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Alexeev Igor I. Belenkaya Elena S. Bobrovnikov Sergey Yu. Kalegaev Vladimir V. 《Space Science Reviews》2003,107(1-2):7-26
A magnetohydrodynamic model of the solar wind flow is constructed using a kinematic approach. It is shown that a phenomenological
conductivity of the solar wind plasma plays a key role in the forming of the interplanetary magnetic field (IMF) component
normal to the ecliptic plane. This component is mostly important for the magnetospheric dynamics which is controlled by the
solar wind electric field. A simple analytical solution for the problem of the solar wind flow past the magnetosphere is presented.
In this approach the magnetopause and the Earth's bow shock are approximated by the paraboloids of revolution. Superposition
of the effects of the bulk solar wind plasma motion and the magnetic field diffusion results in an incomplete screening of
the IMF by the magnetopause. It is shown that the normal to the magnetopause component of the solar wind magnetic field and
the tangential component of the electric field penetrated into the magnetosphere are determined by the quarter square of the
magnetic Reynolds number. In final, a dynamic model of the magnetospheric magnetic field is constructed. This model can describe
the magnetosphere in the course of the severe magnetic storm. The conditions under which the magnetospheric magnetic flux
structure is unstable and can drive the magnetospheric substorm are discussed. The model calculations are compared with the
observational data for September 24–26, 1998 magnetic storm (Dst
min=−205 nT) and substorm occurred at 02:30 UT on January 10, 1997.
This revised version was published online in August 2006 with corrections to the Cover Date. 相似文献
2.
V.V. Kalegaev I.I. Alexeev I.S. Nazarkov V. Angelopoulos A. Runov 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2014
The magnetic field structure and the spatial characteristics of the large-scale currents in the magnetospheric tail were studied during quiet and moderately disturbed geomagnetic conditions in 2009. The magnetic field of the currents other than the tail current was calculated in terms of a paraboloid model of the Earth’s magnetosphere, A2000, and was subtracted from measurements. It was found on the base of obtained tail current magnetic field radial distribution that the inner edge of the tail current sheet is located in the night side magnetosphere, at distances of about 10 RE and of about 7 RE during quiet and disturbed periods respectively. During the disturbance of February 14, 2009 (Dstmin ∼ −35 nT), the Bx and the Bz component of the tail current magnetic field near its inner edge were about 60 nT, and −60 nT that means that strong cross-tail current have been developed. The tail current parameters at different time moments during February 14, 2009 have been estimated. Solar wind conditions during this event were consistent with those during moderate magnetic storms with minimum Dst of about −100 nT. However, the magnetospheric current systems (magnetopause and cross-tail currents) were located at larger geocentric distances than typical during the 2009 extremely quiet epoch and did not provide the expected Dst magnitude. Very small disturbance on the Earth’s surface was detected consistent with an “inflated” magnetosphere. 相似文献
3.
S. Mühlbachler D. Langmayr A.T.Y. Lui N.V. Erkaev I.V. Alexeev P.W. Daly H.K. Biernat 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2009
This study presents several observations of the Cluster spacecraft on September 24, 2003 around 15:10 UT, which show necessary prerequisites and consequences for the formation of the so-called modified-two-stream instability (MTSI). Theoretical studies suggest that the plasma is MTSI unstable if (1) a relative drift of electrons and ions is present, which exceeds the Alfvèn speed, and (2) this relative drift or current is in the cross-field direction. As consequences of the formation of a MTSI one expects to observe (1) a field-aligned electron beam, (2) heating of the plasma, and (3) an enhancement in the B-wave spectrum at frequencies in the range of the lower-hybrid-frequency (LHF). In this study we use prime parameter data of the CIS and PEACE instruments onboard the Cluster spacecraft to verify the drift velocities of ions and electrons, FGM data to calculate the expected LHF and Alfvèn velocity, and the direction of the current. The B-wave spectrum is recorded by the STAFF instrument of Cluster. Finally, a field aligned beam of electrons is observed by 3D measurements of the IES instrument of the RAPID unit. Observations are verified using a theoretical model showing the build-up of a MTSI under the given circumstances. 相似文献
4.
Cosmic Research - A distinctive feature of the Jovian magnetosphere is a powerful disklike current system—the current disk. There are several models of the magnetic field of this current... 相似文献
5.
José Luis Ballester Igor Alexeev Manuel Collados Turlough Downes Robert F. Pfaff Holly Gilbert Maxim Khodachenko Elena Khomenko Ildar F. Shaikhislamov Roberto Soler Enrique Vázquez-Semadeni Teimuraz Zaqarashvili 《Space Science Reviews》2018,214(2):58
Partially ionized plasmas are found across the Universe in many different astrophysical environments. They constitute an essential ingredient of the solar atmosphere, molecular clouds, planetary ionospheres and protoplanetary disks, among other environments, and display a richness of physical effects which are not present in fully ionized plasmas. This review provides an overview of the physics of partially ionized plasmas, including recent advances in different astrophysical areas in which partial ionization plays a fundamental role. We outline outstanding observational and theoretical questions and discuss possible directions for future progress. 相似文献
6.
Using the magnetic storm in January 1997 as an example, we examined the possibilities to employ the magnetospheric field T96 [1, 2] and the dynamic paraboloid model PM of the magnetosphere [3] for modeling the D
st variation. We have revealed the necessity to refine the results of normalizing the free parameters of the model T96 according to the solar wind parameters. The contributions to the D
st variation of magnetic fields of basic large-scale magnetospheric current systems (the field DCF on the magnetopause, the field DR of the ring current, and the field DT in the magnetotail) are estimated for different phases of the storm from model calculations. Possible causes of a discrepancy between the results of modeling D
st using the T96 and PM models are discussed. Special emphasis is made on the ratios of contributions into the D
st variation of the fields of the magnetotail and the ring current in the main phase of magnetic storms and on the contributions to D
st of the fields of various current systems at the recovery phase. 相似文献
7.
T. K. Breus R. M. Baevskii I. I. Funtova G. A. Nikulina E. V. Alexeev A. G. Chernikova 《Cosmic Research》2008,46(4):367-372
Investigations of the effect of geomagnetic activity factors on the cardiac rhythm regulation and arterial pressure of cosmonauts during the expeditions onboard the Soyuz spacecraft, and the MIR and ISS orbital space stations was carried out for various durations of flight in weightlessness and, under control. Groups of cosmonauts were inspected under flight conditions outside the geomagnetic disturbances and in ground preflight conditions, during disturbances without them. The presence of specific effect of geomagnetic disturbances on the system of vegetative regulation of blood circulation of cosmonauts during the flight was demonstrated for the first time. The response of cosmonauts’ cardiac rhythm on the magnetic storm is definitely revealed; however, it depends on the initial functional background and, in particular, on the state of mechanisms of vegetative regulation (the duration of flight and adaptation to it). 相似文献
8.
I. I. Alexeev 《Space Science Reviews》2006,122(1-4):55-68
A dependence of the polar cap magnetic flux on the interplanetary magnetic field and on the solar wind dynamic pressure is
studied. The model calculations of the polar cap and auroral oval magnetic fluxes at the ionospheric level are presented.
The obtained functions are based on the paraboloid magnetospheric model calculations. The scaling law for the polar cap diameter
changing for different subsolar distances is demonstrated. Quiet conditions are used to compare theoretical results with the
UV images of the Earth’s polar region obtained onboard the Polar and IMAGE spacecrafts. The model calculations enable finding
not only the average polar cap magnetic flux but also the extreme values of the polar cap and auroral oval magnetic fluxes.
These values can be attained in the course of the severe magnetic storm. Spectacular aurora often can be seen at midlatitude
during severe magnetic storm. In particularly, the Bastille Day storm of July 15–16, 2000, was a severe magnetic storm when
auroral displays were reported at midlatitudes. Enhancement of global magnetospheric current systems (ring current and tail
current) and corresponding reconstruction of the magnetospheric structure is a reason for the equatorward displacement of
the auroral zone. But at the start of the studied event the contracted polar cap and auroral oval were observed. In this case,
the sudden solar wind pressure pulse was associated with a simultaneous northward IMF turning. Such IMF and solar wind pressure
behavior is a cause of the observed aurora dynamics. 相似文献
9.
Three ways of the energy transfer in the Earth's magnetosphere are studied. The solar wind MHD generator is an unique energy
source for all magnetospheric processes. Field-aligned currents directly transport the energy and momentum of the solar wind
plasma to the Earth's ionosphere. The magnetospheric lobe and plasma sheet convection generated by the solar wind is another
magnetospheric energy source. Plasma sheet particles and cold ionospheric polar wind ions are accelerated by convection electric
field. After energetic particle precipitation into the upper atmosphere the solar wind energy is transferred into the ionosphere
and atmosphere. This way of the energy transfer can include the tail lobe magnetic field energy storage connected with the
increase of the tail current during the southward IMF. After that the magnetospheric substorm occurs. The model calculations
of the magnetospheric energy give possibility to determine the ground state of the magnetosphere, and to calculate relative
contributions of the tail current, ring current and field-aligned currents to the magnetospheric energy. The magnetospheric
substorms and storms manifest that the permanent solar wind energy transfer ways are not enough for the covering of the solar
wind energy input into the magnetosphere. Nonlinear explosive processes are necessary for the energy transmission into the
ionosphere and atmosphere. For understanding a relation between substorm and storm it is necessary to take into account that
they are the concurrent energy transferring ways.
This revised version was published online in August 2006 with corrections to the Cover Date. 相似文献
10.
S.Yu. Bobrovnikov I.I. Alexeev E.S. Belenkaya V.V. Kalegaev C.-R. Clauer Ya.I. Feldstein 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2005,36(12):2428-2433
We compute global magnetospheric parameters based upon solar wind data obtained from the WIND spacecraft upstream. Using the paraboloid magnetospheric model, calculations of the dynamic global magnetospheric current systems have been made. The solar wind dynamic pressure, the interplanetary magnetic field, the strength of the tail current, and the ring current control the polar cap and auroral oval size and location during the magnetic storm. The model calculations demonstrate that the polar cap and the auroral oval areas are mainly controlled by the tail current. The substorm onset at 0630 UT on September 25, 1998 happened near the minimum in the main phase field depression. The substorm expansion onset time is also marked by a sudden enhancement in the solar wind dynamic pressure and an enhancement in the tail current. The magnetic signatures of these two effects cancel each other, which explains why the Dst profile shows no strong time variation during the substorm. Evidence for the substorm expansion includes not only the signature in the AL index but also the strong asymmetry of the low latitude magnetic disturbances (substorm positive bay signature). Model calculations were checked by comparison with the GOES 8 and 10 magnetic field measurements. 相似文献
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