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

To obtain the wave characteristics of hot magnetized plasma, requires investigating a complete dispersion equation describing the oscillations of magnetized plasma, of the form \begin{equation} a+(\omega ^2/k^2c^2)b+(\omega ^4/k^4c^4)c_0=0. \end{equation} Here, \begin{center} $a=(k_{\bot }^2/k^2)\varepsilon _{xx}+(k_z^2/k^2)\varepsilon_{zz}+2(k_{\bot }k_z/k^2)\varepsilon _{xz}$, \end{center} \begin{center} $b=-\varepsilon _{xx}\varepsilon _{zz}+\varepsilon_{xx}^2-(k_z^2/k_{}^2) (\varepsilon _{yy}\varepsilon_{zz}+\varepsilon _{yz}^2)-(k_{\bot }^2/k^2) (\varepsilon_{xx}\varepsilon _{yy}+\varepsilon _{xy}^2)\nonumber +2(k_{\bot}k_z/k^2)(\varepsilon _{xy}\varepsilon _{yz}-\varepsilon_{xz}\varepsilon _{zy})$,\end{center}\begin{center}$c_0=\varepsilon _{zz}(\varepsilon _{xx}\varepsilon_{yy}+\varepsilon _{xy}^2)+\varepsilon _{xx}\varepsilon_{yz}^2-\varepsilon _{yy}\varepsilon _{xz}^2+2\varepsilon_{yz}^{}\varepsilon _{xz}\varepsilon _{xy}$,\vspace*{4pt}\end{center} ω is the complex frequency of the wave, k is the wave number, c is the velocity of light in a vacuum, $k_z$ is the longitudinal (with respect to the magnetic field) wave vector component, $k_{\bot}$ is the transverse wave vector component, and $\varepsilon_{ij}$ stands for the components of the dielectric tensor.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

We report on chromospheric oscillations studied with 15 sec cadence observations obtained at a wavelength of 3.5 mm with the Berkeley-Illinois-Maryland Array (BIMA). Different solar structures, including active and quiet-Sun regions, are analyzed. We compare the high-resolution millimeter 2-D images with Ca II K line images from Big Bear Solar Observatory. Using Fourier and wavelet time series analysis techniques we find signatures of intensity oscillations with periods in the range of 2-7 minutes. We discuss the results in the context of the dynamical model of the solar atmosphere by Carlsson & Stein (1995, 1997).To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

Archival full disk observations of the central depth of Mn 539.467, a photospheric line, have been found to correlate with chromospheric Ca K intensity. In this paper we present spectroheliograms taken in Mn I 539.467 and 542.32 nm lines and other nearby lines to see if the other photospheric lines show chromospheric structures. We see both Mn images and also Si I 542.118 mimic magnetograms the similar way, while strong Fe and Ti lines only faintly reveal magnetic features, and weak Fe lines of comparable strength to Mn show nothing.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

We provide an observational proof of the existence of the global sausage mode oscillations in a flaring loop studying a microwave burst with quasi-periodical pulsations observed with the Nobeyama Radioheliograph (NoRH).To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

This paper presents the results of the active region observations in red coronal line ($\lambda = 6374 \stackrel{\circ}{\rm A}$). The analysis was made of the dependence of the profile parameters of the red coronal line on the exposition value.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

Changes in Total Solar Irradiance (TSI) were studied both in time-frequency and in time-longitude aspects. The continuous wavelet analysis of TSI composite time series (Fröhlich & Lean 1998; Willson & Mordvinov 2003) revealed that the energy of thermomagnetic disturbances due to sunspots and faculae cascades into the magnetic network and facular macrostructure. The time-longitude analysis revealed large-scale patterns of radiative excesses in solar atmosphere. These patterns are organized into 2- and 4- sector structures exhibiting the effects of both activity complexes and magnetically active longitudes. Large-scale patterns with radiative excess display a facular macrostructure. These temperature patterns are causally related to long lived magnetic fields of the Sun. During activity cycles 21–23 the patterns with radiative excess tend to be concentrated around the active longitudes which are centered at about 60° and 230° in the Carrington system (Benevolenskaya et al. 1999; Mordvinov & Willson 2003).To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

A sufficiently thick and dense flaring magnetic loop is shown to be able to support global sausage magnetoacoustic modes. The oscillation period of this mode, calculated in the straight cylinder approximation, is determined by the length of the loop, not by its diameter, as it has previously been assumed. For the existence of this mode, the ratio of the loop length to its diameter is to be less than about a half of the square root of the density contrast ratio. This mode has a maximum of the magnetic field perturbation at the loop apex and nodes at the footpoints. We demonstrate that the 14-17 sec quasi-periodical pulsations of microwave emission, oscillating in phase at a loop apex and at its legs, as observed with the Nobeyama Radioheliograph, are interpreted in terms of the global sausage mode.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

We represent results of experiments on investigation of solar wind plasma by the method of radio sounding, when the signal from the radio source paths through the solar wind plasma and then it's received at ground-based radiointerferometer.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

The CCD spectroheliograph-magnetograph is a focal plane ancillary instrument for Pulkovo horizontal solar telescope ACU-5. The instrument is placed at an exit port of an isothermal high-resolution diffraction-grating spectrograph. The modified Leighton optical scheme for registration of sunspot magnetic fields is used. The instrument provides obtaining FITS digital video cards of radial velocities, magnetic fields and spectroheliogram in any line of spectral region 3900A - 11000A. The time of obtaining of one video card by the size 91″ $\times$154″ is equal 10.24sec. The angular resolution of the instrument is 0″.8; spectral resolution is 0.01-0.03A. There is remote access to a solar telescope in real time on the basis of Internet - process engineerings.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html