%);

4. - high polarization sensitivity (better than 1%).

1. - one-dimensional resolution (about 15 arcsec at wavelength 17 mm);

2. - limited guiding system.

Results of the new observations of long existing microbursts (MB) are presented. It is revealed that the MB spectrum can have the details with the narrow frequency band $(\Delta f/f <0.03)$. It was earlier marked [Bogod, Mercier & Yasnov (2001)] that the MB arise together with noise storms. In the given observations is detected that MB may be connected with a flare and have arisen about 1.5 hours prior to a flare. For the first time it was possible to register MB, which degree of polarization is less 1 (from 0 till 0.16).To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

Comparison of solar magnetic fields observed with various telescopes and/or in different spectral lines is important to verify the data reliability from instrumental points of view, and to determine some physical processes responsible for the origin of polarized emission in the solar atmosphere with extremely complicated distribution of magnetic and thermodynamic parameters in an aperture of observation and along the line-of-sight. When compared observations use the same line, and data reveal a significant systematic discrepancies, the question arises about the reasons of that. If compared data are obtained in different spectral lines, the existence of differences between them could be related to peculiarities of the polarized emission formation in one or another line. In this case the question arises - data in which line are more reliable? This problem is especially acute with regard to observations in the FeI $\lambda$525.02 nm spectral line due to the big Lande factor ($g = 3.0$) and low excitational potentional of this line. Recently this problem has become especially urgent for some space weather tasks. Both the analysis of this problem and main bibliographic references can be found in [1].To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

Oscillations of the magnetic field in sunspot umbra have been detected by Pulkovo CCD spectroheliograph-magnetograph. The manifestations of 3- min oscillations in the power spectra of magnetic field variations are not very strong and can be seen only in a number of larger sunspots. Their power is concentrated in isolated small regions of the boundary between umbra and penumbre of large spots. The waves are produced in short bursts with coherence times of about 10 min. In the sunspot umbra, 30-40 min modes have been also confidently revealed.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

In Eselevich V. and M. Solar Phys. 195, 319, 2000 is shown that in brightness rays of the streamer belt from time to time there exist additional plasma streams of enhanced density moves antisunward and occupies a separate ray. The duration of additional streams can range from a few hours to several days. For that reason, some of them may be categorized as sporadic SW streams and the others as quasi-stationary SW streams. Preliminary investigations showed that the leading edge of such streams can be extremely small in width. The purpose of this paper is to verify the conclusions about the existence of additional plasma streams with steep fronts in streamer belt rays, based on analyzing the calibrated data from LASCO/SOHO C2 and C3.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

The 1N/M7.6 flare of 24 October 2003 at S19E72 were well observed by RHESSI, TRACE, NORH, and the Spectrograph at the Purple Mountain Observatory. After analyzing all the data collected, we established a scenario of the flare and compared it with the standard cartoon of solar flares (e.g., Dennis 1988).To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

Solar energetic particles generated in solar proton events produce in SOHO/EIT (and LASCO) images well-known ‘snowstorm’ effect which interferes analyses of those images. Similar ‘snowstorms’ are also observed in TRACE and CORONAS-F/SPIRIT images due to particles continuously present in the radiation belts and polar caps.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

Analysis Wavelet-spectra has shown that in the with earlier our works, in a field of brightness of thin structure of photosphere scales of formations of granules, protogranules, and mezogranules come to light.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

We study variations of the solar large-scale magnetic field (LMF) with period $\approx$1.0–1.3 years by observational data of Stanford (1976–2004) and Kitt-Peak (1970–1984).To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

In our contribution we introduce the new Interferometric BIdimensional Spectrometer (IBIS) and present the first results on bisector velocities of two dimensional spectral scans in FeI 7090.4 Å comparing granules and intergranular regions.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

The CORONAS project is aimed at observation of the Sun in the wide wave-range. The CORONAS-I satellite has been launched to an orbit on 2 March 1994, the CORONAS-F satellite has been launched on 31 July 2001 (see for example Kazachevskaya et al., 1998; Oraevsky et al., 2002). Solar Ultraviolet Radiometer — SUVR provides measurements in the wavelength region $\lambda < 130$ nm and also in the line $L_{\alpha}(\lambda = 121.6)$nm. (Kazachevskaya et al., 1998).To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

We discuss the polarization signals produced in recent realistic 3D simulations of solar magnetoconvection. The Stokes profiles of the Fe I 6301.5, 6302.5, 15648 and 15652 $\mathrm{\AA}$ Zeeman-sensitive spectral lines are synthesised and smeared to simulate the image degradation caused by the Earth's atmosphere and finite telescope resolution. A Principal Component Analysis approach is applied to classify the profiles. We find that the classes of Stokes $V$ profiles as well as their amplitude and area asymmetries are very close to the observations in the network and inter-network regions.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

The map of the large-scale chromospheric Doppler velocities ($VD$) on the solar disk, obtained from 2D-spectroscopy within the HeI 10830 Å line for June 4 2002, is presented. Velocity field structures larger than the supergranulation cells are studied. Statistical relations between $VD$ and 1) the intensity in the core of the HeI 10830 Å line and 2) the sign and strength of the longitudinal photospheric magnetic field are obtained and discussed.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

The coincidence was observed between the places with weak (probably inverse) photospheric longitudinal magnetic fields in the big spot of the AR NOAA 8340 prior to the start of the flare and a common base of the giant arches (loops) and centers of emission visible in the HeI 10830Å line core during the flare. A number of observational facts compel us to make a supposition that the flare was the consequence of an injection of plasma from the places with marked peculiarity of the photospheric magnetic field into the expanding magnetic arcade.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html