M.G.Gelberg (Institute of Cosmophysical Research & Aeronomy, Yakutsk, Russia)

95 substorms were selected by data catalogs of the geomagnetic indeces and NASACD catalog of the interplanetary media parameters. The substorms, which occurced at the nearly constant negative value of the IMF Bz component, AE index had small variation during 15-30 minutes before the expansion phase onset and attained maximum (or the first maximum ) AE=AEm during 10-15 minutes after onset were selected.

It was shown that:

1. The substorms take place more often at By > 0 than By < 0 (62 and 33 cases respectively).

3. The correlation coefficients between AEp and AEm were 0,76, 0,63, 0,51 for first, second and third groups. The ratios of the mean values AEm/AEp were 2,54, 3,56, 3,91.

4. The correlation ratio for AEp at different magnetc activity and condition |Bz|/|By| was 0,83.

This work was support Russian Fundamental Research Found, grant N 95-05-14329.

S.Z.Kershengolts, M.G.Gelberg

Four types of the high - intensity long duration (more than 10 hours) coutinuous auroral activity (HILDCAA) were distinguished according to the temporal variations of AU, AL, AE - indeces. These four types of HILDCAA or their combinations practically exhaust all variety of arising disturbed situations.

To distinguish each type of HILDCAA we used an existence or absence of the short intensifications in the variations of AE - index, a predominance of the high - frequency or low - frequency components, a modulation depth. The discriminant function for the objective classification of the high - intensity long - duration continuous auroral activity was suggested.

An analysis of the solar wind parameter variations in the periods of the different types of the auroral disturbances shown:

1. Different average values of IMF Bz - component and different coefficients of Bz variation correspond to the different types of HILDCAA.

2. It is established that I type of the disturbance is observed at the average solar wind speeds of I type > 480 km/s, II type - 420 km/s, III type - 390 km/s, IV type - 300 km/s, and these differences are statistically significant.

3. For each type of the HILDCAA the definite interval of variations of the IMF magnetic induction module is corresponded.

This work was support Russian Fundamental Research Found, grant N 95-05-14329.

I.V.Kovalevsky (IZMIRAN,142092 Troitsk, Moscow Region, Russia)

It is proposed a new-theoretical (system dialectical) approach (SDA) for investigation of GMS and GSS as integrity of developing physical processes complex of qualitative conversion of kinetic fluxes and magnetic and electric fields. In the methodical aspects(on the base of PR) the essence of a new approach is dislosed in sequence of genetially interconnected phases of development of these phenomena characterized by different states of physical object inner structures -the solar wind(SW), the geomagnetosphere, ionosphere. Inside this system the conversion take place. This approach is principally different from traditional ones ("geoeffective parameters", for example) and on a new plane set the problem of interpretation and prediction of GMS and GSS.

Spacial possibilities of DSA are demonstrated in connection with the usage of the most detailed data on the complex GMS (March 22,1979,GMS No27). It is analyzed what method of GMS division into system units turns out the most effective. The most satisfactory is the choise of the AE- index splashes as system unites for GMS description. It has been shown that the GMS traditional forecasting(the geomagnetic parameters on the base of the SW parameters) is not correct.The suggested SDA is more effective. It allows: a) to reveal the multi-channel development of the processes, realizing different mechanisms, b) to base on the GMS forecasting on some parameters complex derived from calculated parameters and chooced on the SDA base the delay-time values of the AE-, AL- and Dst- indexes relative to the SW parameters. The suggested SDA of data analysing may be easily automated.

This work has been supported by Russian Foundation for Fundamental Research grant 96-05-64851.

I.V.Kovalevsky and E.I.Kovalevskaya (IZMIRAN,142092 Troitsk, Moscow Region, Russia)

The present work is devoted to investigation of the main phases (MP) of 31 GMS (geomagnetospheric storms) using pattern recognition methods: under analysis is the fact what of greater importance if for "external" classification of GMS-scales of changes of the leading basic characteristics(Dst- and AE-index,By- and Bz-component of IMF -B) or their character not depending on scale.The problem may be formulated in another manner: whether only correlational characteristics of separate GMS similarity in basic processes (classification according to processes type) are sufficient or of necessity is the similarity measure where, along with the correlational characteristics, the difference in scales of basic processes (average level and variational range) is taken into account as well. Hereinafter,it will be shown that both the classifications proves to be effective for GMS MP, but in different aspects-according to inner "similarity" or processes inner "correlativity".The analysis of the separated in various classifications GMS groups according to the peculiarities of their inner structures permitted not only specifying different variants of GMS MP procedure, but also underlying significant local interconnections originating during quick change of the parameters obtained at analysis of the second time derivatives of all 32 parameters involved to investigation.

This work has been supported by Russian Foundation for Fundamental Research grant 96-05-64851.

L.P.Shadrina, S.Z.Kershengolz

L.I.Vagina, V.A.Sergeev (Institute of Physics, University of St.Petersburg, St. Petersburg, Russia; e-mail vagina@snoopy.niif.spb.su)

Using the method of Substorm Current Wedge (SCW) localization on the basis of ground magnetic measurements as well as data of NOAA, TIROS, IMP8, GOES2 and GOES 3 spacecraft the location of particle energization region in the nightiside magnetosphere before the substorm onset as well as just at the onset and during the first minutes after the onset was determined. It was found that the region of particle energization due to magnetic dipolarization is separated from the region of Field-aligned Currents closure in the ionosphere (Westward Electrojet) and magnetosphere (the reconnection region). Isotropic acceleration takes place inside the current layer in its earthward part while the Westward electrojet is located either at the tailward side of the acceleration region or tailward of it. The ionospheric projections of these regions are separated by 0-2 degrees. These results can be used for the estimation of the reconnection region size in the magnetospheric tail.

This work was financially supported by the RFBR Grant N 96-05-64019 as well as by SOLMAG Program grant.

L.I.Vagina (Institute of Physics, University of St.Petersburg, St. Petersburg, Russia; e-mail vagina@snoopy.niif.spb.su)

The problem of taking into account the ground inductive effects in the algorithm of midlatitude magnetic data inversion is considered. It is shown that for substorms with different times of current growth T the induction coefficient k is different. For small T values (T < 15 min) the k value is near to 2, while for large T (T > 40 min) values k is about 1.5.

This work was financially supported by the RFBR Grant N 96-05-64019 as well as by SOLMAG Program grant.

D.G.Baishev1, E.S.Barkova1, J.Kangas2, S.I.Solovyev1, A.G.Yahnin3, K.Yumoto4

1 Institute of Cosmophysical Research and Aeronomy, Yakutsk, Russia

2 University of Oulu, FIN-90570 Oulu, Finland

3 Polar Geophysical Institute, 184200 Apatity, Russia

4 Kyushu University 33, Hakozaki, Fukuoka, 812-81 Japan

The obtained results are interpreted as ground response of an penetration effect of the magnetospheric convection electric field to the evening sector during the substorm expansion phase and continuous and discrete character of equatorward expansion of regions of particle precipitation and currents.

K.I.Nikolskaya and T.E.Valchuk

Nikolskaya K.I., Valchuk T.E. Cosm. research (Russ.), 1996, V.34, N 6, P.415.

Phillips J.L., Bame S.J. et al., Geophys.Res.Lett., 1995, V.22, N3, p.3301.

V.G.Vorobjev, O.I.Yagodkina (Polar Geophysical Institute, Apatity, Russia)

T.E.Valchuk (Institute of Terrestrial Magnetism, Ionosphere and Radio Wave Propagation of Russian Academia of Sciences, 142092, Troitsk of Moscow Region, e-mail: solter@charley.rssi.ru)

Solar energy transformations from the solar source to the Earth are discussed. Taking into account, that the chain of energy transformation and energy transfer has very complex character, all links of this chain should be studied in details. These are: 1) energy transformations in the layers of solar atmosphere, the formation of emission within all spectral ranges and the solar wind formation; 2) the research of energy transfer in the heliosphere; 3) the interaction of solar energy flow with all Earth's atmosphere layers. Energy flow interacts with magnetosphere, ionosphere, upper atmosphere. Geophysical magnetospheric and upper atmospheric phenomena are the manifestation of the energy transfer chain in Earth's upper atmosphere. It's cyclic repetition and characteristic transformation of cyclic parameters are peculiar measure of quality and quantity action of the energy transfer on the dynamics of geomagnetospheric processes. Bright samples were analyzed: magnetospheric disturbance (auroral and geomagnetic storm activities) and atmospheric circulations. The data base including the catalogue of elementary circulation mechanisms (ECM) (Dzerdzeevsky B.L., 1975), geomagnetic indices and Wolf's numbers had used for studying features of circulation characteristics of the atmosphere in Northern hemisphere. The considered period includes solar 11-year cycles from N 11 to N 21 (1899-1985). Transition probability ECM matrices were constructed separately for odd and even cycles, their phases of growth, maximum, declining and minimum W. It is revealed, that the specific change of types of circulations occurs after maximum phase of solar cycle. It is likely that physical reason of circulation changes is connected with variations of the general magnetic field (GMF) of the Sun. This field effects on the character of reconnection processes between solar wind and magnetosphere. The influence of GMF component on the magnetospheric disturbance (M.A.Livshits et al., 1979) has to explain circulation atmosphere features in odd and even solar cycles, if different ECM types have distinct magnetosphere-ionosphere action sensitivity.

Dzerdzeevsky B.L. General atmosphere circulation and climate. "Nauka", Moscow, 1975, 285 p.

Livshits M.A., Feldstein Y.I., Valchuk T.E. Geomagnetic activity and high-latitude magnetic field of the Sun. Nature, 1979, vol.278, p.241-243.

L.Lazutin, T.Kozelova (Polar Geophysical Institute, Apatity, Russia)

R.Rasinkangas (Dept. of Physical Sciences, Univ. of Oulu, Finland)

H.Singer (Space Environment Laboratory, NOAA, Boulder, USA)

K.Torkar (Institute of Space Research of the Austrian Academy of Sciences, Graz, Austria)

S.Ullaland, J.Stadsnes (Department of Physics, University of Bergen, Norway)

In the preceding study of CRRES particle dynamics (Lazutin et al., Apatity, 1996), it was supposed, that enhanced energetic protons play important role in the division of the substorm active phase into short structures - intensifications and activations. Inspection of several new CRRES orbits allows to present additional evidences of proposed scenario. Energetic protons are dumping the current intensification or activation and preparing condition for the new local onset instability. Recently described "enhanced growth phase" effect may be considered as a particular case of described energetic proton dynamics.

R.Stadsnes, S.Ullaland, J.Stadsnes (Department of Physics, University of Bergen, Norway)

Inspection of energetic particle variation nearby the local activity onset using CRRES measurements uncovers a specific category of temporal structures when particle intensity increase or decrease significantly during first several seconds or possibly less than 1 s. Intensity changes or shifts are not simultaneous in all detectors, there are delays depending on particle pitch angle, and energy. Particle shifts may be recorded only in electrons or protons alone. When they are observed together, electron are more often delayed in respect to proton shifts. Magnetic field dipolarizations are frequently accompanying particle fast increases. Possible mechanisms of the fast intensity shifts are discussed.

R. Rasinkangas (Unirversity of Oulu, Finland)

H.Singer (Space Environment Laboratory, NOAA, Boulder USA)

Energetic particle and magnetic field data from the spacecraft CRRES on L=6.3-6.7 are analyzed to study the signatures of magnetospheric substorms at the midnigth sector of the magnetosphere, when proton and electron flux enhancements start simultaneously. Detailed investigation of the pitch-angle distributions and azimuthal anisotropy of the proton fluxes allows to determine the location of particle acceleration region and the dynamics of this region during the substorm. It was found that the enhanced proton flux region differ from one injection to other. Proton flux variations depend on energy of particles and on the spacecraft location relative to the neutral sheet current plane. We also calculate the differential vectors of the magnetic field disturbances and consider the distribution of the equivalent current vectors dJ associated with these magnetic field perturbations during the substorm expansion phase. Maximum of the Z-component of the perturbation, observed between the westward and eastward differential currents, is connected with the magnetic field dipolarization and the particle injections. The rapid dynamical changes in the location, magnitude and orientation of the perturbation current dJ may suggest that the substorm disturbed region consists of localized and transient activation sites. The observed initial signatures of the substorm onset may led to the suggestion that the magnetospheric substorm starts in the near-Earth magnetotail within 7-9 RE from the Earth.