Íàöèîíàëüíûé ãåîôèçè÷åñêèé êîìèòåò
NATIONAL
REPORT
Presented
to
the
International Association of
Geomagnetism and Aeronomy
of
the International
1999 – 2002
Ìåæäóíàðîäíîé àññîöèàöèè ãåîìàãíåòèçìà è àýðîíîìèè
Ìåæäóíàðîäíîãî ñîþçà ãåîäåçèè è ãåîôèçèêè
1999 - 2002
Presented
to the XXIII General Assembly
of the IUGG
Ïðåäñòàâëåí ê XXIII Ãåíåðàëüíîé àññàìáëåå ÌÃÃÑ
2003
NATIONAL
REPORT
To
the International
Association of Geomagnetism and Aeronomy
Of
the International
1999–
2002
of the IUGG
2003
Moscow
Îò÷åò, ïîäãîòîâëåííûé Íàöèîíàëüíîé êîìèññèåé ïî
ãåîìàãíåòèçìó è Àýðîíîìèè ê XXIII ãåíåðàëüíîé àññàìáëåå ÌÀÃÀ è ÌÃÃÑ, îòðàæàåò
íåêîòîðûå îñíîâíûå ðåçóëüòàòû èññëåäîâàíèé, âûïîëíåííûõ ðîññèécêèìè ó÷åíûìè â
1999 - 2002 ãã
ïî ñëåäóþùèì ðàçäåëàì: 1) âíóòðåííåå ìàãíèòíîå ïîëå Çåìëè; 2) àýðîíîìèÿ;
3) ìàãíèòîñôåðà; 4) ñîëíå÷íûé âåòåð è ìåæïëàíåòíîå ìàãíèòíîå ïîëî; 5) ïðèáîðû,
îáñåðâàòîðèè, ñëóæáû è àíàëèç äàííûõ.
Ýëåêòðîííàÿ âåðñèÿ îò÷åòà ñîäåðæèòñÿ íà ñàéòå
Ðîññèéñêîãî Íàöèîíàëüíîãî ãåîôèçè÷åñêîãî êîìèòåòà ïî àäðåñó:
http://www.wdcb.rssi.ru/NGC
Ðåäàêòîðû îò÷åòû
Ïðîô. Âèêòîð Í. Îðàåâñêèé
Ïðîô. Âàäèì Ï. Ãîëîâêîâ
Ïðîô. Èãîðü Ñ. Âåñåëîâñêèé
The report is prepared by the Russian National
commission on the Geomagnetism and Aeronomy to the XXIII IAGA/IUGG General
Assembly. Some main results of 1999 – 2002 are presented on the following
subjects: 1) internal Earth`s magnetic field; 2) aeronomy; 3) magnetosphere; 4)
solar wind and interplanetary magnetic field; 5) observatories, instruments,
surveys and analysis.
The electronic version of the Report
can be found at the Russian National Geophysical Committee web page:
http://www.wdcb.rssi.ru/NGC
Editors: Prof. Victor N. Oraevsky
Prof. Vadim P. Golovkov
Prof. Igor`
© Íàöèîíàëüíûé ãåîôèçè÷åñêèé êîìèòåò ÐÀÍ, 2003 ã.
© National Geophysical Committee, RAS, 2003
Foreword
This
report containing a review of the activities and scientific researches in
1999-2001 in
There
are five sections in the report according to the IAGA Divisions I-V
The
preparation of this report has been organized by the National Commission on the
Geomagnetism and Aeronomy and the National Geophysical Committee as a
collective effort of the team of authors, who compiled the greater parts of the
Sections: S.I. Avdiushin, I.V. Chashey, A.N. Didenko, A.I. Efimov, V.P.
Golovkov, A.M. Gorodnitsky, G.A. Kotova, N.G. Kleimenova, A.P. Kropotkin, S.N.
Kuznetsov, V.E. Pavlov, A.S. Potapov, E.N. Sosnovets, V. Spichak, P.M. Svidsky,
E.D. Tereschenko, I.S.Veselovsky. Some additional information has been provided
by several institutions and researchers. Only minimal editorial work has been
done when putting all these parts together, preserving, thus the diversity in
styles and approaches.
The
report cannot be considered as comprehensive review of the principal
achievements during this period of time in this field of science in
Bearing
in mind all these restrictive circumstances we hope that the readers who are
interested in this field of science can find useful sources of information in
this report.
Acknowledgements
We
are grateful to the authors, institutions and many researches who provided the information for this report. We are
especially grateful to Prof. A.N. Didenko, the Chairman of the Council on
Geomagnetism and Aeronomy of the
The
Editors
Abstract
The
Report is prepared by the Russian National Commission on the Geomagnetism and
Aeronomy to the XXIII IAGA/IUGG General Assembly. Some main results of
1999-2002 are presented on the following topics: 1) Internal Earth's magnetic
field; 2) Aeronomy; 3) Magnetosphere; 4) Solar wind and interplanetary magnetic
field; 5) Observations, instruments, surveys and analysis.
Editors:
Prof. V.N.Oraevsky, Prof. V.P.Golovkov, Prof. I.S.Veselovsky
Contents
Foreword
A.
Contributions from IZMIRAN, IKI, ISTP, PGI, SINP MSU
B.
Contributions from other scientific organizations
I.
Internal Magnetic Fields
II.
Aeronomic Phenomena
III.
Magnetospheric Phenomena
IV.
Solar Wind and Interplanetary Magnetic Field
V.
Observatories, Instruments, Surveys, and Analysis
THE MOST SIGNIFICANT RESULTS OF THE
(compiled by Prof. V.P.Golovkov)
CORONAS-F
The
Russian-Ukrainian satellite CORONAS-F with 15 scientific instruments on board,
launched on
For the present,
the CORONAS-F mission has provided about a million X-ray spectra and more than
300 thousand high-resolution X-ray images of the Sun, many time profiles of the
flare-generated emissions in a broad energy range, as well as new Solar Cosmic
Ray and UV data.
V.N.Oraevsky,
I.I.Sobelman. Comprehensive Studies of Solar Activity on the
CORONAS-F Satellite. Astronomy Letters, Vol.28, ¹ 6, 2002, pp.401-410. (Translated from Pis’ma v Astronomicheskii Zhurnal, Vol.28, ¹ 6,
2002, 457-467).
V.N.Oraevsky,
I.I.Sobelman, I.A.Zitnik, V.D.Kuznetsov. Comprehensive solar studies
by CORONAS-F satellite: new results. Physics – Uspekhi 45(8), p.886-896, 2002.
Terrestrial Magnetizm
1.
Main geomagnetic field and
its secular variations
Using magnetic
surveys, data from satellites Oersted, Champ and Magsat developed new methods
for global modeling the space-time structure of the geomagnetic field. The ST
model was developed with this new technique and use both satellite and
observatory data from 1980 till nowadays Based on this STM candidate models of
a new generation of IGRF were developed for epoch 1985, 1990, 1995, 2000 as
well as a candidate model of SV for 2000-2005 [Bondar et al., Oersted, 4th
International Science team Meeting, Proceedings, Copenhagen, Denmark, 2002, 5
p.] investigated using different approaches. All available data series from
geomagnetic observatory global network from the end of XIX century to nowadays were carefully analyzed in search of jerks epochs [Golovkov
et al., 4th International Science team Meeting, Proceedings,
Method of the
wavelet analysis was adapted for time series of data from observatories of the
global network. The data of the time interval of the XX century was analyzed
with this method. Power, dispersion and fractal characteristics were derived.
As outcome of
this study the following results were obtained:
-
A rather large downfall in the SV power spectra was
discovered about a=28-30 of the wavelet transform.
-
Sharp changes of SV of duration about ten yrs were
discovered in 1969-1970 and 1989-1990 yrs. They are of the undoubtedly inner
origin. It corresponds to the averaged electroconductivity of the mantle about
103 Cm/m [Rotanova et al., Geomagnetism I Aeronomiya, 2002, V.42,
¹5, pp. 708-720].
New interesting
results were obtained in the hydromagnetic geodynamo. The first spherically
symmetrical analytical solutions of the basic linear heat conduction and
admixture diffusion equations was derived for planets of Earth type by
Starchenko and Kotelnikova in Journal of Experimental and Theoretical Physics,
Vol.94, P.459. Starchenko and Jones in Icarus, Vol.157, P.426
considered the possible dynamical regimes in the cores of the Earth, Jupiter
and Saturn, and hence estimated typical velocities and magnetic fields to be
expected in their interiors. These estimates are in reasonable agreement with
observations of the large-scale internal fields of those planets. Frick,
Reshetnyak and Sokoloff proposed the first geomagnetic shell model of
turbulence for the Earth's core in Europhys. Lett. Vol.59, P.217. This approach has made possible the
resolution of MHD turbulence on a wide range of spatial scales: from 1000 km up
to millimeters.
2.
External variations
Using magnetic
data from observatory global network as well as data from low and high altitude
satellites some new results were obtained.
Slow dynamics and
interactions in ensamples of solar photospheric of open magnetic fields lines
have been found [Ivanov et al., 2001]. It was shown that these interactions are
responsible for sunspot generation and decay.
Ivanov K.G.,
Kharshiladze A.F., Mel’nic A.N. Slow dynamics of open field lines as an
indicator of subphotospheric interactions and its relation to solar activity
events and Near-Earth disturbances: 1. Events of July – October 1999. Geomagnetism and Aeronomia (English Translation), 2002, V.41, ¹6,
p.689.
It is established
an approximately comparable contribution of the ring current (DR) and the
magnetotail current (DT) during the storm main phase with calculating of Dst
variation as superposition of the magnetic fields due to the current on the
magnetopause (DCF), DR and DT.
Dremukhina, L.
A., Y. I. Feldstein, I. I. Alexeev, V. V. Kalegaev, M. Greenspan, Structure of
the magnetospheric magnetic field during magnetic storms, J. Geophys. Res.,
104, 28351-28360, 1999
Alexeev,
Analyzing data
from new missions Oersted and Champ the annual magnetic variation nature was
clarified. Annual series of the daily sets of the spherical harmonic
coefficients was expanded into the natural orthogonal components. One of these
components was annual periodicity. In this way spherical-harmonic model of the
annual variation was developed. It was found, that zonal terms of this model
prevail very much over other terms. It gives us very significant argument in
favor of a hypothesis by Pogrebnoy about circumpolar current systems in middle
ionosphere over geographic poles [Zvereva et al., 4th International
Science team Meeting, Proceedings, Copenhagen, Denmark, 2002, 4 p.].
3.
Magnetic anomalies
Magnetic
anomalies were studied using data from magnetic surveys near the Earth surface,
in middle stratosphere (20-40 km) and on the satellite altitudes.
These were
developed new approaches to reveling of singularities in the geomagnetic field structure
and their use for determination of the equivalent dipole depth. Using wavelet
transformation of the profile surveys of different altitudes over the
Studying magnetic
anomalies, obtained from the satellite surveys data over
IONOSPHERE
A new theoretical model of the Earth's low and middle
latitude ionosphere and plasmasphere has been developed [Pavlov, 2003]. The new
model uses a new method in ionospheric and plasmaspheric simulations. It takes
advantage of a combination of the Eulerian (an Eulerian computational grid is fixed in
space co-ordinates) and Lagrangian (it is needed to solve only one dimensional
time dependent ion and electron continuity and energy equations along a
magnetic field B in the moving Lagrangian frame of reference)
approaches. New equations which determine the trajectory of the
ionospheric plasma perpendicular to B
and an electric field E and take
into account that magnetic field lines are "frozen" in the
ionospheric plasma are derived and included in the new model. Different new strategies for solving the
continuity and energy equations and a new direction splitting technique
are developed and employed at the same time with the use of low and middle
latitude boundary conditions. The model
takes into account the role of vibrationally excited N2 and O2
and electronically excited O+ ions in the ionosphere and calculates
altitude profiles of electron and ion densities Ne and Ni
and temperatures Te and Ti above 130 km. We have
presented a comparison between the modelled NmF2 and hmF2 and NmF2 and hmF2
which were observed at the anomaly crest and close to the geomagnetic equator
simultaneously by the Huancayo,
There were very serious problems with explanations of existence
of high plasmaspheric electron temperatures Te (~7200-10700 K)
measured by the instruments on board of the EXOS-D satellite and low Te
measured by the Millstone Hill radar in the topside ionosphere within the same
magnetic field line tube. The additional heating of electrons found brings the
measured and modelled Te into agreement in the plasmasphere and into
very large disagreement in the topside ionosphere (up to 1000-2000 K) if the
classical Spitzer-Harm electron heat flux is used. The discovery of the
phenomena of the reduced and nonlocal electron temperature conductivity of the
plasmasphere and the topside ionosphere [Pavlov et al., 2000] solves this
problem. The new approach are derived leads to a heat flux which is much less
(up to a factor of 2-3) than that given by the classical Spitzer-Harm theory.
As a result, the high plasmaspheric Te and low ionospheric Te
can exist at the same time.
1. Pavlov, A.V., New method in computer simulations of electron and ion
densities and temperatures in the plasmasphere and low-latitude ionosphere,
Annales Geophysicae, Vol. 21, No. 8, 2003, in press (http://www.copernicus.org/EGU/annales/ag_pt.htm).
2. Pavlov, A.V., Abe, T., and Oyama, K.-I., Comparison of the measured
and modelled electron densities and temperatures in the ionosphere and
plasmasphere during 20-30 January 1993, Annales Geophysicae, Vol. 18, No. 10,
P. 1257-1272, 2000.
It has been shown
that the influence of superheat electrons essentially increases the pumping of
plasma oscillations, excited by a powerful HF radiation, into the
short-wavelength band.
Powerful wave
beams in a medium with saturated nonlinearity have been analytically studied.
The dynamic range of maximum nonlinear effect is found, the possibility of the
beam bistability is investigated.
Theoretical
modeling of the nonlinear interaction of EM waves with the ionospheric plasma
has been performed. Creation, stability and decay of a multisoliton wave packet
have been studied.
Long-range HF
propagation in waveguiding cavities appearing at sunrise in the equatorial
ionosphere has been described. Anomalous long pulse delays about 150 msec have
been reveald by numerical simulation, which exceeds the round-the-world
propagation time.
Theory of radio
wave propagation in oversized waveguides, based on the vectorial parabolic
equation, has been developed.
Dispersion of
ultrawide-band EM pulses propagating over nonuniform earth surface has been
studied.
Solar-terrestrial
Physics
A semi-empirical
model has been developed to provide an adequate description of density
variations of the 10-GeV cosmic rays during the past three solar cycles. The
model involves the solar magnetic field parameters calculated for the solar
wind source surface (tilt of the heliospheric current sheet, magnetic field
mean strength, and polarity of the global magnetic field). The proposed model
can be used for short-term (1 to 12 months) prediction of the cosmic ray
modulation depth.
Observations of
the total solar eclipses of
The data of the
radio occultation experiments in the solar plasma environment carried out in
1995-1997 have been analyzed to reveal a correlation between the position of
the inner boundary of the solar wind transition region and the calculated
intensity of the coronal magnetic field. Three types of the flows have been
found to exist, differing by the solar wind acceleration rates. These flows are
associated with different configurations of the coronal magnetic field, which
correspond to different morphological features in the white-light corona.
The SOHO/EIT data
have revealed a new kind of the dimmings or transient coronal holes observed on
the solar disk after the halo-type coronal mass ejections (CME). Along with the
relatively compact dimmings adjacent to the eruption center, the major events
produce strongly anisotropic, canalized dimmings, which are stretched along
several narrow, extended structures (channels) and may cover the entire visible
disk. These transient features are due to strong disturbance and reconstruction
of large-scale magnetic structures involved in the CME process, and the
channeling of the dimmings manifests the complex nature of the global solar
magnetosphere in the vicinity of the solar maximum.
THE MOST IMPORTANT RESULTS OF THE SPACE RESEARCH
INSTITUTE (IKI) OF THE
(compiled by Dr. G.A. Kotova)
DIVISION
II
Long-lasting
ground based measurements of a polarization jet (PJ) by the latitudinal chain
of ionospheric stations in Yakutia (3 < L < 5; MLT = UT + 9 h) and by 5
subauroral Russian stations were analyzed together with energetic ion
observations by AMPTE/CCE (1984-1989). It was discovered that in the near
INTERBAll
2 measurements were used for the detailed study of energy-dispersed proton
structures observed at polar edge of auroral zone. These structures are the
auroral signatures of ion beams in the magnetosphere. A new type of dispersed
structures accelerated at the front of large-scale instabilities in the
magnetotail during break-up phase of substorm was found. These new type
sporadic structures are associated with different times of flight of different
energy protons along magnetic field from the source in the plasma sheet at
10-30 Earth radii to the auroral zone (Stepanova et al., 2002).
DIVISION
III
A
new analytical model of the bow shock surface is suggested for accurate and
fast prediction of this boundary position near obstacles of different shape.
For axially symmetric obstacles the model was verified by comparison with
experiments and results of GD code application for a wide range of upstream
polytropic indexes 1.15 < ( < 2, and Mach numbers 1 < Ms < (. The
model can be also used for prediction of the bow shock position around
non-axially symmetric obstacles.(Verigin et al, 2003)
Analysis
of Magion 4 (subsatellite of Interball 1) and Wind observations of the subsolar
bow shock position as a function of Alfvenic Mach number (Ma) revealed fine
effect that this boundary tends to approach the Earth when Ma is decreasing for
magnetic field aligned flow of the solar wind, while for non field-aligned flow
the bow shock moves away from the planet in accordance with traditional
expectations. It was also found that inclined solar wind flows with high
anisotropy of phase velocity of fast magnetosonic wave result in the formation
of the bow shock with terminator cross section elongated in north - south GIPM
direction and shifted toward positive Ygipm values. (Verigin
et al., 2001).
First
exact analytical solution was accomplished for determining the asymptotic
downstream slope of planetary MHD Mach cones at any clock angle for arbitrary
Ms, Ma, and (bv. The solution obtained includes all previously
known symmetric cases. The elongation and shift of the asymptotic fast mode
shock cross-section are studied for a wide range of upstream plasma parameters
as well as its unusual 'chopped' shape under certain conditions. (Verigin et al., 2003a.)
The
unique energy and time resolution of the INTERBALL 1,2/DOK-2
instrument permitted to obtain principally new results on energetic ion
features, the processes of their acceleration and propagation.
*
Almost Monoenergetic Ion (AMI) beams (E=50-600 keV) were discovered in
different parts of the Earth's magnetosphere: in the magnetosheath, upstream of
the bow shock and in the magnetotail plasma sheet. These beams originate as a
result of solar wind ion acceleration in bursts of potential electric field by
current sheet disruptions. A connection of some AMI events with collisions of
current sheets in the solar wind with the bow shock was established.
*
In the auroral zones Fine Dispersion Structures (FDS) in ion and electron
spectra (50-800 keV) were discovered. They appear as a result of the
gradient-curvature drift of particles after their pulse injection on the closed
field lines on the night side of the magnetosphere. Analysis of these
structures provides new important information on particle acceleration processes
during substorms: accurate time and duration of the acceleration, position of
the acceleration site and particle spectra in the source. The periodic
modulation of FDS by PC-5 type magnetic field oscillations was found in several
cases ("wavy" FDS). Longitudinal amplitude of field line oscillation
in "field line resonance" phenomenon was estimated (Sarafopoulos et
al., 2001, Lutsenko et al., 2002)
Observations
of ions with SCA-1/Interball frequently show bi-directional ion velocity distribution within LLBL
. Analysis of these velocity distributions indicate that they are formed during
multiple reconnection at the dayside magnetopause. (Vaisberg et al., 2001)
Analysis
of high latitude reconnection under northward component IMF confirms that in
sub-alfvenic magnetosheath flow the reconnection site is stable. (Avanov et
al., 2001)
The
Interball spacecraft ion plasma measurements in the magnetotail revealed the
net vertical plasma drift towards equatorial plane equal to 7 km/s during
southward IMF. This is the first observation of the vertical component of the
global convection cycle in the Earth's magnetosphere (Petrukovich andYermolaev,
2002).
Interball,
Geotail and Wind spacecraft data comparison shows that the northward-Bz
(contracted oval) substorms are similar to normal substorms and are actually
associated with azimuthal but not northward IMF .
Comparison of the solar wind energy input to the magnetosphere as measured by
Wind and Interball-1 spacecraft, shows that the
spacecraft-distant monitor adequately measures solar wind input during storms
and large substorms, while the use of solar wind measurements for small
substorm predictions is unreliable due to natural variability of solar wind and
IMF (Petrukovich et al., 2000).
Multispacecraft
data from INTERBALL 1, MAGION 4, POLAR, GEOTAIL, WIND, and DMSP revealed that
magnetosheath plasma flow is thermalized through the formation of
"long-operating" vortex streets and local discontinuities and
solitons in a distributed region over polar cusps (stagnation region). Plasma
percolation through the structured boundary and secondary reconnection of
fluctuating magnetic fields in a high-latitude turbulent boundary layer can
account for the main part of solar wind plasma inflow into the magnetospheric
trap. The ion thermalization is accompanied by the generation of coherent
Alfven wave cascades with scales ranging from ion gyroradius to the radius of
curvature of the averaged magnetic field, as well as by the generation of
'diamagnetic bubbles' (of few 100-1000 km thick) with a demagnetized heated
plasma inside. This 'boiling' plasma has kinked power-low spectra with two
characteristic slopes (1.2 & 2.4), that differ from the Kolmogorov law.
Despite similar scale and spectral characteristics, topologies of the summer
and winter exterior cusps are different. (Dubinin et al.,
2002).
Just
inside the magnetopause, the 'plasma balls' (few RE thick) are regularly
encountered, which contain highly reduced field and heated magnetosheath
plasma. We suggest micro-reconnection of fluctuating fields and percolation of
the 'diamagnetic bubbles' as most effective mechanisms for filling of the
'plasma balls'. (Mainard et al., 2001).
Self-consistent
kinetic description of turbulent plasma and fields at the nonequilibrium stationary
states (
The
self-consistent theory of thin current sheets, where the tension of magnetic
field lines is balanced by the ion inertia is created and investigated. Based
on the assumptions that ions are the main current carriers and their dynamics
is quasi-adiabatic, the original system of Maxwell-Vlasov equations is reduced
to the nonlocal analogue of the Grad-Shafranov equation. It is demonstrated
that the non-adiabaticity of particle motion influences significantly the
structure and evolution of TCSs. The accumulation of quasi-trapped ions with
large magnetic moments ("aging" process) leads to the local reduction
of the current near the neutral plane and the decay of current sheet
equilibrium. This effect provides a new evolutionary mechanism, which might
explain the disruption of CS structure on a time scale comparable with the
duration of the substorm growth phase. (Zelenyi et al.,
2002).
MARS
Data
recently retrieved from the High Energy Neutron Detector (HEND), a Russian
instrument currently operating onboard NASA's Mars Odyssey mission, allowed for
the first time to estimate the abundance of subsurface water on Mars. Large
areas of permafrost have been detected. At high latitudes, mass mixing ratio of
water reaches 35% and there are also two sites in equatorial latitudes with
high water content. Data involved are related to the depth of 1-2 meters. (Mitrofanov et al., 2002).
In
cooperation with GFDL (Princeton, USA) a comprehensive numerical model of
Martian climate, capable of simulating water cycle on the planet, is developed
(Richardson et al., 2002).
Detailed
analysis of the Martian magnetotail boundary crossings by Phobos 2 orbiter
revealed that highly localized strong magnetization of planetary crust
increases the downstream magnetotail thickness by 500-1000 km (Verigin et al.,
2001a). Existence of this effect was confirmed by subsequent analysis of MGS
orbiter data and should be taken into account during Martian obstacle modeling.
VENERA
From
infrared spectroscopy on Venera 15-16, new results on structure and composition
of the Venus atmosphere have been obtained, in particular water vapor abundance,
structure of thermal tides, and sun-synchronous variations of cloud deck upper
boundary. (Ignatiev et al., 1999).
DIVISION
IV
The
coordinates of x-ray solar flares in 8-20keV energy range with 2 arcmin
precision were found with the help of WATCH/GRANAT and SIGMA/GRANAT data. For
one of the flares (2 hour long
INTERNATIONAL
CONFERENCES
Once
per year international conferences on the topics covered by INTERBALL mission
were held in different countries with significant input of IKI scientists.
Symposium "Dynamics of the magnetosphere and its coupling to the
ionosphere on multiple scales from INTERBALL, ISTP Satellites and Ground-Based
Observations" was held near
20-22
January 2003 International conference "Plasma theory, space research and
international cooperation: horizons and challenges" devoted to the 70-th
anniversary of academician Roald Sagdeev was held in Space Research Institute
of Russian Academy of Sciences in Moscow. Famous Russian and foreign scientists
participated in the conference presenting interesting reviewing reports.
4-7
February, 2003 International Symposium devoted to the memory of Professor Yuri
Galperin "Auroral Phenomena and Solar-Terrestrial Relations" was held
in Space Research Institute of Russian
PARTICIPATION
IN INTERNATIONAL MISSIONS
THE
INTERBALL
INTERBALL
is the solar-terrestrial program aimed to study various plasma processes in the
Earth magnetosphere by a system of spacecraft consisting of two
satellite-subsatellite pairs above the polar aurora and in the magnetospheric
tail respectively. The two pairs of satellites study the cause-and-effect
relationships in the solar wind/magnetosphere interactions. Tail Probe with its
subsatellite MAGION 4 was launched on
MAGION
5, the INTERBALL-Auroral Probe Subsatellite was successfully reactivated on
On
16 October, 2000 in accordance with orbit calculations the INTERBALL / Tail
Probe entered dense layer of the Earth`s atmosphere and finished its operation
in space. The INTERBALL 2 data were transmitted to the Earth till February
1999.
The
INTERBALL project involved the efforts of a large international community of
Russia together with Austria, Bulgaria, Canada, Czech Republic , ESA, Finland,
France, Germany, Hungary, Italy, Kirgizia, Poland, Romania, Slovakia, Sweden,
United Kingdom and Ukraine. Besides that a close cooperation within the project
with the ground-based geophysical observations was provided. The INTERBALL
project became an inherent part of the vast international cooperation within
the IACG (Inter-Agency Consultative Group) with the other major space missions:
GEOTAIL, WIND, POLAR,
The
INTERBALL scientific instrumentation includes 16 experiments designed for a
wide range of plasma and wave, UV, magnetic and electric field measurements in
different regions of the magnetosphere and in the solar wind. IKI scientists
using the INTERBALL data obtained the most important recent results.
HEND/2001
MARS ODYSSEY
In
FUTURE
MISSIONS
Scientific
instrumentation for Mars Express ESA mission has been developed and prepared
for space flight. IKI participates in such experiments as ASPERA (versatile
exosphere and circumplanetary plasma analyzer), OMEGA (mapping IR spectrometer
for surface studies), PFS (IR Fourier spectrometer for atmospheric studies),
and SPICAM (integrated UV and IR spectrometer targeted at Martian water cycle
studies). Mars Express spacecraft is expected to be launched in April-May 2003,
observations will begin in 2004.
Some
of instruments listed above (ASPERA, PFS, and SPICAM) will be employed in for
Venus studies in the framework of Venus Express ESA mission finally approved in
2003. The spacecraft is scheduled for launching in November 2005.
MAIN
REFERENCES
Avanov,
Boynton,
W. V., ... Igor Mitrofanov, et al., Distribution of
Hydrogen in the Near Surface of Mars: Evidence for Subsurface Ice Deposits,
Science, 297(5578), 81-85, 2002.
Breus
T.K. et. al.; Effects of magnetic anomalies discovered
at Mars on the structure of the Martian ionosphere and solar wind interaction
as follows from radio occultation experiments; J. Geoph. Res.,105(A7),
15991, 2000.
Dubinin,
Å., A.Skalsky, P.Song, S.P.Savin, J.Kozyra, T.E.Moore,
C.T.Russell, M.O.Chandler, A.Fedorov, L.Avanov, J.-A.Sauvaud, R.H.W.Friedel.
Polar-Interball coordinated observations of plasma and magnetic field
characteristics in the regions of the northern and southern distant cusps, J.
Geophys. Res., 107(A5), 10.1029/2001JA900068, 2002.
Ignatiev,
N.I., Moroz V.I., Zasova L.V., Khatuntsev I.V. Water vapor in the middle
atmosphere of Venus: an improved treatment of the Venera 15 IR spectra,
Planetary and Space Sci, 47, 1061, 1999.
Khalipov,
V. L., Yu.I. Galperin, A.E. Stepanov, L.V. Shestakova, Formation of a
polarization jet during the expansion phase of a substorm: Results of
ground-based measurements, Cosmic Res., 399(3), 226, 2001.
Krasovsky
V.L., H.Matsumoto, Y.Omura. Approximate invariant of electron
motion in the field of a whistler propagating along the geomagnetic field,
Geophys. Res. Lett., 29(12), 1691, 2002.
Lutsenko,
V.N., T.V. Gretchko, A.V. Kobelev, and K. Kudela, Dispersion structures in the
energetic ion and electron spectra in the auroral regions: their nature,
properties and implication, Adv. Space. Res., 30(7), 1787,
2002.
Milovanov,
A.V., L.M.Zelenyi, G.Zimbardo, P.Veltri. Self-organized
branching of magnetotail current systems near the percolation threshold.
J. Geophys.Res., 106(A-4), 6291-6307, 2001.
Milovanov,
A. V. and L. M. Zelenyi, Nonequilibrium stationary states in the Earth's
magnetotail: Stochastic acceleration processes and nonthermal distribution
functions, Phys. Rev. E, 64, 052101, 2001.
Mitrofanov,
I., et al., Maps of Subsurface Hydrogen from the High Energy Neutron Detector,
Mars Odyssey, Science, 297, No. 5578, 78-81, 2002.
Petrukovich,
A.A. and Yu. I.Yermolaev, Vertical Ion flows in the
plasma sheet: INTERBALL-Tail observations, Ann. Geophys., 20, 321-327, 2002.
Petrukovich,
A.A., W. Baumjohann, R.Nakamura, T.Mukai, O.A.Troshichev, Small substorms:
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Pokhotelov
O. A., O. G. Onischenko, M. A. Balikhin, R. A. Treumann, and V. P. Pavlenko,
Drift mirror instability in space plasmas,2, Nonzero
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Richardson,
M. I., R. J. Wilson, A.V. Rodin Water ice clouds in the
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Sarafopoulos
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Terekhov,
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Terekhov,
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MOST IMPORTANT RESULTS OBTAINED DURING 1922-2002
IN THE INSTITUTE OF SOLAR-TERRESTRIAL PHYSICS (ISTP) OF THE SIBERIAN BRANCH OF
THE
(compiled by Dr. A.S.Potapov)
Research
results
In the years of the 23-rd solar cycle
maximum, the closest attention was devoted to a comprehensive study of strong
geomagnetic disturbances, and to their manifestation at high and mid-latitudes.
Thus, the incoherent scatter radar [1]
provided unique experimental data on magnetosphere-ionosphere coupling effects
caused by the geomagnetic superstorm of
An analysis was made of the emission
variations in the mid-latitude airglow during a major magnetic storm of
Data from the international network of
receivers of the navigation GPS system were used to construct a global picture
of the mid-latitude ionospheric electron density response to sudden magnetic
storm commencements, and it was established that this response includes the
phases of instantaneous and delayed response. The instantaneous response
manifests itself with a delay of 3-5 min with respect to the sudden
commencement and is characterized by a short-lasting (about half an hour)
decrease in electron density throughout the entire dayside. In the delayed response
phase with a delay of about 2-6 hours, with the equatorward expansion of the
auroral oval, the mid-latitude ionosphere is taking the features of the auroral
ionosphere, which is accompanied by the development of medium- and small-scale
ionospheric plasma irregularities, causing radio signal distortions and
malfunctions of satellite-borne navigation systems. [5-10].
It was found that the electric field of
the polar cap ionosphere is screened by the system of the highest-latitude
field-aligned currents. The system is produced in the course of the
magnetospheric substorm during southward IMF. The screening is ideal before and
after the substorm, but it decreases (sometimes to zero) in the course of
loading and is restored during the active (unloading) substorm stage [11].
The other effects of strong heliophysical
and geomagnetic disturbances have been considered in papers [29-36].
At the ISTP, a series of theoretical and
experimental investigations was carried out into impulsive disturbances of the
ionosphere of a natural and technogenic origin (earthquakes, solar flares,
explosions, rocket launchings, underground nuclear testing). Within the
framework of these research efforts, the following results have been obtained:
*
The theory of MHD oscillations generated in the magnetosphere by pulsed sources
localized in the ionosphere has been constructed. As a result of such an
effect, the field of quasi-Alfv(n oscillations of a
universal kind is excited in the magnetosphere, which is determined by
magnetospheric parameters on those magnetic shells where the source is
localized [12, 13].
*
The method has been developed for detection and locating the sources of pulse
disturbances of the total electron content in the ionosphere, based on
processing the data from the global navigation GPS system. Whatever the type of
source, the pulse disturbance has the character of an N-wave with the amplitude
exceeding the level of background fluctuations by a factor of 2-5. The source
position corresponds to the portion of the trajectory of carrier rockets at a
distance no less than 500-1000 km from the launching pad, and at the flight
height no less than 100 km. During earthquakes, the source position coincides
with the epicenter. [14, 15].
The theory of eigen-oscillations of the
magnetosphere was further developed. In particular, the self-consistent problem
of resonance MHD oscillations in the axisymmetric dipole-like model of the
magnetosphere was solved. Magnetosonic waves are incident on the magnetosphere from
the solar wind region and excite Alfv(n waves on
resonance magnetic shells. The amplitude of the magnetosonic oscillations, when
they penetrate inside the magnetosphere, decreases several orders of magnitude.
The amplitude of the Alfv(n oscillations excited
inside the magnetosphere can be comparable with or even exceed the magnetosonic
wave amplitude in the solar wind region. [16-23].
A new mechanism has been proposed for the
formation of the cosmic-ray energy spectrum by coronal mass ejections. The parameters
of the resulting spectrum determine the electromagnetic and scale
characteristics of solar wind features, which are responsible for the sporadic
phenomena in the heliosphere. This is an essential prerequisite to the
development of monitoring and forecasting techniques for electromagnetic and
radiation conditions in interplanetary space, which is extremely necessary when
dealing with the "space weather" issues [24].
The model of the galactic cosmic ray
origin has been suggested. It was shown that within the framework of the
"surfing-tron" acceleration mechanism it is possible to explain the
formation of the energy spectrum right up to the most ultimate energies
observed on the ground. A detailed consideration was given to: the acceleration
mechanisms, the injection problem, the galaxy sources of cosmic rays, the
cosmic ray energy losses during the propagation in galactic plasma, and others.
Acceleration characteristics of both the ion and electron components of cosmic
rays have been determined [25].
The model has been developed for the open
ion-cyclotron resonator that forms in the neighborhood of the equatorial region
of the magnetosphere because of the presence in plasma of an addition of heavy
oxygen and helium ions. Ion-cyclotron waves with a frequency of about 1 Hz are
confined within the resonator and are enhanced through the wave-particle
interaction with resonance ions. Some of the wave energy leaks through the end
walls thus penetrating to the ground and is observed there as discrete wave
packets (geomagnetic Pc1 pulsations). The proposed model readily explains
satellite observations, which bring to a deadlock the previous models of
generation of discrete ion-cyclotron emissions. The model gives significantly
greater insight into the role of ion-cyclotron wave activity in magnetospheric
processes and opens up brand new vistas for the diagnostics of geospace plasma.
[26-28].
International
activities that were carried out on the IAGA topics
A development of important international
significance was the creation of the
Furthermore, three Russian-Mongolian
conferences on astronomy and geophysics were held to discuss results of
cooperation in the field of geomagnetism and solar-terrestrial connections.
The Institute organized and participated
in the preparation of two international symposia on "Atmospheric and Ocean
optics. Atmospheric Physics" held in 2001 and 2002 at
Participation
in international projects
Institute staff members are engaged in
collaboration with the
In accordance with the ongoing
international "Active cavity radiometer for measuring solar
luminosity" project (
Cooperative investigations into solar
activity are carried out under agreements on scientific cooperation with
Nobeyama Radio Observatory (
Magnetic observatory "
Under the agreement on scientific
cooperation with the MIT Haystack Observatory (USA), programs of joint
ionospheric research by the method of incoherent scatter have been worked out
and are being implemented.
Institute staff members are engaged in a
number of international INTAS projects. In particular, under infrastructure
project IA-01-01 CRENEGON, initiated by the ISTP, upgrades to magnetic
observatories
References
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investigation of the upper atmospheric optical radiation in the line of atomic
oxygen 557.7nm in
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Mikhalev A.V. Some observational characteristics of
mid-latitude airglows and upper-atmospheric emission disturbances during
magnetic storms over the region of east
5.
Afraimovich E.L., Berngardt O.I., Zolotukhina N.A., Shpynev B.G. Correlation of
geomagnetic field Ps6 pulsations and variations in total electron content and
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V.V., Leonovich L.A., Lesyuta O.S., Mikhalev A.V., Yakovets A.F. Simultaneous
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Yakovets, A. F. Simultaneous radio and
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Shirapov D.Sh., Mishin V.M., Urbanovich V.D. Saturation effect of the
ionospheric electric field during strong disturbances.
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Leonovich A.S., Mazur V.A. Standing Alfven waves in the magnetosphere from a
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Afraimovich E.L., Kosogorov E.A., Plotnikov A.V. Shock-acoustic waves generated
during rocket launchings and earthquakes.
Kosmicheskiye issledovaniya, 2002, v.42, No.3, pp.261-275.
15.
Afraimovich, E.L., Kosogorov E.A,. Perevalova N.P,
Plotnikov A.V. The use of GPS-arrays in detecting shock-acoustic waves
generated during rocket launchings // J. Atmos. Solar-Terr. Phys.- 2001.- Vol.63, N18,- P.1941-1957.
16.
Dmitrienko I.S. Nonlinear non-stationary Alfven resonance // Geophysical
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Leonovich A.S., Mishin V.V. Energy flux of magnetosonic waves from the solar
wind to the magnetosphere. Geomagnetizm i aeronomiya, 1999,
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acceleration in galactic plasmas. Journal of
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magnetospheric ion-cyclotron resonator. Doklady RAN, 2002,
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29.
Degtyarev V.I., Popov G.V., Chudnenko S.E. The dynamics of
trapped electron fluxes injected into geostationary orbit during magnetic
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30.
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variations over the East-Siberian region. Geomagnetizm i
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BRIEF REPORT ABOUT THE MOST IIMPORTANT SCIENTIFIC
RESULTS OBTAINED DURING 1999-2002 BY THE POLAR GEOPHYSICAL INSTITUTE (PGI) OF
THE
(Compiled by Dr. E.D.Tereschenko )
1.
Main Science Results
A modern type observatory has been constructed and put into operation at the Spietzbergen archipelago with the aim of multi-instrumental monitoring of geophysical phenomena at high latitudes. The observatory facilities provide digital registration of geomagnetic pulsations in the 0.1 through 20 Hz frequency range, satellite radio probing of the ionosphere, all-day-round television registration of auroras during winter seasons, measurements of total ozone content and of meteorological parameters. In coordination with the satellite, radar, and other types of measurements the observatory major operation objectives are to study the complex processes of the solar wind interaction with the terrestrial magnetosphere, to provide data for theoretical modeling and forecasting of the state of the high latitude ionosphere, to study the effects of the solar and geophysical factors on the climate and biological systems in the Arctic.
A unique
facility, territorially extended over a wide area, for measurements of extra
low frequency (ELF) and ultra low frequency (ULF) electromagnetic fields,
incorporating receiving stations on the Kola peninsular and the Spietzbergen
archipelago has been also constructed and put into operation recently. The
facility allows registration of signals in both the wide band channel (0.1–1.0
kHz) and in narrow band channel (~5 Hz)
simultaneously at several frequencies.
The developed measuring system allows to obtain
experimental data of a new type on the structure of the lower ionosphere and
magnetosphere. At the same time, the
greater penetration depth into the natural conducting media for the ultra low
frequency fields makes it possible to use them for the development of the deep
terrestrial sounding techniques.
By the analysis
of low altitude satellite data and on the basis of comparison with ground observations
of Pc1 pulsations, for the first time, a type of energetic proton precipitation
closely related to generation of electromagnetic ion-cyclotron (EMIC) waves was
found and described. It is localized (~1˚
in latitude) precipitation burst within the zone of highly anisotropic fluxes
equatorward the isotropy boundary. Theoretical predictions on generation of the
EMIC waves (Pc1 pulsations) in the near-Earth equatorial plane region, where
drifting energetic proton contact the cold plasmaspheric plasma, were, for the
first time, experimentally confirmed using complex observations of cold plasma,
hot particles, and waves onboard several high- and low-orbiting
satellites. The EMIC wave generation
occurs within localized tubes with enhanced cold plasma density. The observations suggest multiple sources of
the waves and related proton precipitation.
Using the data of
the high-resolution induction magnetometer installed at the Lovozero
observatory of the PGI, the main features of a new kind of magnetic pulsations
at the Pc1 frequency range are investigated. The pulsations have a form of
series of 3-20 short-living bursts initiated by sudden increase of solar wind
dynamic pressure. It is shown that the
necessary condition for the excitation of a series of pulsations is the
presence of hot protons in the dayside magnetosphere. The first burst in a series is delayed by
about 1 minute with respect to the auroral riometric absorption enhancement,
which allows to estimate the velocity of the Alfven
wave propagating in the magnetosphere.
The first experimental evidence of the VLF/ULF chorus generation in the
backward wave oscillator (BWO) regime of the magnetosphere cyclotron maser has
been found from the results of ground-based and satellite observations. A new numerical model of the VLF/ULF chorus
generation to explain the dynamics of the VLF/ULF chorus elements is
developed. The model is based on the
assumption that the chorus element generation is the same as in the backward
wave oscillator (BWO). However, the
BWO-like generator is driven by some other dynamic system, which has a noise
component. In such a case the occurrence
of the so-called “on-off” intermittency regime is possible if the BWO-like
generator is near the generation threshold.
A power-law distribution of the time intervals between bursts of
generation is a manifestation of the intermittency regime. Just this power-law distribution has been
found from the ground-based and satellite observations.
Temporal
intensifications of the auroral hiss observed by the INTERBALL-2 satellite well
poleward from the auroral oval have been found to correlate with the auroral
intensifications during substorms or pseudobreakups. The hiss frequency correlates with the distance
between the satellite footprint and the location of bright auroral arcs. The frequency increases (or decreases) when
the distance also increases (decreases).
Such behavior can be explained by the propagation of quasi-electrostatic
whistler waves coming from a localized source placed near the aurora.
Using the data of
the high-resolution TV registration of auroras, a new type of multiple arc-like
forms has been found in pulsating and diffuse auroras. The forms look like a spatial series of
narrow bands of luminosity drifting poleward at the velocity of
~300 ì/s at ionospheric altitudes.
It is suggested that these forms result from the ionospheric
manifestation of the specific MHD waves propagating inside the internal blur
edge of the magnetospheric plasma sheet.
The forms are frequently observed before the onset of the magnetospheric
substorms and may be regarded as substorm precursors.
The Polar UVI
Imager observations in the Northern Hemisphere have been used to examine
morphological features of the dayside auroral transient events which are
identified as the sharp increase in the auroral luminosity with duration
lasting for 5-30 min and accompanied by longitudinal auroral displacement. Two types of the phenomena with the initial
brightening have been found: one in the prenoon (08-10 MLT), and the other in
afternoon (14-16 MLT) time sector, which exhibit distinctive
characteristics. The ground magnetograms
and the IMF signatures indicate that the auroral transients may result from
variations in the dynamic pressure applied to the prenoon or afternoon
magnetopause following abrupt changes in the foreshock geometry.
DMSP spacecrafts
observations have been used to construct the empirical model of the
The experimental
reconstructions of the two-dimensional polar aurora volume luminosity
distributions for the 427.8 and 557.7 nm emissions have been obtained along the
geomagnetic meridian using the tomography method. The particular feature of the derived
distributions is the lowering of the luminous structure bottom edge and maximum
volume luminosity heights in the northward direction. This result testifies for the systematic
increase of the precipitating electron flux hardness for the studied auroras in
the northward direction.
Using the
radiotomography method, for the first time an experimental reconstruction of
the ionospheric F-region electron density structure has been carried out
simultaneously with the reconstruction of the electron density in the Å-layer.
Tomographic reconstruction of the electron density structure simultaneously at
the Å- and F-layer heights allows to study the coupling
of processes that take place in different ionospheric regions. It also allows to compare
the electron density structure with the optical luminosity data.
From the analysis
of the simultaneous EISCAT data on the electric field in the F region of the high
latitude ionosphere and the radio tomography data obtained in the northern
Scandinavia during the international heating experiment in November 1997, it
has been shown that both artificial and natural electron density irregularities
in a plane perpendicular to the magnetic field were elongated in the direction
of the F region plasma convection.
For the first
time the reduction of the first and second Schumann resonance frequencies (7.8
and 14.2 Hz) during solar proton events has been found and investigated in
details. The effect duration is about
several hours. The mean decrease of the
first resonance frequency is about of 0.2 Hz and it agrees fairly well with the
results of theoretical calculations using the ionosphere model for solar proton
events.
Using the
database of atmospheric ozone measurements by the Arctic stations lasting for
many years of observations, it has been found that violation of the tropopause
quasistationarity condition in the region of the polar jet flow can result in
the formation of tropopause "folds" which are filled by the
stratospheric ozone. The quasihorizontal
advection process in the troposphere then leads to the formation of lenses-like
structures that have enhanced ozone content and the lifetime of 3 to 5
days. Because of atmospheric drift these
structures can move over large distances from the original polar jet area where
they are generated. So the ozone data
analysis presents the evidence of irreversible stratosphere - troposphere
exchange.
2. Participation in the International Projects
(abriged).
INTAS 99-0078
«Quantitative description of the magnetospheric dynamics on the basis
multi-satellite and ground observations». Head
organization - INTAS,
INTAS 99-0335
«Ionospheric Alfven resonator, ULF waves, and particles in the near-Earth
space». Head organization - INTAS,
INTAS 99-0502
«Fine space-time correlation between discrete electromagnetic emissions and
energetic particles in the near-Earth space». Head
organization - INTAS,
INTAS 2000-752
«Development of the Key Parameter Set for Space Weather prediction». Term: 2001-2003.
INTAS 01-0016
Spatial and temporal variations of tropospheric ozone and precursors over
INCO-Copernicus ERB IC 15 CT 98-0123 EXTRATERRESTRIAL. Head organization - INCO-Copernicus. Participants –SPbO IZMIRAN. Term: 1999-2001.
NATO EST.CLG 975144 «Fine
structure of electromagnetic emissions and precipitation of energetic
electrons». Chief –Dr. David Nunn,
IMAGE. Participants - Finish Meteorological Institute,
ICA2-CT-2000-10038 "The formation of the phytotoxic
substance trichloroacetic acid – its significance for desertification of
semiarid and arid regions in southern Russia and its influence on the natural
resources of Arctic regions in northern Russia". Head organization - UFZ Centre for Environmental Research
Barents-INTERREG-2. Head organization – EISCAT. Participants:
Tropospheric Ozone Research
(TOR-2). Head organization - Swedish
Environmental Research Institute;
Network Detection
Stratospheric Change (NDSC) – "Studies of the nitrogen dioxide vertical
distribution variations". Head organization - National
Institute of Water and Atmospheric Research (New Zeàland). Participants:
IPHA RAS,
3.
Major Recent Publications
Aladjev G.A., Evstafiev
O.V., Mingalev V.S., Mingaleva G.I., Tereshchenko E.D., and Khudukon B.Z.. Interpretation of ionospheric F-region structures in the vicinity
of ionisation troughs observed by satellite radio tomography. // Annales Geophysicae. –2001. –V.19. -P.25-36.
Beloglazov
M.I., A.Yu. Karpechko, G.N. Nikulin,
S.A. Roumjantsev. Surface ozone dynamics in the
Borodkova N.L., A.G. Yahnin, K. Liou, J.-A. Sauvaud, A.O. Fedorov, V.N. Lutsenko, M.N. Nozdrachev, and A.A. Lyubchich. Plasma sheet fast flows and auroral dynamics during substorm: A case study // Annales Geophysicae. -2002. -V.20. -Ð.341-347.
Galperin Y.I.,
J.-M. Bosqued, R.A. Kovrazhkin, A.G. Yahnin, Stationary Magnetospheric
Convection on
Kozelov B.V., Titova E.E., Trakhtengerts V.Y., Jiricek F., Triska P. Collective Dynamics of Chorus Emissions Inferred from MAGION 5 Satellite Data // Geomagnetism and Aeronomy. –2001. -V.41, N.4, -P.457.
Moretto T., M. Hesse, A.G. Yahnin et al. Magnetospheric
signatures of ionospheric traveling convection vortices // J.Geophys. Res.- 2002. -V.107, N.A6. - 10.1029/2001JA000049, SMP 5 1-9.
Nygren T.,
E.D. Tereshchenko, B.Z. Khudukon, O.V. Evstafiev,
M.S. Lehtinen, and M. Markkanen. Manifestations of
field-aligned currents in tomographic observations of the ionospheric F region
// Adv. Space Res. –2000. -V.26, N.6. -P.939-942.
Roldugin
V.C., M.I. Beloglazov, G.F. Remenets. Total ozone decrease in the
Roldugin
V.C., S.Kirkwood, Yu.P.Maltsev, A.A.Galakhov. EISCAT radar reflections from the
vicinity of a noctilucent cloud // Physics and Chemistry of the Earth. Part B.
–2000. –V.25, N.5-6. -P.507-509.
Roldugin
V.C., Yu.P. Maltsev, A.N. Vasiljev, E.V. Vashenyuk. Changes of the first
Schumann resonance frequency during relativistic solar proton precipitation in
the
Roldugin,
V.C., Y.P. Maltsev, G.A. Petrova, and A.N. Vasiljev.
Decrease of the first Schumann resonance frequency during solar proton events
// J. Geophys. Res. – 2001. –V.106. –P.18,555-18,562.
Safargaleev V.V., Kangas J., Kozlovsky A.E., Vasilyev A.N., Bursts of ULF noise excited by sudden change of solar wind dynamic pressure // Annales Geophysicae. –2002. -V.20, N.11. -P.1751.
Safargaleev
V.V., Lyatsky V.B., Gazey N. et al. The
response of the azimuthal component of the ionospheric electric field to
auroral arc brightening // Annales Geophysicae. –2000. -V.18, N.1. -P.65.
Safargaleev
V.V., Osipenko S.V., Vasilyev A.N. Spatially periodic arc-like forms in
pulsating auroras // Geomagnetism and
Aeronomy. –2000. -V.40, N.6. -P.38.
Tagirov V.R.,
Ismagilov V.S., Titova E.E., Perlikov A.M. Arinin V.A. Manninen J.,
Turunen T., K. Kaila. Auroral pulsations and accompanying VLF-emissions
// Annales Geophysicae. –1999. –V.17. –P.66-78.
Tereshchenko E.D.,
B.Z. Khudukon, M.O. Kozlova, O.V.Evstafiev, T.Nygrén,
M.T.Rietveld, A.Brekke. Comparison of the orientation of small-scale electron
density irregularities and F region plasma flow direction // Annales Geophysicae. –2000. -V.18, N.8. -P.918-927.
Tereshchenko E.D.,
B.Z. Khudukon, M.O. Kozlova, T. Nygren. Anisotropy of
ionospheric irregularities determined from the amplitude of satellite signals
at a single receiver // Annales Geophysicae. –1999. - V.17.
-P.508-518.
Tereshchenko E.D.,
M.O. Kozlova, O.V. Evstafjev, B.Z. Khudukon, T. Nygren,
M.T. Rietveld, A. Brekke. Irregular structures of the F layer at high
latitudes during ionospheric heating // Annales
Geophysicae. –2000. -V.18, N.9. -P.1197-1209.
Titova E.E, A.G.Yahnin,
F.Jiricek, J.Smilauer, M.M.Mogilevsky, T.V.Romantsova, A.A.Rusanov,
J.-A.Sauvaud, R.Smith. INTERBALL-2 observations of auroral hiss and the aurora
dynamics // Czech. J. Phys. –1999. -V.49, N.4a. –P.657-666.
Trakhtengerts V.Y.,
Demekhov A.G., Pasmanik D.L., Titova E.E., Kozelov B.V., Nunn
D., Rycroft M.J. Highly anisotropic distribution functions of energetic
electrons and triggered VLF // Geophys. Res. Lett. - 2001. -V.28, N.13. - P.2577-2579.
Vorobjev V.G.
Yagodkina O.I., Sibeck D., Liou K., Meng C.-I.
Vorobjev V.G. Yagodkina
O.I., Sibeck D.G. Newell P. Daytime high-latitude auroral pulsations:
some morphological features and the region of the Magnetospheric Source //
J. Geophys. Res. -1999. -V.104, N.A5.
-P.10135-10144.
Vorobjev V.G.
Yagodkina O.I., Sibeck D., Liou K., Meng C.-I. Polar UVI
Observations of dayside auroral transient events. // J. Geophys. Res. -2001. -V.106, N.A12. -P.28897-28911.
Vorobjev V.G.,
Yagodkina O.I. and Zverev V.L. Morphological features of bipolar
magnetic impulsive events and associated interplanetary medium signatures //
J. Geophys. Res. -1999. -V.104, N.A3.
-P.4595-4608.
Yahnin A. G., Sergeev V. A., Bosinger T., Sergienko T. I., Kornilov I.
A., Borodkova N. L., Thomsen M. F., Belian R. D., Sauvaud J.-A., Lutsenko V.
N., Skalsky A. A. Correlated Interball/Ground-Based Observations of Isolated
Substorm: The Pseudo-Breakup Phase // Annales Geophysicae. – 2001. -V.19. –P.687-698.
Yahnin A.G., V.A.
Sergeev, B.B. Gvozdevsky, S. Vennerstrom.
Reply on Comment by Y.I. Feldstein and Y.I. Galperin // Annales Geophysicae. – 1999. -V.17. –P.42.
Yahnin A.G., V.A. Sergeev, M.V. Kubyshkina, T.I. Pulkkinen, K. Liou, C.-I. Meng, V. Angelopoulos, N.L. Borodkova, T. Mukai, S. Kokubun, Timing and Location of Phenomena During Auroral Breakup: A Case Study // Adv. Space Res. -2002. -V.30, N.7. -P.1775-1778.
Yahnina T.A., A.G. Yahnin, J. Kangas, J. Manninen, Proton precipitation related to Pc1 pulsations // Geophys. Res. Lett. -2000. -V.27, N.21. –P.3575-3578.
THE MOST IMPORTANT RESULTS OF THE D.V.
SKOBELTSYN INSTITUTE OF NUCLEAR PHYSICS,
Magnetospheric studies
The
nature of explosion-like nonlinear processes in the dynamics of current sheets
was studied as applied to particular nonlinear mechanisms of a substorm burst
in the geomagnetic tail. When the magnetospheric system, during the substorm
growth phase, has approached the marginal stability condition, a catastrophe of
equilibrium takes place. Models are constructed of both "rigid" and
"soft" regimes of the equilibrium loss, when the substorm activation
arises either under action of external disturbance or autonomously, without
such an external trigger.
A.
P. Kropotkin, O. O. Trubachev, and K. Schindler.
Nonlinear Mechanisms for the Substorm Explosion in the
Geomagnetic Tail. Geomagnetism and Aeronomy, Vol. 42, No. 3, pp. 277-285, 2002.
A.
P. Kropotkin, O. O. Trubachev, and K. Schindler.
Substorm Onset: Fast Reconfiguration of the Magnetotail Caused by Explosive
Growth of the Turbulence Level. Geomagnetism and Aeronomy,
Vol. 42, No. 3, pp. 286-294, 2002.
Sporadic
fluxes of relativistic electrons play a crucial role in space weather. It has
been suggested that generation of such electrons in the magnetosphere is due to
intense nonstationary processes characteristic of a magnetospheric substorm.
Such intense electromagnetic disturbances are field-line-resonant poloidal
Alfven waves. The spatio-temporal model of their generation in the nightside
magnetosphere where they are observed as time-dependent substorm current wedges
and Pi2
pulsations,
was elaborated.
Antonova,
A. E., Yu. I. Gubar', and A. P. Kropotkin. A model of
spatio-temporal structure of the substorm electromagnetic disturbance and its
consequences. Phys. Chem. Earth (C), vol. 25, no1/2,
pp. 43-46, 2000.
Model
concepts of drift shell branching for energetic charged particles, and of their
trapping in the dayside high-latitude outer magnetosphere, in the neighbourhood
of the off-equatorial magnetic field minima, have been put forward as long ago
as 1968, by Shabansky and Antonova. There was a considerable experimental
support of those concepts, both in the missions of 60ties and 70ties and in
recent missions (Interball, Polar). Recently, the motion of energetic charged
particles was examined in a simple axially symmetric model of the magnetic
field near the neutral points in the outer dayside magnetosphere forming and
adiabatic trap [Antonova et al., 2001]. The boundaries of the particle trapping
region are determined in the coordinates which are similar to the McIlwain (L,B)-coordinates. In the paper [Antonova et al., 2003],
violation of adiabaticity of the energetic particle bounce motion was studied,
caused by the change from one field minimum to two minima and back, along the
particle longitudinal drift path. A "jump" of the second adiabatic
invariant was evaluated. It was demonstrated that the shell branching
accompanied by this jump happens in a rather narrow zone on the equatorial
plane adjacent to the dayside magnetopause. The particles mirroring near the
equator and traveling on the nightside through a region with a relatively
weak
field (about 40 nT), can, consequently, be globally trapped: instead of
escaping through the magnetopause, they come into the dayside cusps regions.
Antonova,
A.E., Gubar', Yu.I., Kropotkin, A.P., Trapped
Energetic Particles in a Model Magnetic Field of the Magnetospheric Cusp,
Geomagn. Aeron., 2001, vol. 41, no. 1, p. 8.
Antonova,
A.E., Gubar', Yu.I., Kropotkin, A.P., Effects in the Radiation Belts Driven by
the Second Adiabatic Invariant Violation in the Presence of High-Latitude Field
Minima in the Dayside Cusps, Geomagn. Aeron., 2003,
vol. 43, no. 1, p. 3-8.
A
method has been developed of kinetic numerical simulation of evolution of the
magnetotail current sheet, situated in a background
plasma, under the action of a weak MHD disturbance
arriving
from outside. It is shown that, due to nonlinear processes, the forced kinetic
current sheet (FKCS) with extremely anisotropic ion distributions and a
characteristic scale length of an order of background ion gyroradius,
is formed. All of the features of this structure correspond well to those
predicted by the theory we developed earlier. The FKCS formed in this way is a
site of magnetic field merging in the magnetotail. Electromagnetic energy flux
brought from both sides to the CS, is transformed
there into the energy of field-aligned ion flows.
Domrin
V.I., Kropotkin A.P. Kinetic model of fast current sheet evolution in the
magnetotail during a substorm. Sixth International Conference
on Substorms,
V.
I. Domrin and
A. P. Kropotkin. Kinetic Current Sheet Generation in the Geomagnetic Tail:
A
Particle-Code Simulation, Geomag. Aeron., 2003, v. 43,
no. 3.
New
experimental data on relativistic (1-5 MeV) electron flux dynamics from
geosynchronous satellites EXPRESS-A2 and A3 and on magnetosphere plasma fluxes
(0.1-12 keV) from meteorological satellite METEOR-3M were obtained for the solar
activity 23-d cycle maximum (2000-2002).
N.A.Vlasova,
E.V.Gorchakov, T.A.Ivanova, V.A.Iozenas, Yu.V.Kutuzov, et al. Monitoring System
of Radiation Conditions in the Earth's Magnetosphere aboard Russian
Communication, Navigation, and Television Satellites, Cosmic Research, vol. 37,
No. 3, pp. 230-239, 1999.
The
theory conclusion about coincidence of position of the injected during magnetic
storms relativistic electron flux maximum with location of the ring current
maximum and the minimal geomagnetic latitude of the western electrojet was
confirmed experimentally. The Lmax value
is determined from an empirically obtained formula:
(Dst (max = 2.75 ( 104
/ L4max . This formula is true in the whole range of known magnetic storms,
including the strongest one with (Dst (max = 600 nT on March 13 and 14, 1989. The
seasonal variation of outer radiation belt relativistic electron flux was
discovered. The flux maxima were
observed in spring and autumn.
L.V.Tverskaya. Diagnosing the
Storm-Time Ring Current and Other Magnetospheric Plasma Domains Using
Relativistic Electron Data, Adv. Space Res., Vol. 25, No. 1-2, pp. 2315-2318,
2000.
A
concept - "Geocorona of Hot Plasma" - was developed. This approach allows to explain
uniformly particle flux dynamics at the outer radiation belt, the ring current,
and the near plasma sheet and a complex of associated geophysical phenomena.
A.S.Kovtyukh.
Geocorona of Hot Plasma, Kosmicheskie Issledovaniya, vol. 39, No. 6, pp.
563-596, 2001.
The
developed theory of the Earth's magnetosphere plasma sheet with medium scale
turbulence has predicted a value for the plasma sheet diffusion coefficient in
the Z direction, makes possible to explain observed features and the amplitude
of electric field variations.
A
geomagnetic storm model based on experimentally observed radial and azimuth
gradient of plasma pressure was suggested.
E.E.Antonova.
Magnetostatic equilibrium and turbulent transport in Earth's magnetosphere: A
review of experimental observation data and theoretical approaches. International Journal of Geomagnetism and Aeronomy, Publ. by
American Geophysical Union Vol. 3, No 2, pp. 117-130, 2002.
The series of works was prolonged on
studying the energetic charge particle nonadiabatic motion in the dipolar
magnetic field. The Poincare mapping equation system for the description of
particle motion with c(e) < 0.4 was proposed.
S.N. Kuznetsov, B.Yu. Yushkov, Boundary of the
Adiabatic Motion of a Charged Particle in
a Dipole Magnetic Field, Plasma Physics Reports, Vol. 28, No. 4, 2002, pp.
342-350.
A
data base (http:// dec1.sinp.msu.ru/apev) is compiled for the study of the
solar and heliospheric origins of all geomagnetic perturbations with the daily
average index Ap>20 observed during the period of
current 23-rd solar cycle in 1997-2002 comprising its rising and maximum
phases. This work represents a part of the ESA -INTAS Project 99-00727
fulfilled currently by Max Planck Institute fur Aeronomie (
Bothmer
V., Veselovsky I.S., Dmitriev A.V., Zhukov A.N., Cargill P., Romashets E.P.,
Yakovchouk O.S. Solar and heliospheric reasons for geomagnetic perturbations
during the growth phase of solar cycle 23. Solar System
Research, 36, #6, 2002.
A
simple analytical model of the polarity reversal of the heliospheric magnetic
field is developed.
Veselovsky
I.S., Zhukov A.N., Panasenko O.A. Reversal of heliospheric magnetic field
polarity: theoretical model. Solar System Research, 36, #1, 2002.
Nonlinear
self-gravitation oscillations of the subphotospheric layers on the Sun coupled
to the luminosity variations are considered as a hypothetical physical
mechanism responsible for the empirical inverse relation between the duration
of the rising phase and the maximal amplitude of the solar cycle.
Veselovsky
I.S. and Tarsina M.V. Intrinsic nonlinearity of
the solar cycles. Adv. Space. Res., 29, #3, 417-420,
2002.
Variations
of the solar wind and the heliospheric magnetic field parameters with time
scales greater than an hour during three solar cycles are investigated. The
variations in all time scales from hours to many years are related to the
regular and irregular changes of the solar wind sources with open, closed and intermittent
magnetic configurations.
Dmitriev
A.V., Suvorova
A.V., Veselovsky I.S. Solar wind and interplanetary magnetic field parameters
at the Earth's orbit during the three solar cycles. Phys.Chem.
Earth (C), 25, #1-2, 125-128, 2000.
The
concept of the turbopause around the Sun is introduced and developed based on
the dimensionless scaling approach to the analysis of physically distinct
radiation MHD and plasma kinetic regimes in the solar wind formation region.
New dimensionless parameters like Faraday F, velocity-emission Ve and Trieste T
numbers are introduced to evaluate the relative role of potential and inductive
electric fields (F), radiation and plasma losses of the solar corona (Ve) and
the openness degree of different morphological elements on the Sun (T).
The
analysis of the SOHO/EIT data for the period of several years revealed the
existence of the significant contribution of the numerous intermediate
brightness elements that are globally distributed over large areas of the Sun
(up to 2/3 of the whole surface) to the global asymmetry and hence to the 27-
day variability of the solar radiation. During the low activity years this contribution is comparable or even dominate over the
more localized contribution of active regions and bright points.
Veselovsky I.S., Zhukov A.N., Dmitriev A.V.,
Tarsina M.V., Clette F., Cugnon P., Hochedez J.F. Global asymmetry of the Sun
observed in the extreme ultraviolet radiation. Solar Phys.
201, 27-36, 2001.
CORONAS-F satellite was launched on
A.V. Bogomolov, A.P.
Ignat'ev, K. Kudela, S.N. Kuznetsov, Yu.I. Logachev, O.V. Morozov, I.N.
Myagkova, S.N. Oparin, A.A. Pertsov, S.I. Svertilov, B.Yu. Yushkov, Parameters
of the Intense X-ray and Gamma_ray Radiation from Solar Flare of May 20, 2002,
as Observed from Coronas-F Spacecraft, Asrtonomy Letters, Vol. 29, N. 3, 2002,
pp. 199-204.
In
the frame of the reflection model, created at SINP, a concept about Sun's Local
Radiation Belts was suggested.
G.P.Lybimov
Sun's Local Radiation Belts, Kosmicheskie Issledovaniya, vol. 40, No. 6,
pp.610-615, 2002.
Systematic description of
structures and dynamics of flows originating at the thermal convection on the
Sun and in a flat horizontal layer of liquid heated from below, Rayleigh-Benard
convection, was performed.
A.V.Getling
"Rayleigh-Benard Convection: Structures and Dynamics",
I. Internal Magnetic Fields
The
magnetic laboratory of the P.P.Shirshov Institute of Oceanology of the
1.Petrographic
and petromagnetic studies of a collection of peridotites from various
localities on the Mid-Atlantic Ridge. Petromagnetic characteristics were
obtained of 26 samples from 14 localities near the axis of the Mid-Atlantic
Ridge, collected on the cruises of the R/V "Akademik Boris Petrov"
and the R/V "Faranaut" (samples collected by the manned submersible
Nautile). The study of the present collection show the correlation to be strongest
for peridotites that experienced extensive medium-temperature metamorphic
recrystallization, are characterized by broadly variable contents of the
magnetic phase at a rather large value of its grain size which corresponds to
some 20 micron. Overall, the increase in the degree of serpentinization of the
rocks during the mesh serpentinization stage is accompanied by a moderate
increase in the abundance of the magnetic phase. The relative size of magnetic
grains is small, averaging corresponds to 3 micron. It increases somewhat with
the degree of serpentinization. Rocks with an increased degree of
medium-temperature recrystallization occasionally exhibit an increased size of
magnetic grains. Increased mean sizes of magnetic grains, just as in rocks with
green serpentines, are detected only in rocks with intensive (over 25%)
manifestation of the preceding medium-temperature metamorphic
recrystallization. Therefore, the mean grain size of the magnetite that is
formed at various stages of serpentinization of oceanic peridotites is
1-7micron, the increase in magnetite content with the degree of rock
serpentinization and with the transition to the subsequent serpentinization
stage involving no perceptible change in the mean integrated size of magnetite
grains in the rocks. The data obtained afford the corollary that the origin of
magnetization in oceanic peridotites is due not only to their serpentinization,
but also to the preceding medium-temperature metamorphism of the rocks. Hence,
the thickness of the lithospheric magnetic layer beneath MOR axes, evidently,
is constrained not by the depth of the 350-400 C isotherm,
as is assumed in the current petromagnetic models for the structure of oceanic
lithosphere, but by the 580 C isotherm depth. The depth of this isotherm in axial MOR regions, according to
geothermal gradient estimates Bazylev and Silantiev, may range from 6 to 15 km.
This suggests that the uppermost layer of the lithospheric mantle beneath
The
conclusion is that the magnetization in MOR peridotites takes origin not only
from their serpentinization, but also from the preceding medium-temperature
recrystallization. The grain size of the magnetite that is formed at various
stages of serpentinization of oceanic peridotite averages 3-4 micron. For the
lower boundary of the magnetic layer of oceanic lithosphere, one should adopt
the depth of the 580C isotherm, corresponding to the Curie point for magnetite.
Accordingly, the thickness of this layer in MOR axial parts may reach 15 km.
B.
A. Bazylev, K. V. Popov, and V. P. Shcherbakov, Petrographic features of
oceanic peridotites as reflected by their magnetic characteristics. Russian Journal of Earth Sciences, Vol. 4, No. 3, June 2002 (in
Russian).
2.The
study of the thin structure of the anomalous magnetic field on aquatories.
On the basis of an original hardware -
methodical complex using the gradient method of measurements of a magnetic
field on oceans and seas, large volume of precision geomagnetic survey in
various regions of World ocean is executed to
investigate thin spatial structure of an anomalous magnetic field (AMF). The
received experience testifies to high efficiency of research of thin spatial
structure of the magnetic anomalies for the decision of problems of fundamental
geology, and also for the decision of a wide circle of applied tasks. The main
and most urgent is the task of detection on sea bottom of the flooded vessels
and other iron objects, and also ammunition creating ecological threat.
A.Gorodnitsky
& A. Filin. Techniques and
results of magnetic detection of dumped weapons in
3.
The analysis of a magnetic field of a late cenozoic
volcanos in the northern part of the Kuril island arch.
With
the purpose of division of an anomalous magnetic field into components
connected with different depths of a field sources, the analysis of an abnormal
magnetic field of three late cenozoic volcanos located
in the northern part of the Kuril island arch was executed. For this purpose
the materials of detailed geomagnetic surveys obtained in the cruises of the
R/V "Vulkanolog" were used. For the analysis of fields the program
complex ""SAPFIR" was used developed in by A.N. Ivanenko in the
Laboratory of Geomagnetic Researches. This software allows to
carry out every possible transformation and spectrum analysis. All
accounts are carried out in an interactive mode and are based on 2-D fast
Fourier transformation, that allows for short time to consider set of variants
and to choose most realistic one. The analysis of a magnetic field of these
volcanos consist in reduction of an initial field to a pole with meanings of
magnetic declination -6 degree., and inclination 60 degree, that meets to a
modern site of volcanoes. After a reduction to a pole a number of
transformations was executed and the spectrums of
initial fields were calculated. For the analysis the maps of anomalous magnetic
fields of three volcanoes were used. The analysis showed high efficiency of the
offered technique and allowed us to make conclusions that the deep character of
sources of magnetic anomalies probably is connected with deep eruption channels
is for a volcano 1.4. whereas local extremums are connected with internal
heterogeneity in a structure of this volcano.The basic contribution into
magnetic field above the Edelshtein volcanic complex bring basis of
construction, probably, generated on a deep break of northeast extending. For a underwater volcano 3.18., the significant contribution to
an observable field brings the component connected directly to the top part of
a cone, as well as, component connected with deep roots of a volcano. The age
of all three volcanos does not exceed 0.7 ml. years.
A.Gorodnitsky.
Nature of magnetic anomalies and structure of an oceanic crust in
slow-spreading ridges. Izvestiya,
A
new scheme of terrestrial paleoclimate evolution during the last 1.5 ma in the
western
On
the base of archaeomagnetic investigations according the data for different
regions in longitudinal sector 4-136 degrees E it is shown the existence of the
eastward drift of 8000-annual variation in the geomagnetic field intensity.
This fact is required the change viewpoint on nature of secular variation of
geomagnetic field.
The
correlation between the magnetic moment and climate variations with
characteristic times of 10-10 yr is traced for 450 kyr, but the observed
relationship is complex: the relation between the geomagnetic moment and
paleoclimate changes becomes substantially weaker, which is shown in high
correlation coefficients outside the periods of the geomagnetic excursions and
in a very low correlation during these periods. A revised time scale of
excursions of the geomagnetic field in the Brunhes epoch is created. The
relation between excursions and the magnetic moment minima is confirmed.
The
large volume of the magnetostratigraphic investigations of the Lower Paleozoic
key sections of the Siberian platform has been carried out. The obtained data
indicate the occurrence of a reversed polarity superchron between the Uppermost
Tremadoc and the Middle Llandeilo, including the Arenig and the Llanvirn. This
superchron would have duration of about 25 to 30 Myr. Our new results indicate
that the Middle Cambrian is characterized by at least 60 magnetic intervals
that give a magnetic reversal frequency not less than ~5.5 to 7.0 reversal frequency per Myr during the Middle Cambrian. It confirms
that a strong decrease in magnetic reversal frequency happened between the
Middle Cambrian and the upper part of the Ordovician when a superchron probably
existed. This behavior is clearly reminiscent to the one prevailing before the
Cretaceous normal superchron. It is also in agreement with the persistence of a
~150-200 Myr time constant in changes in magnetic reversal frequency over the
whole Phanerozoic.
Tsatskin,
F. Heller, T.S. Gendler, E.I. Virina, S. Spassov, J. Du Pasquier, J. Hus, E.A.
Hailwood, V.I. Bagin, S.S. Faustov. A new scheme of terrestrial paleoclimate
evolution during the last 1.5 ma in the western
Morner
N.-A., Petrova G.N., Pilipenko O.V., Raspopov O.M., Trubikhin V.M. Excursions
in relation to the variation in the Earth's magnetic moment file://Fizika
Zemli. 2001. N 10. P. 24-32. (in Russian and English).
Petrova
G.N., Pilipenko O.V., Raspopov O.M., Trubikhin V.M. The Relation between
geomagnetic field variations and climate changes at different characteristic
times // Geomagnetism and Aeronomy. 2001.V. 41. N 2. P. 272-288 (in Russian and English).
Nachasova
I,E., Burakov K.S., and Bernabeu J. Archaeomagnetic studies of ceramic from the
Spain multilayered Neolithic Cendres Cave monument // Geomagnetism and
Aeronomy, 2002, T.42, N.6, pp.845-851, (in Russian, translated in English).
V.
Pavlov, Y. Gallet. Middle Cambrian high magnetic reversal frequency (Kulumbe
river section, northwestern
Didenko
A.N., Bondarenko G.E., Sokolov S.D., Kravchenko-Berezhnoy I.R.
Jurassic-Cretaceous history of the Omolon massif, northeastern Russia: Geologic
and paleomagnetic evidence // In: Tectonic evolution of the Bering Shelf - Shukchi
Sea - Arctic Margin and adjacent landmasses. Ed. E.L. Miller,
A. Grantz, and S.L. Klemperer. Pub. by the Geological Society of
Geoelectromagnetic Research Institute RAS has organized in
Scientific
program of MEEMSV-02 included 7 sections:
·
electromagnetic investigations in
seismic and volcanic areas;
·
electromagnetic images of active
zones;
·
Earth’s crust structure and
physical properties of rocks;
·
studies of seismo-electric and
seismo-magnetic effects;
·
electric, magnetic and
electromagnetic monitoring of seismic and volcanic activity;
·
ionosphere – lithosphere EM
coupling;
·
data
processing and instrumentation.
The Workshop was followed by the first business meeting of the
IAGA/IASPEI/IAVCEI Working Group EMSEV (Electromagnetic Studies of the
Earthquakes and Volcanoes, Chairman – Prof. S. Uyeda), established in January
2003.
II.Aeronomic Phenomena
4.
In 1999 when the MIR space station stopped functioning joint Russian-French
works on the atmospheric lidar sounding from the station have been accomplished
(ALISSA project). During 1996-99 about 60 sounding sessions of different types
of clouds were conducted under night conditions. Engineering methods of lidar
information processing were developed and data on geometric and optical
characteristics of cloudiness were obtained in the E.K.Fedorov Institute of
Applied Geophysics.
3.
New data on absolute values and variations in the solar ultraviolet emission
fluxes at the initial phase of a solar activity decline in the 23-rd cycle were
obtained as a result of measurements with SUFR and VUSS equipment onboard
CORONAS-F satellite in 2001 - 2002. Processing of data on the extreme ultraviolet
irradiance from CORONAS-F satellite made it possible to determine radiation
fluxes at the epoch of the onset of a solar activity decline in the 23 cycle.
The main task which had to be solved with the SUFR equipment was to obtain a
flux value of the solar EUV irradiance and to determine possible variations
associated with solar activity. From SUFR measurement data in the period of
observations the solar radiation (emission) intensity in a hydrogen line was 10
erg cm-2s-1, the solar emission flux in the EUV-region at (< 130 nm ) on the average, amounted to 11-11,5 erg cm-2s-1.
Flux
values correspond to the maximum solar activity phase that confirms the
assumption about an unusual behavior of the Sun in the 23-rd cycle.
Investigations
of the line intensity variations during flares showed that the increase in line
Lyman-alpha flux does not exceed a few percent even during the most strong flares.
It
is essential for aeronomy tasks that from VUSS equipment measurements onboard
CORONAS-F intensity variations in this line from day-to day do not exceed 1% as
well.
Measurements
of the extreme ultraviolet radiation complement considerably continuous time
series of data on the UV radiation. These data were used for a model of a EUV
background flux as part of a general model of electromagnetic radiation
variations in the solar
cycle.
A.A.Nusinov,
T.V.Kazachevskaya, V.V.Katyushina, D.A.Gonykh Instruments and measurements of the solar EUV irradiance onboard CORONAS-F at
the solar activity maximum period \\Conference
Innovative Telescopes and Instrumentation for Solar Astrophysics (AS20)
22-28 August 2002,
Nusinov
A.A., Kazachevskaya T.V., Katyushina V.V., Gonyukh D.A. Measurements of the
Solar EUV Irradiance Onboard Coronas-F at the Solar Activity Maximum Period \4
th (Virtual) Thermospheric\Ionospheric
Geospheric Research (TIGER) Symposium.
DATE:
2.
Data on the F2-layer critical frequencies observed at 25 ionospheric stations
of the Eastern hemisphere have been analyzed. A special method developed at the
A.D.Danilov.
Trends of the F2 layer critical frequencies independent of the geomagnetic
activity. Geomagnetism and Aeronomy, v.43,N 2, 2003
The ionosphere was investigated at "Mir"
manned space station during 1998-1999 by the method of radio sounding from
extremely low heights of 340-370 km. The experimental results have confirmed
the stated earlier hypothesis about an opportunity of definition of all
necessary ionosphere parameters for a radio communication at an ionosonde
location at these heights. At sounding from heights lower than a maximum of
ionization were received new unknown earlier ionograms. The quantitative data
processing has shown, that these ionograms testify the existence of macro scale
and rather specific ionospheric heterogeneities.
Danilkin
N.P. The results of the satellite radio sounding of the ionosphere below the
F-layer maximum. International Journal of Geomagnetism and
Aeronomy, 2001, vol. 3, ¹ 2, pp.173-180.
Danilkin
N.P., Review of the results of the satellite radio sounding of the ionosphere
in the vicinity of the F-layer maximum Proc. GA URSI, August 2002, (Session:
Gji); ¹625;
Danilkin
N.P. and Kotonaeva N.G., The features of ionospheric radio sounding performed
using the "Mir" space station; Radiophysics and Quantum Electronics,
Vol. 45, No. 6, 2002, pp. 431-439.
III.Magnetospheric Phenomena
The
main wave geomagnetic response of the interaction of the front edge of an
interplanetary magnetic cloud with the Earth's magnetosphere represents the
Pc5-6 (1-3 mHz) geomagnetic pulsations generation at
the polar cap with the highest intensity near dayside polar cusp. The critical
role in these processes plays the existence strong wave IMF fluctuations under
high and variable solar wind dynamic pressure. The time of the appearance and
main spectral and wavelet structure of geomagnetic pulsations on the ground and
IMF fluctuations on the front edge of the magnetic cloud sometimes were roughly
similar. We assume that the polar Pc5-6 geomagnetic pulsations could be results
of a direct penetration and transformation of turbulent hydromagnetic IMF waves
into the open magnetosphere as well as wave generation at the ionosphere
altitudes by quasi-periodic particle precipitation modulated by compression IMF
oscillations.
Kleimenova
N.G., Kozyreva O.V., Bitterly M., Schott J.-J. Long period (1-6 mHz) geomagnetic pulsations in the initial phase of the
large magnetic storm on
Kleimenova
N.G., Kozyreva O.V. Daytime high-latitude geomagnetic pulsation response to the
front edge of the magnetic clouds //Physics of Auroral Phenomena, 25 Annual
Seminar, Apatity, 26 Feb.-02 Mar.2002. Abstracts, p.46.
Manninen
Î., Kleimenova N. G., Kozyreva O.V., Ranta À. High-latitude geomagnetic
pulsation response to the passage of the front edge of the interplanetary
magnetic cloud of January 10, 1997 //J. Atm. Solar-Terr. Physics. Vol. 64/17. pp. 23-32, 2002.
IV. Solar Wind and Interplanetary Magnetic Field
P.N.Lebedev
Physical Institute and the
1.
The estimates of the turbulence outer scale are deduced in the range of
heliocentric distances between 7 and 80 solar radii from the processing of very
long observation series of the frequency fluctuations by the solar radio occultation experiments
with the GALILEO and ULYSSES spacecraft. The radial dependence of the
turbulence outer scale is shown to be approximately linear with the typical
scale value of order of 1011 cm. The outer scale is one of the most important
characteristics of turbulence because the spectral energy flux from the large
scale to small scale disturbances is formed in the spectral range near this
scale providing a quasi-steady regime of turbulence in the moving plasma flow.
The model of turbulence evolution is developed based on assumption that the
outer scale is formed as a result of competition between the linear
amplification of Alfven waves in smoothly irregular moving plasma and nonlinear
cascading of turbulence energy to small scale spectral range. The comparison
between the observational data and the possible versions of theoretical model
shows that the main nonlinear processes responsible for the formation of the
inertial spectral range are three-waves decays with
the participation of Alfven and magnetosonic waves.
Chashei
I.V., Bird M.K., Efimov A.I. On the outer scale of turbulence in the solar
wind // Proc. Solar Wind 10 Conf. 2003 (in press)
2.
The turbulence regimes in the solar wind acceleration region are investigated
in a wide range of heliolatitudes and heliocentric distances using frequency
fluctuations measurements of the occulted radio signals of the GALILEO and
ULYSSES spacecraft. It is shown that the power exponent of 1D large scale turbulence
spatial spectrum changes from 1 to 1.6-1.7 by the increase of heliocentric
distance from < 10 solar radii to > 20 solar radii at low heliolatitudes,
while the turbulence spectrum remains flat up to heliocentric distances about
30 solar radii at high heliolatitudes. In the several observation series the
unusual turbulence spectra with sharp break at the fluctuation frequencies
about 0.02 Hz were for the first time detected. Break
spectra were observed only at heliocentric distances less than 10 solar radii
and only by sufficiently low fluctuations levels.
Samoznaev L.N., Efimov A.I., Andreev V.E.,
Bird M.K., Chashei I.V., Edenhofer P., Plettemeier D., Wohlmuth R. Turbulence
regimes of the solar wind in the region of it's acceleration and initial stage
of supersonic motion // Proc. Solar Wind 10 Conf. 2003 (in press)
3.
The analysis of the statistical characteristics of the frequency fluctuations
of ULYSSES and GALILEO spacecraft occulted radio signals was carried out using
the solar wind speed values estimated from simultaneous fluctuation
measurements at widely spaced ground based receiving sites. The estimates of
the fractional plasma density fluctuations are obtained in the range of
heliocentric distances between 7 and 31 solar radii. Some tendency to the
fractional turbulence level increase with heliocentric distance increasing was
found from the observational data.
Efimov A.I., Armand N.A., Samoznaev L.N., Bird
M.K., Chashei I.V., Edenhofer P.,
Plettemeier D., Wohlmuth R. Characteristics of the near Sun solar wind
turbulence from spacecraft radio frequency fluctuations // Proc. Solar Wind 10
Conf. 2003 (accepted)
4.
Two-fluid hydrodynamics model was developed describing protons and pick-up ions
in the outer heliosphere. Thermal properties of particles in this model are
defined by the competition of three effects: 1) adiabatic cooling, 2) heating
by damped MHD waves of the solar wind background turbulence, 3) heating by MHD
waves generated by pick-up ions by the evolution of their pitch angle distribution
from unstable toroidal distribution to stable bi-spherical distribution. The
comparison between two heating sources of the protons shows that heating
process is connected mainly with pick-up ions at heliocentric distances greater
that 10 AU while heating at smaller distances is dominated by background
turbulence. The radial profiles of protons temperature and effective polytrope
index found from the model are in a good agreement with the measurements of
distant spacecraft PIONEER 10,11 and VOYAGER 1,2. The
expected latitudional profile of the proton temperature was found taking into
account the dependence of solar wind speed on heliolatitude. The radial
dependence of the pick-up ions temperature was also calculated showing that the
pick-up ions temperature approach asymptotically to a constant value which is
dependent only on solar wind speed.
Fahr
H.J., Chashei I.V. On the thermodynamics of MHD wave-heated solar wind protons
// Astron. Astrophys. 2002. V.395. P.991-1000
Chashei
I.V., Fahr H.J., Lay G. A consistent thermodynamics of the MHD wave-heated two
fluid solar wind // Annales Geophys. 2003 (in press)
5.
Quasi-periodic magnetic field fluctuations with typical period about 4-5 min
were for the first time detected in the solar wind acceleration region. This
result was deduced from the analysis of temporal Faraday rotation fluctuations
of the HELIOS spacecraft polarized radio signals by the coronal occultation
experiments. The value of fractional magnetic field amplitude of quasi-periodic
fluctuations is about 0.1 at heliocentric distances 3-10 solar radii as it
follows from our estimations. Quasi-periodic magnetic field fluctuations can be
explained by the isolated Alfven waves trains propagating away from the Sun
from the inner solar atmosphere. The conclusion was drawn that the 5 min Alfven
waves can be of considerable importance in the energy balance of the outer
solar corona and of the solar wind acceleration region. Typical transversal
scale of the propagating 5 min magnetic field disturbances projected to the
Sun's surface is about 30 000 km. That means that quasi-periodic Alfven
disturbances seem to be generated initially in anisotropic non-steady magnetic
structures of the chromospheric network.
Chashei
I.V., Bird M.K., Efimov A.I., Andreev V.E., Samoznaev L.N., Five minute
magnetic field fluctuations in the solar wind acceleration region // Solar
Phys. 2000. V.189. P.399-413.
The model of large scale magnetic variations
at the coronal base was developed and applied to the interpretation of
line-of-sight magnetic field behavior peculiarities at solar polar caps.
Yu.V.Pisanko. A model of the
magnetic field long-term evolution at the coronal base and polar heliospheric
regions. Space Science Reviews, vol.97, pp. I83-I87, 2001.
Report
on activity of Solar and Cosmic Ray Research Laboratory of Lebedev Physical
Institute (
Long-term
cosmic ray monitoring in the Earth's atmosphere has been performed since 1957
up to now with balloon borne Geiger counters at a number of latitudes several
times a week. During 1999-2002 the observation were made at the Arctic,
Antarctic and
The
main results in 1999-2002 are the following:
(1)
Analysis of the cosmic ray fluxes in four consecutive minima of solar activity
showed the negative trend of (0.01-0.09)% per year. It
was suggested that the trend in the cosmic ray fluxes is due to supernova
explosion at the distance of 30-150 parsec 104-5x105 years ago.
(2)
From the correlation between the interplanetary magnetic field and the cosmic
ray fluxes on the Earth's orbit and from analysis of cosmic ray measurements by
the ground-based and balloon borne detectors, it was shown that the average
magnetic flux from the Sun was constant within limits of (5-7)% in the period
from ~1940 up to now.
(3)
About 100 solar proton events were observed in the polar atmosphere in
1958-2002. It was found that protons
with E<500 MeV generated in the solar flares are accelerated further at the
shocks associated with coronal mass ejections, their energy losses in the solar
corona being compensated. However, the acceleration rate is not enough to
compensate the energy losses of protons with E>500 MeV and the later do not
reach an observer at the Earth in the case of a flare occurred eastward from
the Sun's central meridian.
(4)
Simulation of phenomena in the solar corona for a well known Bastille Day event
(
(5)
It was shown that a phenomenon of local minimum in solar activity around the
maximum phase of the 11-year cycle (double-peaked structure or the Gnevyshev
Gap) could be a sequence of superposition of quasi-biennial and 11-year
oscillations, the amplitude of the former changing in phase with the 11-year
cycle. The result was found from the sunspot area, optical solar flares, and
photospheric magnetic field data considered separately for the northern and
southern solar hemispheres in solar cycles 21 and 22.
(6)
More than 400 events of relativistic electron precipitation were observed in
the cosmic ray balloon experiment (1957 to 2002). The occurrence rate of
electron precipitation demonstrates an 11-year cycle with a maximum at the
descending branch of a solar cycle in accordance with the rate of corotating
solar wind streams from solar coronal holes. A special kind of electron
precipitation with a rather hard energy spectrum happens against a background
of solar particle events.
(7)
Close correlation was found between cosmic ray fluxes and atmospheric processes
such as thundercloud electricity, lightning production, cloudiness coverage,
and precipitation. The chain of solar-terrestrial relationship was established:
solar activity - cosmic ray modulation - changes in the global electric
properties of the atmosphere - changes in weather and climate
Main
publications.
Bazilevskaya
G.A., Fluckiger E.O., Krainev M.B., Makhmutov V.S., Sladkova A.I., Storini M. The Gnevyshev gap effect in solar cosmic rays. - Proc. 26th
Int. Cosmic Ray Conf., 1999, v. 6, p. 240-243.
Bazilevskaya
G.A., Krainev M.B., Makhmutov V.S. Effects of cosmic rays on the Earth's
environment. - J. Atm. Solar Terr. Phys, 2000, v. 62,
No. 17-18, p. 1577-1586.
Bazilevskaya
G.A., Krainev M.B., Makhmutov V.S., Fluckiger E.O., Sladkova A.I., Storini M.
Structure of the maximum phase of the solar cycles 21 and 22. - Solar Physics,
2000, v.197, No. 1, p. 157-174.
Bazilevskaya
G.A., Makhmutov V.S., Svirzhevskaya A.K., Svirzhevsky N.S., Stozhkov Yu.I.,
Vashenyuk E.V. Intrusion of energetic electrons into the polar atmosphere
during the solar proton events of 24 September,
2001. - Proc. XXV Annual Seminar, Apatity, 2002, p. 125-128.
Bilenko
Ermakov
V.I., Stozhkov Y.I. New mechanism of thundercloud electricity
and lightning production. - Proc. 11th Int. Conf. on Atmospheric
Electricity, 1999, p. 242-245.
Krainev
M.B., Storini M., Bazilevskaya G.A., Fluckiger E.O., Makhmutov V.S., Sladkova
A.I., Starodubtsev S.A. The Gnevyshev gap effect in galactic cosmic rays. - Proc.
26th Int. Cosmic Ray Conf., 1999, v. 7, p. 155-158.
Krainev
M.B., Bazilevskaya G.A., Makhmutov V.S. The general features of the galactic
cosmic ray intensity in the maximum phase of solar cycles 19-23. - Proc. 27th Int. Cosmic Ray Conf.,
2001, v. SH, p. 3847-3850.
Krainev
M.B., Bazilevskaya G.A., Makhmutov V.S. Solar magnetic field and dynamic
phenomena in cosmic rays. - Advances
in Space Research, 2002, v. 29, No. 3, p. 331-336.
Makhmutov
V.S., Kaufmann P., Costa J.E.R., Lagrotta P.R., Magun A., Arzner K.,
Bazilevskaya G.A., Shea M.A. Great solar bursts of October
19, 22 and 23, 1989. - Advances in Space Research, 2002, v. 29, No. 12,
p. 2101-2104.
Makhmutov
V.S., Storini M., Bazilevskaya G.A., Krainev M.B. Observation of energetic
electron precipitation events in the Southern polar atmosphere. Proc. 9th Workshop Italian Res.on Antarctic Atmosphere. Roma, 2001, p.433-443.
Makhmutov
V.S., Bazilevskaya G.A., Krainev M.B., Storini M. Long-term cosmic ray
experiment in the atmosphere: energetic electron precipitation events during
the 20-23 solar activity cycles. Proc. 27th Int. Cosmic Ray Conf., 2001, v. SH,
p. 4196-4199.
Minami
S., Morimoto M., Podgorny A.
Podgorny
Stozhkov
Y.I., Pokrevsky P.E., Okhlopkov V.P. On supernova explosion
in the nearby interstellar space. - Proc. 26th Int. Cosmic Ray Conf.,
1999, v. 4, p. 283-286.
Stozhkov
Yu.I., Pokrevsky P.E., Okhlopkov V.P. Long-term negative trend in cosmic ray
flux. - J. Geophys. Res., 2000, v. 105, No. A1, p.
9-17.
Stozhkov
Y.I., Ermakov V.I., Makhmutov V.S. Cosmic rays and atmospheric processes. -
Proc. 27th Int. Cosmic Ray Conf., 2001, v. SH, p. 4157-4160.
Stozhkov
Y., Okhlopkov V., Pokrevsky P. Cosmic rays tell us on supernova explosion in
the nearby interstellar space. - Nuclear Physics B (Proceedings Supplements),
2001, v. 97, p. 207-210.
Stozhkov
Y.I., Svirzhevsky N.S., Makhmutov V.S., Svirzhevskaya A.K. Long-term cosmic ray
observations in the atmosphere. - Proc. 27th Int. Cosmic Ray Conf., 2001, v.
SH, p. 3883-3886.
Stozhkov
Y.I. On the magnetic flux from the Sun in the last century.
Geomagnetizm and Aeronomy, v.42, No. 6, p.746-751.
Stozhkov
Y.I. The role of cosmic rays in the
atmosphere processes. - Journal Physics G: Nuclear Particles Physics, 2002, v.
28, in press.
V.Observatories, Instruments, Surveys, and
Analysis
1.
During past four years the E.K.Fedorov Institute of Applied Geophysics has been
performing within the framework of the National Heliogeophysical Service and
Regional Warning Center (RWC)
-conducted
heliogeophysical observations using its own ground-based and space facilities,
-coordinated
works of other observatories in the Russian region incorporated into the observational
network of the Service (I0 ionospheric and 13 magnetic stations).
-collected
and analyzed data from the network, prepared and issued current summaries and
forecasts, performed an
operative exchange of the information with other RWCs.
Ionospheric,
magnetic forecasts as well as forecasts on the radiation situation in the NES
have been regularly issued.
During
the period under consideration the Valkarkai station has been put into
operation, the
With
the launch of the "Meteor-3M" satellite monitoring observations of
the penetrating radiation fluxes were renewed in 2002 (solar and galactic
cosmic rays, energetic particles and the Earth's radiation belts) at 1000 km
heights (almost a 30-year series of observations at these orbits was
interrupted in I998).