The existence of the enigmatic X-ray emission extended along the plane of our Galaxy, and also discovered in other galaxies, puzzled the astrophysicists around the world for more than 25 years. Due to research carried out in our group in 2006-2008, a solution of this problem emerged. To verify our hypothesis that the Galactic Ridge X-ray Emission is the cumulative emission of a great number of weak X-ray sources, a key experiment was needed, namely ultradeep (with a flux limit of 1å-17 erg/s/sq.cm) observations of a region of the Galactic ridge with an instrument having an angular resolution of at least 1-2 arcseconds. In 2008, such observations, with a total exposure of 0.9 million seconds, were performed by the Chandra orbital observatory following our proposal. Our analysis of all the available observations (nearly 1 million seconds) of this field has confirmed the estimates we did previously based on indirect arguments and has led us to the following conclusions:

1. In a typical Galactic Ridge region, a large number of faint X-ray sources is detected, with a column density of 100 thousand sources per square degree,
2. 88 +/-12 % of the Galactic Ridge X-ray Emission in the energy range 6-7 keV is resolved into discrete point sources,
3. Ihe integrated sources counts as a function of flux is in good agreement with the numbers of sources expected from the statistics of X-ray sources in the solar neighborhood. These results are published in the Nature journal.

Fig.1. Simultaneous observation of two beamlet with essentially different energies which were accelerated in the CS at different resonant sources R1 and R2.	Fig.2. Geotail observation of quasi-steady energy collimated ion beamlet which was accelerated in the distant CS at the region of closed magnetic field lines.

1. Grigorenko, E. E., M. Hoshino, M. Hirai, T. Mukai, and L. M. Zelenyi, J. Geophys. Res., 114, A03203, doi:10.1029/2008JA013811, 2009.
2. Grigorenko E.E., L.M. Zelenyi, M.S. Dolgonosov, J.-A. Sauvaud, Spatial and temporal structures in the vicinity of the Earth’s tail magnetic separatrix. Cluster observations, Book of Proceedings of 15th Cluster Workshop and CAA School, p.p. 435-453, 2009.
3. E. Grogorenko, R. Koleva. Variability of discrete plasma structures in the lobe-plasma sheet interface, Compt. Rend. Acad. Bulg. Sci. v.62, No11, p. 1449-1456, 2009.

Numerous experimental data testify that the geomagnetic storms, generated by the different interplanetary phenomena, manifest themselves in different development of disturbances inside magnetosphere. On the basis of the OMNI archive data on interplanetary conditions during 1976-2000 we made statistical analysis of interplanetary drivers of 798 geomagnetic storms with Dst < -50 nT. We categorized various large-scale types of solar wind as interplanetary drivers of storms: corotating interaction region (CIR, 145 storms), Sheath (96), interplanetary CME (ICME) including magnetic cloud (MC, 62) and Ejecta (161), and drivers for 334 storms (”Inde- terminate” type) have not been determined because of data gaps for numerous intervals of solar wind. To make the given analysis, we used for the first time a method of double superposed epoch analysis which uses two reference times: onset of magnetic storm and the minimum Dst index (see Figure). On the one hand, by means of this method the earlier received results have been confirmed, and on the other hand, new results are received:

1. For the first time clear indications that there are distinctions in efficiency of two subclasses interplanetary ÑÌÅ (MC and Ejecta) and also Sheath before them have been received (see figure)
2. The fact that there is «a memory of prehistory» for process of generation of a magnetic storm has been confirmed by independent method

Figure 1. Temporal variations of electric field Ey, Bz component of interplanetary magnetic field (IMF), magnetospheric Dst* and AE indexes(left ), B, Bx components and magnitude of IMF, ratio of thermal to magnetic pressures (plasma beta-parameters) for different interplanetary drivers(see designation under figure). Durations of main phase of all storms have been re-scaled in a such manner that, respectively, onsets (left dashed line, time”0”) and minima of Dst index (right dashed line, time “6”) for all storms coincide.

For the first time a proportionality of the flare plasma temperature to the logarithm of hard X-ray intensity was discovered during pre-flare and impulsive phases of the 2006 December 6 solar flare. The hard X-ray intensity was estimated from count rate of the anticoincidence system of the spectrometer on INTEGRAL (ACS SPI) with energy threshold of 80 keV for gamma-quanta. Moreover non-thermal processes were observed about 5 min earlier than the onset of thermal emission. These demonstrate that electrons generating hard X-ray intensity have been an initiator and main source of flare plasma heating, the particle acceleration and the plasma heating is a system with positive feed back. The proportionality disappears after beginning of plasma expansion, when plasma cooling becomes more effective than its heating by non-thermal electrons. These effects were not observed earlier due to low sensitivity of detectors (for example, NASA RHESSI). Preliminary analysis of some other events confirms our findings.

1. A. Struminsky and I. Zimovets, OBSERVATIONS OF THE 2006 DECEMBER 6 SOLAR FLARE: ELECTRON ACCELERATION AND PLASMA HEATING, Astronomy Letters, in press 2010.
2. A. Struminsky: ‘Relationship between plasma temperature and HXR intensity from INTEGRAL’, WorkGroup 2, 9th RHESSI workshop, September 2009, Genova, Italy
3. A. Struminski: ‘Cross calibration with Anti-Coincidence System of Spectrometer on INTEGRAL (ACS SPI)’, WorkGroup 3, 9th RHESSI workshop, September 2009, Genova, Italy
4. A. Struminsky and I. Zimovets, PARTICLE ACCELERATION AND HEATING OF SOLAR FLARE PLASMA, The Sun: from active to quite, International Coronal Workshop, 19-23 October, 2009, FIAN, Moscow, Russia.