PROBLEMS OF GEOCOSMOS

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Proceedings of the 7th International Conference "Problems of Geocosmos" (St. Petersburg, Russia, 26-30 May 2008) Table 1. (Continuation) Project Time interval Physical experiment Amount of data Meteor-3M 01.2002 - 12.2003 Tatyana 02.2005 - 02.2007 Cosmos 1686 02.1986 - 12.1986 MIR orbital station – radiation experiment (Ryabina) MIR orbital station – gamma experiment (Grif) 11.1990 - 06.2000 Differential spectra of electron and ion (proton) components of corpuscular radiation in Earth's magnetosphere Flux of charged particles in Earth's magnetosphere Flux of charged particles in Earth's magnetosphere Flux of charged particles in Earth's magnetosphere 6Gb 430Mb 150Mb 70Mb 10.1995 - 06.1997 Flux of gamma and X-rays 1.5Gb Prognoz-9 06.1983 - 03.1984 Flux of gamma and X-rays 20Mb User can build his request to the comprehensive database we possess with just a few clicks using our data forms. First, the user has to select the spacecraft he is interested in. Then, the time interval and the channels to retrieve must be selected. After that, the user has to select the representation of the data that he needs. Figure 1. Example of data retrieval form. Data retrieved can be provided as text, graphic or as an archive. The visual representation allows to graphically preview the data to determine whether or not it is actually of interest in the context of a particular problem. The textual representation usually serves error catching, value confirmation and debugging purposes, since it dumps a portion of the data table directly into the user's web interface. The archived representation is useful for retrieving large amounts of data for subsequent client-side processing. Data visualization is performed by our inhouse software project Qlook [7]. 207
Proceedings of the 7th International Conference "Problems of Geocosmos" (St. Petersburg, Russia, 26-30 May 2008) In order to assist researchers attempting to develop their own software for processing spacecraft telemetry data, we provide FTP access to communication session files for most SINP space experiments. Currently, telemetry data for Universitetsky-Tatyana is already available; we are planning to deploy data for Coronas-F/I, Mir station, Prognos-9 and other spacecrafts in the nearest future. Supplemental information Besides spacecraft data and telemetry, SMDC also contains processed and analyzed datasets. They have been built based on space experiment data available at SMDC as well as at other data centers. Magnetic Storms catalogue. We have analyzed data produced by the OMNI project to detect magnetic storms and to separate them from the general data flow. Only magnetic storms with Dst less than -70 nT have been selected in the 1998-2003 time interval. Data on these magnetic storms includes interplanetary magnetic field components, solar wind bulk velocity, proton density, Dst and AL indices. There's also a Dst threshold selector which allows to view only storms during which Dst index reaches a particular value. Solar flares. It is well known that the Sun is the most energetic particle accelerator in the Solar system, producing ions of up to tens of GeV and electrons of up to tens of MeV. The information regarding peak gamma emission energy obtained by the SONG experiment allows us to estimate the flux and spectra of charged particles accelerated in the Solar atmosphere. The CORONAS-F duty cycle of solar flare detection lasted approximately 40% of its total flight time as a consequence of its orbital parameters; thus many major flares that occurred since August 14, 2001 till September 12, 2005 were not observed. Yet, 9 flares with HXR emission have been detected by CORONAS-F during 2004 and 23 ones during 2005. Data on HXR and gamma fluxes produced by solar flares and detected by SONG (CORONAS-F) experiment [2004-2005] is available at SMDC. APEV database. This tool provides access to time profiles of the key geomagnetic and solar wind parameters and solar event maps. APEV database has been initially developed by by Alexei Dmitriev, Andrey Zhukov and Igor Veselovsky [2]. Coronal holes database. This tool provides access to a large catalogue of solar imagery automatically processed [3] to detect and measure coronal holes (CH), as well as their numeric characteristics. Solar images are taken from SOHO/EIT measurements data bases. CH area is measured in relative units, where total area of the Sun equals one unit. Minimal significant area is 0.002 relative units. Average intensity is calculated after filtering and histogram scaling into the range from 0 to 255. Calculation is performed not taking into account correction for spherical shape of the Sun. This tool is based on an earlier work by J. Shugai and SOHO/EIT consortium. Magnetopause crossings. It has been demonstrated [4] that the shape of the Earth's magnetosphere depends upon the IMF orientation, while remaining self-similar for variations in solar wind dynamic pressure. Data set of 1821 magnetopause crossings has been processed and matched with simultaneously observed hourly averages of solar wind dynamic pressure and IMF Bz. The data set used includes data collected from IMP 1/2/3/4/6/8, Explorer-33, Prognos 7/8/10, ISEE 1/2, IRM spacecraft. SMDC portal provides full access to this data set, which covers the time period from 07.08.1968 through 21.02.1979. 208
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vertical fields. The vertical field
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Introduction ON THE NATURE OF PLASM
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Vy Here index j =1,2 characterizes,
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Fig. 3. Dependence of 1D interpreta
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2. Burlaga & Klein method. The main
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PROBLEMS OF GEOCOSMOS

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