The $\bf {E \times B}$ drift allows plasma to move through the magnetic field lines and may contribute to various motions inside the Sun (e.g. to explain the adverse gradient of differential rotation in the equatorial zone), at its surface and in the corona. Here we treat an example: using a given azimuthal angular frequency $\omega$(r, $\theta$), rather arbitrary, and the corresponding exact solution for $\bf{B}$, we obtain $\bf{E}$ and the drift velocity. The latter is comparable with the original velocity, but has components in all directionsTo search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

Height series of Doppler observation in $H_{\alpha}$ and $D_3$ spectral lines of solar spicules obtained by big coronagraph (53 cm) of Abastumani Astrophysical Observatory have been analyzed. Time duration of each height series was 7 s. Totally 8 different heights from the photosphere were covered. Spatial difference between neighboring heights was 1 arc sec. We found the periodic spatial distribution of Doppler velocities during height series in certain spicules. We suggest that the periodic spatial distributions are caused by propagating or standing kink waves. The wave length is found to be in the range 3500–4000 km which probably indicates to the granular origin of the waves.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

Based on analyzing the fine structure of time series of solar and heliospheric parameters a universal numerical technique is developed to study large-scale patterns of solar activity and the heliospheric structure. The Solar Mean Magnetic Field (SMMF) time series and the magnetic fields in solar corona (Hoeksema & Scherrer 2004) were studied in time-longitude aspect (figures 1a,b,c,d). It is shown that the behavior of the large-scale magnetic field, its multiperiodic rotation determine the heliospheric structure and changes in space weather (Mordvinov & Plyusnina 2004). Time-longitude analysis of Interplanetary Magnetic Field (IMF) near the Earth (King et al. 2004) reveals similar diagram (figure 1e) shifted relative to the photospheric and coronal magnetic fields by the transport time.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

The possible mechanism of cosmic ray influence on clouds formation in the atmosphere is considered. Ionization of the atmosphere caused by cosmic rays can lead to the formation of condensation centers. But at the same time interaction between cosmic ray and the atmosphere might change transparency of the atmosphere and the atmospheric temperature, too. Calculations of changes of the condensation growth rate of water drops due to changes of the temperature have been performed. This effect can provide an increase in a few percents of growth rate of drops. This can explain the observed correlation between cloudiness and cosmic ray intensity.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

Available YOHKON, TRACE, SOHO/EIT and CORONAS-F data are interpreted as evidences of the non-local coronal mass ejection initiation processes when rapidly increasing electric currents appear in the coronal loops and arcades. These electric currents are driven by subphotospheric processes. Self-similar plasma motions are due to the electric drifts in crossed inductive electric and magnetic fields. Expanding non-planar loops often mimic “reconnection” features, being in reality projection effects of the “twist and fold” processes on the image plane. Among such patterns one can find examples of spurious x-points, concave fronts, blobs, islands, etc. Coronal mass ejections often proceed without large scale topological changes of magnetic fields. They are accompanied by enhanced small-scale turbulence.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

We model hot collisionless solar corona/slow solar wind (SW) by kinetic Vlasov equation. The equatorial region with an unprescribed magnetic field is under electromagnetic action, and we have formation of a 3D Quasi-Stationary Coronal Structures (QSCS) in the current-carrying (CC) plasma with SW flows. The QSCS are generated via electromagnetic mode development in plasma having anisotropic velocity distribution function (VDF). As a result we get streamers like stratification mode, CMEs like tearing mode and heliospheric sheet like pinch mode in anisotropic plasma. The scales in the QSCS are defined via angle dependent magnetic Debye scale. The scale itself depends on value and sign of plasma anisotropy parameter which is calculated for postulated plasma VDF.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

The results of complex investigations of solar and interplanetary large-scale magnetic fields (LSMS) are set out. A rotation of sector structures of several types of LSMF was studied analysing evolution of their primary (main) rotation periods. It is confirmed the changing of Sun's rotation regime in the middle of century XX.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

To explain the origin of hard X-ray emission, we suggest the internal shocks could be created in the reconnection jet and accelerate the energetic particles in the solar flares. We examine its possibility by performing 2D resistive MHD simulations. We use very small very small grid to resolve the diffusion region and remove the effect of numerical noise. As the results, the current sheet becomes thin by tearing instability, and collapses to Sweet-Parker sheet. It becomes unstable again so that the secondary teaing instability occurs. Immediately after the plasmoid ejection, anomalous resistivity sets in and Petschek-like reconnection starts. During the Petschek reconnection, many plasmoids are created by the secondary tearing instability and ejected along the current sheet. The multiple fast shocks are created in the current sheet. We suggest that the internal shocks shown in this paper are possible sites for the particle acceleration in the solar flares.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

After briefly summarizing the outstanding achievements and new tendencies witnessed in recent years in the studies of magnetic fields of solar active regions (ARs), we focus on the current understanding on flux appearance and disappearance. On flux appearance, the moving magnetic features (MMFs) stand still as a mystery in solar physics, although the emergence of magnetic flux in the bipolar form are fairly understood. However, the possibly sympathetic flux emergence of several ARs and the appearance of active longitudes or hot spots are poorly understood. The only confirmed model of flux disappearance is the observed flux cancellation. Detailed analysis of the alignments of transverse magnetic fields and the history of magnetic flux evolution suggest that flux cancellation is more likely to be the magnetic reconnection in the lower solar atmosphere. Magnetic and current helicity provide new diagnosis in understanding flux emergence and disappearance, and constrains the energy process in solar activity.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

Many records of climatic and environmental changes based on various proxy data exhibit distinct cyclicities that have been attributed to extraterrestrial forcing such as changes in solar activity. To study the long-term changes of solar activity, different data sets of solar activity, both indirect data (the Schove series) and proxy data (cosmogenic isotopes) were analyzed. Both sets of solar activity clearly show centennial and millennial changes.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

Long-term behaviour of the interplanetary magnetic field is compared with that of the quadrupole harmonic of the solar axisymmetric magnetic field. Substantial correlation between them is found both on the time scale of 22-yr cycle and on the shorter time scale of several years.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

Transits of Venus occur in pairs 8 yr apart, the pairs separated by intervals of either 112 or 130 yr, because of the pattern of approximate orbital resonances. Transits of Mercury show a different pattern, partly because of the more eccentric orbit, and also because the structure of the approximate resonances is different. The near-resonance in Venus' axial rotation strongly suggests a tidal link with the Earth.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html