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

A new information resource to study solar magnetic field variations and their influence on the Earth extending ordinary lengths of some traditional indices of solar activity is introduced.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

The short-term periodicities of the flare index (FI) which is roughly proportional to the total energy emitted by the flare, are investigated in detail using Fourier transform (FT) for the full-disc and for the northern and the southern hemispheres of the Sun separately over the epoch of almost 4 cycles (1966-2002) which covers 13392 days. Figure 1 shows the power spectra of the three time series of FI calculated for the 289-771 nHz (15-40 days) range with 0.24 nHz interval. The uncertainty in each frequency is ±0.4 nHz due to the 36.5-year data length. The dashed lines indicate the false alarm probability significance levels. In this figure, there are several pronounced power peaks whose significances are enough high. These are at 25.6, 27.0, 30.2 days for the full-disc, 27.0 days for the northern hemisphere and 27.5 and 33.8 days for the southern hemisphere. Since commonly used FT is not able to disclose the possible changes in the periodicities over the period studied, the wavelet transform (WT) was applied to search for temporal variability. The wavelet transform results show that the occurence of periodicities of flare index power is highly intermittent in time. All three FI time series show that the major periods, obtained by Fourier transform are localised in short time intervals (typically up to half of a year).To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

The cause of 92 geomagnetic disturbances in the period of 1997 – 2003 was analyzed. There were used data from LASCO C3 instrument from SOHO satellite, SOHO LASCO CME Catatalog, and the daily average indices Ap. In this contribution we proposed to search sources of the geomagnetic storms taking into account the old idea by Newkirk and Bohlin (1965). According to this idea a solar coronal streamer can cause geomagnetic disturbance when it crosses the Earth's space.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

The investigation of coronal holes (CH) is in progress now thanks to a number of high precise experimental projects and a lot of observations (Ulysses, SOHO, Yohkoh and many others). Historical epoch of CH discovery and study is prolonged today on the new experimental materials. Our considerations of CH and its manifestations in SW near the Earth were connected with minimum, growth and maximum phases of solar cycle. In this work we deal with the descending phase of solar cycle 23. There was the interval of comparatively quite Sun in March 2004, when strong sporadic phenomena were not observed. The existence of long-lived transequatorial recurrent coronal holes on the solar disk allows the investigation it imprinting in SW flows, using Wind data in near Earth cosmic space, data SOHO, Yohkoh and others.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

Here we show that archaeomagnetic measurement confidence interval ($\alpha_{95}$) may serve as a new proxy for the past solar activity estimation. This proxy is compared with sunspot numbers during 1700-2000 yr and with other proxies during 1500–2000 yr.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

We have used most recent archaeomagnetic and ice core $CO_2$ records for the long-term trend correction in global tree ring radiocarbon concentration ($\Delta^{14}C$). The short-term $CO_2$ exchange system was approximated via first order differential equation with frequency dependent coefficients. A generalized multi-scale box model was constructed and used for the reservoir effect correction.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

We present a brief review of published results on the geomagnetic storm effectiveness of CMEs and solar flares as well as of interplanetary events. Attention is drawn to the fact that the published values of storm effectiveness are in conflict with one another. Possible reasons of their differences are discussed.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

The very weak storm-effectiveness of frontside partial halo coronal mass ejections (FPH CMEs) suggests that many, if not most, FPH CMEs are not Earth-directed. Based on the cone model (Zhao et al., 2002) we put forward a method to identify Earth-directed partial halo CMEs from FPH CMEs.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

We present a brief review of scientific milestones of the Russian Space Research Program for 2006-2015 in the field of solar and solar-terrestrial physics and describe several space projects: CORONAS-PHOTON, RESONANCE, CLIPPER, INTERHELIOPROBE, and THERION-F2.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

The Advanced Technology Solar Telescope (ATST) will perform high-resolution studies of the Sun's magnetic fields needed to understand their role in the fundamental processes responsible for solar variability. The generation of magnetic fields through dynamo processes, the amplification of fields through the interaction with plasma flows, and the destruction of fields remain poorly understood. There is incomplete insight as to what physical mechanisms are responsible for heating the corona, what causes variations in the radiative output of the Sun, and what mechanisms trigger flares and coronal mass ejections. Progress in answering these critical questions requires study of the interaction of the magnetic field and convection with a resolution sufficient to observe scales fundamental to these processes.

The 4-m aperture ATST is designed as a unique scientific tool, with excellent angular resolution, a large wavelength range, and low scattered light. With its integrated adaptive optics, the ATST will achieve a spatial resolution nearly 10 times better than any existing solar telescope.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

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