Proceedings of the 33

Effects of long-term variations of solar wind parameters in near-Earth space. In this paper we use the simple 2D model of the turbulent electromagnetic field: particles move in the neutral plane of the Earth's magnetic tail.

Figure 2. Panel (a): Power law exponent of structure functions as a function of its order for different values of β

INDICES OF HUMAN URINARY EXCRETION OF THIOL AND

UROCHROME IN THE ANTARCTIC AND THEIR CORRELATION TO COSMOGEOPHYSICAL FACTORS

The intradiurnal dynamics of fluctuations of Σsh, Csh, Σur and Cur for the entire period of the study and for the periods of polar night and polar day were also studied. For the first time, a screening analysis of the thiol content in urine was carried out during a long-term stay and work in extreme conditions in Antarctica (judging by the works known to us).

Fig. 1. Dynamics of daily average values of urine samples number (n, 1/day) within synodic month

ON MANIFESTATION OF PERIODICAL DISTURBANCES OF INTERPLANETARY MEDIUM IN FLUCTUATIONS OF UNTIL

Introduction

Mesorhythms and circannian fluctuations in the dynamics of unithiol test results

It is noted that the correlations between CF of UOHT and SA and between CF of UOHT and ET and EE are inverse, which indirectly proves that the highly cosmophysical factors, especially SA and ET, have physical interrelationships. Moreover, there is no observable direct relationship between CF of UOHT and SA variations, while the correlation between CF of UOHT and ET and EE appeared clearly modulated by changes in SA over the 21-year cycle.

Cycles of planet interactions in the Solar system and fluctuations in unithiol test results

The search for extreme points for the correlation coefficients of UOHT and CI, SA and CI was carried out using the method of sequential phase shift (from 1 to 29 months forward and backward) of the CI of the corresponding planets. The correlation coefficients for UOHT, SA and CI of Mrc-Jup and Mar-Npt were found to differ in clearly defined waves.

Fig. 1. Components of UOHT S 1 , ..., S 7 (curves 2-8) resulted from adaptive filtration of the primary range of monthly average values (1)

OBSERVATIONS OF POLAR STRATOSPHERIC CLOUDS OVER MURMANSK IN JANUARY-FEBRUARY 2010

Second, the influence of dynamical processes that take part in the stratosphere also affects the dynamics of the troposphere. TIME DEPENDENT MODELING OF THE INITIAL PHASE OF INTRATROPICAL CYCLONE FORMATION.

Fig. 1. Nacreous clouds above Murmansk on 11 January 2010

TIME-DEPENDENT MODELING OF THE INITIAL STAGE OF THE FORMATION OF CYCLONES IN THE INTRATROPICAL

CONVERGENCE ZONE OF THE NORTHERN HEMISPHERE

Time-dependent modeling of the initial phase of cyclone formation in the Northern Hemisphere intratropical convergence zone. The width of the intratropical convergence zone can reach several hundred kilometers.

Fig. 3. The same as in Fig. 1, but obtained for the third initial configuration of the intratropical convergence zone

10 YEARS INVESTIGATIONS OF THE SOLAR UV RADIATION AND TOTAL OZONE IN STARA ZAGORA, BULGARIA

The ratio between the intensity of the flux, reflected by the Earth, and the direct solar signal is used to calculate the total ozone content. The dependence analysis of the UV radiation on the sun zenith angle (SZA) at fixed total ozone shows a.

Fig. 1. UV solar spectra, registered by Photon , at different solar zenith angle: (1) SZA=53, (2)

INFLUENCE OF HF POWERFUL WAVES ON THE OZONE CONTENT IN THE EARTH’S ATMOSPHERE

In the right panel, the spectra of the ozone emission intensities recorded under night (black line) and day (gray line) conditions are shown. The effect of the drop in ozone number density during atmospheric pumping is clearly visible.

Fig. 2 displays the spectral data from microwave measurements made on March 14

ON THE CONNECTION BETWEEN VARIATIONS OF ATMOSPHERIC ELECTRIC FIELD AS MEASURED AT GROUND SURFACE IN THE

Fig.1 Diurnal curves of the thunderstorm part of the atmospheric electric field measured in Vostok st. 2 Daily curves of thunderstorms that are part of the atmospheric electric field for Antarctic summer and winter (left panel) and Carnegie curve (right panel).

Fig. 2 Daily curves of thunderstorms part of the atmospheric electric field for Antarctic summer and winter (left panel) and Carnegie curve (right panel )

SUBSTORM EFFECTS IN THE POLAR LATITUDE ATMOSPHERIC ELECTRIC FIELD DISTURBANCES

Observations

The preliminary phase of this substorm was accompanied by the significant positive Ez anomalies at Hornsund. The late evening substorm was observed at ~ 19-20 UT on this day and it was accompanied by the negative Ez anomalies.

Discussion

It is clearly seen (Fig. 3) that every negative magnetic anomaly observed at HOR was accompanied by a simultaneous positive anomaly in atmospheric electric field (Ez) variations at that station. We speculate that the significant changes in the atmospheric electric field (Ez) at the Hornsund observatory observed during the development of magnetospheric substorms are due to the penetration of polar ionospheric convection electric fields (which are strengthened during the substorm) to the Earth's surface.

Fig. 3. The Ez variations and the magnetogram (X- (X-component) at obs. Hornsund on October 27, 2005

Conclusions

STUDY OF GAMMA-RADIATION CONNECTED TO ATMOSPHERIC PRECIPITATION

Instrumentation

Scintillation spectrometer
Additional equipment

Observations
Discussion
Conclusions

The intensity of photons is determined by the generation of energetic electrons and positrons in the form of bremsstrahlung and an alternative process of absorption in air [3]. The energy spectrum of electrons in the energy range (E < 1MeV) can be approximated by the exponential law [3].

Figure 1 shows typical profiles of the count rate increase in the X-ray channel > 20keV and precipitations (rain) for the Apatity station

INVESTIGATION OF THE IONOSPHERIC F-LAYER RESPONSE TO THE FAC2 VARIATIONS DURING APRIL 16 AND 17, 2002 USING THE

INVESTIGATION OF THE IONOSPHERIC F LAYER RESPONSE TO THE FAC2 VARIATIONS DURING 16 AND 17 APRIL 2002 USING THE. Model interpretation of the unusual nocturnal electron density behavior in the F region observed by the Millstone Hill incoherent scattering radar in April.

Figure 2. The time variations of hmF2 (above) and foF2 (below) observed by the Sondrestrom ionosonde during April 15-20, 2002 (dots) in comparison with the UAM results (solid and dotted lines)

STUDY OF HIGH-LATITUDE D-REGION IONOSPHERE

CHARACTERISTICS DURING PERIODS OF POLAR MESOSPHERIC ECHO (PME) APPEARANCES

The solid line in the figure on the left shows the profile of the electron density, measured by incoherent scattering (IS). Therefore, determination of the effective loss factor can be an effective method for dust determination in the mesosphere.

Fig. 1. Time-altitude dependence of the amplitude reflections of the ordinary (A o ) and extraordinary (A x ) waves and

CONJUGATE AND INTER-HEMISPHERIC OCCURRENCE OF GPS TEC FLUCTUATIONS IN HIGH LATITUDE IONOSPHERE

This is also confirmed by a comparison of the aurora distribution in the oval (Feldstein et al, 1974, Zverev and Starkov 1975) and TEC measurements with GPS receivers (Shagimuratov et al, 2006). Primary images of the auroral oval for the azimuth vector diagram were generated using the data described in (Feldstein et al., 1974;

Fig 1. a) Variations of Bz and TEC fluctuations occurrence over geomagnetic conjugated polar cap stations MCM4 (south) – RESO (north)

WAVE DISTURBANCES IN THE LOWER IONOSPHERE DURING THE EARTHQUAKES ON AUGUST 2006

The analysis of experimental data

On the spectrum of the common component, the amplitude of the partially reflected signal is broader than the spectrum of the amplitudes on August 7. Daily spectrum amplitudes of lowest frequency fmin in days of the August 7 and 11, 2006 earthquakes are shown in Figure 6.

Fig. 3. The variations of riometer absorption at the frequency 29.9 MHz on August 7 and 11, 2006 at stations Ivalo (IVA) and Sodankyla (SOD)

Summary

Precipitating high-energy electrons are the main source of ionization at dusk and at night, even under calm conditions. Rheometric absorption at the frequency of 29.9 MHz at the Ivalo and Sodankyla observatories increased to 2.5 dB in the first half of the day.

LONG-TERM VARIATIONS OF ENERGETIC ELECTRONS AT LOW ALTITUDES

Whenever the satellite is poleward of about 35° latitude, this detector monitors electrons in the atmospheric loss cone that will enter the Earth's atmosphere below the satellite. This is best seen in the years 2006 to 2009, when significant geomagnetic conditions caused the least disturbance in electron flows.

Fig. 1. NOAA-15 to MetOp-2 data comparison. Month averaging of > 30 keV, 0º-channel

UNIVERSITY SATELLITES DEVELOPMENT PROGRAM

Its main scientific goal - detection of transient light effects in the atmosphere and ionosphere - was raised after the "Universitetsky-Tatiana" experiment with UV detector. The study of transient events in the Earth's upper atmosphere is already a tradition of Moscow University.

Fig. 2. The model of the Tatiana-2 satellite. The fields of view of optical detectors are shown on the figure

In the lower part, the ratio of the horizontal vector variations to the vertical components is presented. This event is characterized by large value of the ratio of the horizontal vector to the vertical component.

Figure 3. Variations of the horizontal vector (top diagram) and its ratio to the vertical component for one hour of the heating on July 12.

NUMERICAL SIMULATION OF THE DYNAMICS OF FINE-SCALE IRREGULARITIES IN THE NEAR-EARTH RAREFIED PLASMA

NUMERICAL SIMULATION OF THE DYNAMICS OF FINE SCALE IRREGULARITIES IN THE PLASMA, RARE ON EARTH. Numerical simulation of the dynamics of fine-scale irregularities in the rarefied plasma near Earth.

Fig. 1. The calculated spatial distributions of the relative decrease of the electron

THE ROLE OF ION DIFFUSION IN FORMATION OF 3-D SPATIAL STRUCTURE OF THE PLASMASPHERE

Model result

Near-equatorial maximum
Sub-auroral maximum
Mid-latitudinal maximum

Therefore, during the day, a considerable number of O+ ions are produced here, which accumulate in the upper part of the tube, where there is almost no recombination. Therefore, both in the shorter and in the longer tube, nighttime recombination takes place faster, and a maximum appears between them.

Figure 2. The horizontal cut of the ionosphere after 1 (left panel) and 5 (right panel) days of modeling time

Conclusions

In order to discover the physical mechanism of its formation, we performed another simulation in which the temperature of the ions was constant in the entire space. At latitudes of 30-40°, the diffusion currents are strong enough to fill the relatively small volume of the tube during the day and return a large part of the accumulated ions back to the ionosphere at night (Fig. 5, right panel).

VALIDATION OF THE MODEL IRI - 2007 BY THE LATEST EXPERIMENTAL DATA IN AURORAL IONOSPHERE

The latest experimental data shows that the solar wind value of the magnetic field has very low values (Figure 5). Thus, the model is not accepted for such low values of the solar wind parameters and consequently for low values of maximum height and electron density in the F2 layer.

Table 1 Difference between real data and simulation results

TESTING OF THE UPPER ATMOSPHERE MODEL USING THE EMPIRICAL IONOSPHERIC MODELS

The UAM-TT version underestimates the daytime f0F2 values at the end of the third twenty-four hour integration period in all seasons. The poleward wind speed increases and this causes a decrease in the hmF2 and f0F2 in winter and summer solstices.

Figure 1. The calculated F2-layer critical frequency (f 0 F2), height of the F2-layer peak (h m F2), northward neutral wind velocity at the altitude of 300 km (V nx ) and ratio of the O and N 2 concentrations at the altitude

MAGNETOSPHERIC AND THERMOSPHERIC ORIGIN ELECTRIC FIELDS INFLUENCE ON THE ENHANCED ELECTRON DENSITY

Magnetospheric electric field influence on the EEDR’s

In the top row—calculated by UAM-MSIS taking into account field line ion transport caused by the thermospheric wind, the geomagnetic height–latitude distributions of Lg(ne) along the nighttime geomagnetic meridian 01:30 MLT for height range from 800 to 3000 km, bottom row – corresponding geomagnetic latitude–longitude distributions of the eastward electric field at 175 km altitude for 24:00 UT 16.04.2002. In the left column – the meridional section and the map corresponding to the model calculation with ∆φ=20 kV, in the right column – with ∆φ=60kВ.

Figure 1. At the top row – the calculated by the UAM-MSIS with taking into account the thermospheric wind induced field-aligned ion transport the geomagnetic altitude-latitude distributions of Lg(n e ) along the night-time geomagnetic meridian 01:30 MLT

Thermospheric (dynamo) electric field influence on the EEDR’s

The equatorial sides of the EEDR's abut the equatorial anomaly remain in the MLT sector at night. Thus, our study shows that the magnetospheric and thermospheric (dynamo) origin electric fields influence the latitudinal location and shape of the equatorial sides of the EEDR adjacent to the equatorial anomaly remains in the nighttime MLT sector.

NUMERICAL MODELING OF THE ALASKA 1964 EARTHQUAKE IONOSPHERIC PRECURSORS

Calculation results of ∆Ezon, ∆Emer, ∆foF2 and ∆TEC with penetrated vertical electric field at electric potential irregularity, which is equal to 10 kV (left panel) and 30 kV (right panel). Numerical simulation of the electric field and zonal current in the Earth's ionosphere: the dynamo field and the equatorial electrojet.

Fig. 1 presents the diurnal variation in critical frequency of F2-layer, foF2, above station Anchorage obtained in calculation results with electric potential irregularity, which equals 10 and 30 kV, and without seismogenic sources and obs

DISTURBANCES OF HELIOGEOPHYSICAL PARAMETERS

DISPLAYING IN THE MAXIMUM OBSERVED FREQUENCIES ON IONOSPHERIC OBLIQUE SOUNDING TRACES

Used data

Search of linear correlations and their estimation

Nonlinear connections and MOF restoration on examined traces

A solid line - real MOF values of Irkutsk - Rostov-on-Don track, a dotted line - the values recovered by neural network. Similar neural network recovery of MOF data was performed for railway Cyprus - Rostov-on-Don.

Table 1. Interplanetary space parameters and characteristic time delays of DMOF reaction on changes in given parameters

MAGNETOTAIL STRETCHING UNDER DIFFERENT SOLAR WIND CONDITIONS

The latitude of the isotropy boundary corresponding to the magnetic clouds (or their parts) with north. Latitude of the proton isotropy limit as a function of MLT for different solar wind conditions.

Table 2. Mean solar wind parameters for 2001 and some selected solar wind stream intervals Number of

EARLY FORECAST OF RADIATION HAZARDOUS SOLAR COSMIC RAY FLUXES ON THE NEUTRON MONITORS DATA

Analysis of separate events Event of 21 May 1990

Event of 14 July 2000
Event of 15 April 2001

Points is a spectrum of time of maximum (TOM) spectrum, according to direct measurement of solar protons on the GOES-10 spacecraft. Dots are the TOM spectrum of the maximum fluxes according to direct measurements of solar protons on the GOES-8 spacecraft.

Fig. 1. a - profiles of ground level enhancements at NM stations Apatity (Ap) and Magadan (Ma)

SOLAR WIND RECURRENT PHENOMENA IN 23-th MINIMUM

Data and calculations

To interpret the image of the last minimum, we select data representing the near-Earth cosmic space: parameters of the plasma and interplanetary magnetic field in the SW (Wind data; SOHO, University of Maryland), data on the sector structure (SS) of the IMF (ACE). ). Solar parameters are presented as follows: LASCO SOHO coronal images; MDI magnetograms and the solar disk in the EIT SOHO soft X-ray; disk sunspots in the continuum (SOHO); and also photospheric magnetic field synoptic maps and WSO source surface field maps; and also CH cards in the Fe XIV NSO Sacramento Peak line to add dynamic CH transformation to CR 2052-2091 in the 23rd minimum in 2007-2010.

IMF polarity and SW flows

The Higuchi method allows us to estimate fractal dimension (FD) of SW plasma, as the characteristic of SW plasma flow structure.

Fractal dimension variations in front of fast SW streams in HPL transitions

The dividing line in the WSO source surface field synoptic chart proves a true situation. Solar activity and the connection of geomagnetic disturbances // In "Physics of solar corpuscular currents and their action in the upper atmosphere of the Earth", Publishing House of the Academy of Sciences of the USSR.

THE FORECAST OF GEOMAGNETIC ACTIVITY UNDER THE ESTABLISHED CHARACTERISTICS OF SOLAR WIND MAGNETIC

Base of force-free cylindrical model magnetic clouds

Analysis of influence of magnetic cloud parameters on its geoeffectiveness

Technique of short-term forecast of geomagnetic storms intensity caused by magnetic clouds The technique of short-term forecast of geomagnetic storm intensity caused by magnetic clouds includes two basic

Manifestation of configurations of magnetic clouds of the solar wind in geomagnetic activity // Kosmicheskie Issledovaniya (RAS). Effects of magnetic clouds on the occurrence of geomagnetic storms: The first 4 years of Wind // J.

Fig. 3. The same, that in Fig.1, but for magnetic cloud 28.10.2000

THE ACTIVE REGION MAGNETIC FLUX CORRELATION WITH FLARES APPEARANCE

The association of the active region magnetic field and flares has been investigated for many years. The calculations were performed in the domain 41010 см × 41010 см, when the active region of the eastern limb is displaced in ~30О. The figure shows that the line-of-sight magnetic field distribution is quite different from distribution of the normal magnetic component. б) Calculated magnetic field distribution of the normal magnetic field component.

Fig. 2. a) Line of sight SOHO MDI (http://soi.stanford.edu/magnetic/index5.html, in the active region AR10486 (24.10.2003 19:15)

MODELLING OF HADRON INTERACTIONS IN THE NEUTRON MONITOR

To calculate the response function of the neutron monitor, first of all, information is needed about the neutrons that have reached the detector and interacted with the 10B nuclei. A modeling and calculation of a response function of the standard neutron monitor NM-64 to different types of secondary cosmic rays was performed with a GEANT4 software package.

Fig. 2. Visualization of neutron monitor model with a graphic system FreeWRL. In the figure the neutron monitor 6- 6-NM-64 is placed in a particles beam with random incident positions (particles fall on the monitor from above)

EFFECTS OF THE LONG –TERM VARIATIONS OF THE SOLAR WIND ON THE NEAR-EARTH SPACE

Experimental data

EFFECTS OF LONG-TERM SOLAR WIND VARIATIONS ON THE NEAR UNIVERSE.

Results of experimental data analysis

One can find in the long-term variations of the solar wind density some evidence for the existence of cyclic wind. Quite good agreement was found between the long-term variations of solar wind density and sea ice cover in the Arctic.

Figure 1. Long – term (1965 -2007) variations of annually averaged values of the Sun spot number (W), full vector of the IMF (Bsw), critical frequency (h max F2), values of altitude of maximum of F2 layer (h max F2) on station Sodankyla together with t

FULL-WAVE SOLUTION FOR A MONOCHROMATIC VLF WAVE PROPAGATING THROUGH THE IONOSPHERE

A deviation of the reflection coefficient from unity at h = 600 km is thus only due to energy absorption in the ionosphere. A numerical study of excitation, internal reflection and limiting polarization of whistler waves in the lower ionosphere.

Fig. 1 Electron density and collision frequency profiles.

CONTRIBUTION OF THE MHD WAVE MODES TO THE GLOBAL Pc5 PULSATIONS

The global pulsations of PC5 on 31 October 2003 are Alfvén waves on both the morning and afternoon sides. Generation of Pc5 pulsations of the geomagnetic field and rheometer absorption // Space Research (Kosmicheskie issledovanija).

Fig. 1. Proton density at ACE, GEOTAL, WIND spacecrafts and magnetic field at ABK station for the morning (left panel) and afternoon (right panel) Pc5 pulsations

CALCULATION OF THE MAGNETOPAUSE STAND-OFF DISTANCE

The authors found changes in the shape of the magnetopause with varying dipole tilt angle. Analytical models for estimating the distance to the magnetopause R0 [Kuznetsov and Suvorova, 1998; Shue et al.

Table 1 shows magnetopause stand-off distance R 0 predicted according to following models: Shue et al

MODELS OF THE GEOMAGNETIC FIELD AND MAGNETOMETER MEASUREMENTS OF CLUSTER FGM IN THE MAGNETOSPHERIC

Furthermore, the results of the statistical analysis of the impact of Bz events on geomagnetic activity are presented. The annual variation of SME events is similar to the same variation of solar activity.

Figure 1: Variation of the FGM measurements along the Cluster C3 orbit, compared with the corresponding 1-min model values of T01, T96 and PM for the time interval August 10, 23 UT, till August 11, 2007, 20 UT (left) and August 19, 0

IMF B

Weak magnetic storms could develop without the occurrence of Bz-events in the solar wind. However, it is impossible to estimate the intensity of a magnetic storm by evaluating the intensity and duration of Bz-events.

MORNING – EVENING ASYMMETRY OF AURORAL PRECIPITATION DURING MAGNETIC STORMS

In the main phase of the storm (maximum magnetic activity) the region of mild auroral precipitation (SDP) located poleward of the AOP disappeared. As can be seen, the width of DAZ precipitation in the evening sector (18-21 MLT) does not change significantly, while in the morning sector (06-09 MLT) DAZ.

Figure 1. The variations of AL- and Dst indices, dynamics of the precipitation boundaries in the N- and S- hemispheres in the morning (a) and evening (b) MLT sectors

STRENGTHENING EFFECT OF THE MAGNETIC FIELD DUE TO THE PRECIPITATION OF CHARGED PARTICLES

The distribution of the plasma pressure field in the magnetosphere before (1) and after before (1) and after dipolarization (2). The distributions of the kinetic energy of charged particles in magnetic flux tubes vs colatitude θ before (1) and after dipolarization (2).

Fig. 1. The distribution of B z component of the magnetic Fig.2. The distribution of the plasma pressure field in the magnetosphere before (1) and after before (1) and after dipolarization (2)

THE STELLACAM II AS AN ALL-SKY IMAGER DURING THE SCIFER 2 ROCKET CAMPAIGN

Short background
Parts and components
Experimental setup
Rocket animation
Concluding remarks

The green circle is the missile's position determined on the geomagnetic field line at an altitude of 200 km. A video overlay projects information on the date, time, position, viewing angles and altitude of the missile.

Figure 1. Left: The StellaCam II from WATEC Inc. with its manual controller. Right: The CS-mount fisheye lens from Fujinon with a focal length of 1.4mm to 3.1mm at an aperture of F/1.4

IONOSPHERIC DISTURBANCES GENERATED IN THE AURORAL ZONE DURING MAGNETIC STORMS

Simulation of the motion of points in the geomagnetic and geographic coordinate

According to calculations, the speed of the point in the geographical system consists of two components: along the geographical meridian (meridional component, Vr) and along the geographical parallel (zonal component, Vφ). The meridional velocity component Vr in the geomagnetic longitudes near 0° and 180° varies slightly with latitude and is close to the meridional velocity in the geomagnetic coordinate system.

Conclusion

An analysis of the table in [Leonovich et al., 2004] shows that westward dayside anomalies were observed in the American region; eastward anomalies on the night side, in the European and Asian regions. However, during the October 29, 2003 storm, a westerly deviation was recorded in the European and Asian sectors [Perevalova et al., 2008].

DAYSIDE STORM-TIME ULF PULSATION IN THE SOLAR ACTIVITY MINIMUM

Data and results

The variations in the speed (V) and density (N) of the solar wind, the Bz component of the IMF, Dst and AE indices, and also the ULF index of the aurora and polar zones in the morning and afternoon sectors of the magnetic storm on May the CIR storm). The most intensive ULF were observed in the pre-noon sector of the polar latitudes.

Fig. 1. The variations in the velocity (V) and the density (N) of solar wind, Bz component of IMF, Dst- and AE- indices, and also ULF- of index for the auroral and polar zones in the forenoon and post-noon sectors the magnetic storm o

BEHAVIOR OF IONOSPHERIC PARAMETERS AT MID-LATITUDE STATIONS DURING SEQUENCE OF GEOMAGNETIC STORMS ON

The new approach has allowed to significantly improve the agreement of the calculation results with the experimental data. Numerical simulation effects of magnetospheric convection, particle precipitation, and field currents of the second region during the 9–14 September 2005 geomagnetic storm sequence.

Fig. 2. Calculated particle precipitation energy and energy fluxes for different Kp-indices

BEHAVIOR OF THE 5577Å AND 6300Å EMISSIONS DURING SUBSTORMS CONNECTED WITH RECURRENT SOLAR WIND

In the upper panels, the 5577 Å images showing the development of the auroral bulge are shown. Dmitrieva (1979), Substorm in the polar cap - the effect of high speed solar wind streams.

Fig. 1. The first substorm on 3 November 2005 at Andenes. The upper panel shows the substorm development by chosen images of the red (up) and green (down) lines intensity taken from ASI

NONLINEAR CONNECTION OF RING CURRENT AND AURORAL ELECTROJETS ACTIVITY WITH SOLAR WIND AND

INTERPLANETARY MAGNETIC FIELD PARAMETERS

The search of linear correlations

The speed of the solar wind and its density have a greater influence on an annular current (SYM, ASY) compared to auroral electric currents. For storms of strong intensity the influence of the solar wind speed is greater than for storms of moderate intensity and weak storms.

The search of nonlinear connections and neural network reconstruction

Solar wind speed, IMF component Bz and, to a lesser extent, solar wind density have the greatest influence on the development of auroral electrojets in the main phase of a geomagnetic storm. In the current work, the influence of the parameters of the solar wind and the interplanetary magnetic field on the circular flow and the development of auroral electrojets in the main phases of magnetic storms is investigated.

Fig. 1. (continue) Examples of neural network reconstruction of auroral electrojets and a ring current intensity indices on the PSW and IMF data

SOFTWARE-COMPUTER COMPLEX FOR SPACE WEATHER PREDICTING

Review of existing computer complexes for space weather forecast
Application interface
Used data
Statement of experiments through the web- interface
Conclusion

By clicking on “Results of the calculations”, you will be taken to the page with the results of previous experiments. Artificial neural network technique for predicting the critical frequency of the ionospheric F2 layer // Radiophysics and Quantum Electronics, 2005, V.48.

Kp INDEX CORRECTION IN ORDER TO ELIMINATE EXCESS IMPACT OF HIGH LATITUDE MAGNETOSPHERIC DISTURBANCES

Check of existence Kp index error

Low correlation factors between low and high latitude magnetograms from Kp index calculation stations are confirmed. In this regard, the offered correction of the Kp index of the planetary magnetic activity, the cleaning of the magnetograms of the polar contribution from the observatories of the Kp calculation is reduced.

Algorithm of «clearing» magnetograms from the polar contribution is working out

3 «clearing» magnetogram example of observatories Calculation of Kp index from the polar contribution registered at high-latitude station Yellowknife from calculation of AE index in disturbed day on January 7, 2004 is shown. Magnetograms of Meanook observatory of calculation of Kp index of the polar contribution are cleared.

Calculation of a new index on the basis of «cleared» magnetograms

The magnetic records of Kp observatories are identified, which require cleaning by correlation analysis of magnetic records for each pair of observatories for an excess correlation factor (|R |>0.5). Then, by repeating the official Kp-index calculation algorithm on the corrected magnetograms, we calculate a certain Kp index that does not contain excess effects of polar electrojets.