Abstracts & Presentations

Abstracts

What can we learn from the Sun's interior useful for an understanding of Solar-Terrestrial links?

Rozelot Jean-Pierre⁽¹⁾, S. Lefebvre⁽²⁾, S. Pireaux⁽¹⁾, N. Fazel ^(1)
(1) Observatoire de la Cote d'Azur (OCA)- GEMINI, Av. Copernic, 06130 GRASSE, France Dpt
E-MAIL:rozelot@obs-azur.fr
⁽²⁾ Department of Physics and Astronomy, UCLA, Los Angeles CA 90095 USA

The baryonic Universe is mainly composed by plasma and so, magnetism plays a fundamental role. However magnetism is still poorly known. Equations of the magnetic field are not yet taken into account in all the equations describing our Universe, and in particular in stellar (and solar) equations. Nevertheless, it is known that the magnetism of the solar interior has a key role. Understanding its role also understands our terrestrial climate. In this lecture we will emphasize the Sun as a unique object for which we may hope a quantitative approach before generalization to other more energetic objects (young stars, final evolution stages)

The slow and organized activity of the Sun is not a superficial phenomenon: it implies the core, where the mass is concentrated, and we are still far to control mechanisms (rotation, spin...). We will describe how to progress and we will show that irradiance might be not only a surface manifestation of the magnetic activity, but could take its origin in deeper layers. So, a better modelization of the irradiance will lead to a better modelization of the response of our outer atmosphere. We will conclude by showing some dedicated space joint missions, such as SDO and GOLF-NG.

PLANS FOR THE INTERNATIONAL HELIOPHYSICAL YEAR (IHY)

Nat Gopalswamy
IHY Secretariat

Fifty years after the International Geophysical Year 1957-58, a new program for coordinated research is planned - the International Heliophysical Year. This tals presents an overview of the goals, organization, planning, campaign framework and overall schedule of the IHY

         

International Heliophysical Year (Overview)

Carine Briand
Meudon Observatory, France - IHY-European Section

This talk is an overview of the activities in Europe related to the International Heliophysical Year. The goals of the program, the organizational structure and the Coordinated Investigation Programs are described.

         

Statistic Study of Relationships Between Solar, Interplanetary and Magnetospheric Disturbances

We continue our investigation (see for instance, Yermolaev Yu.I., Yermolaev M.Yu. Statistical relationships between solar, interplanetary, and geomagnetic disturbances 1976-2000, Cosmic Research, v.40, N 1, p.1-14, 2002) where we study 25-year sets of solar x-ray observations, measurements of plasma and magnetic field parameters in the solar wind and Dst index variations with the purpose of revealing the factors rendering the greatest influence on development of magnetospheric storms and their variations in two solar cycles (1976-2000). Value of correlation (about 40%) between large solar phenomena (strong solar flares and halo-CMEs) and magnetic storms practically does not exceed a level of correlation of random processes. Furthermore it was not possible to find out any dependence between importance of solar flares and value of magnetic storms. The most geoeffective interplanetary phenomena are magnetic clouds (MC) which, as many believe, are interplanetary manifestations of CMEs and compressions in the region of interaction of slow and fast streams in the solar wind (Corotating Interaction Region, CIR). On the average the parts of moderate and strong magnetic storms (with Dst < -60 nT) generated by MC and CIR are equal about 30% each (for strong storms with Dst < -100 nT the part from MC is 1/2) but change in solar cycle: storms from MC have 2 maxima during start of rising and start of declining phases and storms from CIR have 2 maxima during end of rising and end of declining phases.

ADVANCING OUR UNDERSTANDING OF THE COSMIC RAY PROCESSES
THAT GOVERN THE SOLAR INFLUENCE ON EARTH AND PLANETS

Introduction. In the beginning of the cosmic era is established the important role of the different particle types in the extraterrestrial and interplanetary space: galactic cosmic rays (GCR), solar cosmic rays (SCR), radiation belt and aurora particles, solar wind (SW), etc. Because of that the energetics and the variations of these particles appear as essential aspect of solar-terrestrial physics. All energy fluxes in the interplanetary space with extrasolar origin are neglectable small in comparison with the energy fluxes from the Sun, at least near the Earth’s orbit. But namely GCR possess maximal penetration capability (Velinov, Nestorov and Dorman, 1974), which is by us the key of the understanding of solar-terrestrial relationships.

Cosmic rays and processes in space and Earth. Cosmic rays form the lower parts of the terrestrial and planetary ionospheres. They create in the Earth environment independent cosmic ray layer, so called C layer in the ionosphere D region, which is situated at heights 50 - 80 km (Velinov, 1966, 1968). Therefore they influence on the propagation on radiowaves, particularly in the range of medium, long and very long waves. The cosmic rays maintain the ionization not only in the ionosphere but also in the atmosphere, the hydrosphere and the lithosphere of the Earth.

CR determine the ionization rate and conductivities in the atmosphere and the ionosphere and therefore the atmospheric electric fields. The last influence the thunderstorms, Earth’s global charge and global electric circuit between the ionosphere and the ground. It is already established (Ermakov, 1992; Ermakov and Stozhkov, 2003), that the main cause of thunderstorm discharges are external atmospheric showers (EAS) of high energy primary CR particles with energy more than 10¹⁴ eV. CR produce also nuclear reactions with ground, water and air atoms. On this way cosmogenic nuclides in space, in bodies, and in atmospheres are created. Such cosmogenic isotopes are ¹⁰Be, ⁷Be, ³He and ³H (Dorman, 2004). All this shows the great importance of cosmic rays for the processes of solar-terrestrial relationships, solar-terrestrial physics and solar-planetary physics in the whole heliosphere.

On the mechanism of solar-terrestrial influences. We suppose the following heliogeo-magnetic mechanism (see the Figure): the Sun sends to the Earth different types of radiations - photons (visible optical OPT, infrared IR, X-rays, gamma rays, etc.) and particles (the permanent SW, the sporadic SCR, etc.). The Sun also generates magnetic field, i.e. the interplanetary magnetic field IpMF. The whole Solar system is radiated by GCR, which are generated in the supernovae stars and in the Nucleus of the Galaxy in the galactic center (GC). The solar wind and interplanetary magnetic fields modulate GCR with their cycles (11- and 22- years, 27-days, etc.). Besides in the magnetosphere, ionosphere and atmosphere exist 12- hour and diurnal variations. Consequently SW and IpMF modulate all primary and secondary GCR particles.

However GCR determine the chemistry and electrical parameters in the atmosphere. They create ozonosphere and influence actively on O₃ processes. GCR transmit to the ozonosphere their solar modulation. But the ozonosphere controls the meteorological solar constant and the thermal regime and dynamics (including the dynamics of the cloud system) of the lower atmosphere, i.e. the weather and climate (Velinov, 1998, 2000). This mechanism may be expanded still taking into account that the GCR create not only the atmospheric but the hydrosphere and lithosphere part of the ozonosphere also. The so shown mechanism of the solar-terrestrial relationships shows the way to a non-contradictory solution of the key problems of the solar-terrestrial physics.

CR spectrum and ionization. The observed CR spectrum can be distributed into the following five intervals: I (E = 3.10⁶ - 10¹¹ GeV/n), II (E = 3.10² - 3.10⁶ GeV/n), III (E = 30 MeV/n - 3.10² GeV/n), IV (E = 1 - 30 MeV/n) and V (E = 10 KeV/n - 1 MeV/n), where E is the kinetic energy of the particles (Dorman, 1977; Velinov, 2000). Some methods exist for calculating ionization by relativistic particles in CR intervals I, II and III. For the high latitude and polar ionosphere, however, intervals III, IV and V are also significant since they contain solar cosmic ray and anomalous cosmic ray components. Formulas for the electron production rate q(cm^-3s^-1) at height h in the planetary ionosphere as a result of penetration of energetic particles from intervals III, IV and V are deduced in this paper. For this purpose the law of particle energy transformation by penetration through the ionosphere - atmosphere system is obtained. A model for the calculation of the cosmic ray spectrum on the basis of satellite measurements is created. This computed analytical model gives a practical possibility for investigation of experimental data from measurements of galactic cosmic rays and their anomalous component (Velinov, Buchvarova, Mateev and Ruder, 2001).

3D-modelling GCR ionization in terrestrial atmosphere. 3D-model of the CR electron production rate q(h) (cm^-3s^-1) has been developed for the strato-mesosphere and lower thermoshere (altitude range 30 - 100 km) with 10 km step (Velinov and Mateev, 2005). The proposed 3D-model contains a theoretical part and numerical computation. The GCR spectrum is modelled with analytical expression with input data from CREME96 (2002). The longitudinal effect of CR ionization has been calculated. The longitudinal effect corresponds to the planetary distribution of the geomagnetic threshold rigidities R(GV). The atmosphere density profiles are taken from COSPAR International Reverence Atmosphere - CIRA 1989. In the polar regions the contribution of the anomalous CR with energies less than 50-60 MeV significantly increases (Velinov, 2004). These results provide a basis for quantitative understanding of the processes of space weather.

CR ionization in the planetary ionospheres. As a continuation of our studies of cosmic ray (CR) ionization in the atmospheres of the planets in the Solar system (Velinov et al. Adv. Space Res. 27, №11, 1901-1908, 2001) we present a new method for the calculation of the electron production rate q(h) profiles due to particles of all energy intervals: galactic CR, anomalous CR component and other types of high energy particles. In the above mentioned paper ionospheres of terrestrial planets are investigated, where the spherical model is used. For giant planets which have significant oblateness in spite of the isotropic penetration of the galactic CR in their atmospheres, the trivial integration on the azimuth angle is not applicable, because of the presentation of the planets as rotational ellipsoids and the azimuth dependence of the integrand function.

The difference between profiles for spherical q_S and ellipsoidal q_E models of the terrestrial planets (Earth, Venus and Mars) is small. These differences between q_S and q_E profiles increase significantly in the upper atmospheric layers of outer major planets Jupiter, Saturn, Uranus and Neptune. This requires the introduction of a modified Chapman function for oblate planet in the Particle Depth Parameter (PDP), while considering the CR influence and ionization processes in the ionospheres of the giant planets. New calculations for relative profiles q_E / q_S in the atmosphere of Saturn are presented. For this purpose an improved primary CR spectrum with a new type of smoothing function f with tangens hyperbolicus is used (Velinov, Ruder, Mateev, Buchvarova and Kostov, Adv. Space Res. 33, 232-239, 2004).

Conclusion. On 4 October 2007 will be marked 50 years of the first artificial satellite and the beginning of space exploration. Fifty years after the International Geophysical Year (1957-1958), the world scientific community will come again for an international collaboration: the International Heliospheric Year 2007. The term "heliospheric" is an extension of the term "geophysical" in the region of the whole Solar system. One of the objects of IHY will be undoubtedly the advancing our understanding of the cosmic ray processes that govern the solar influence on the Earth and planets.

Solar Variability and Climate - UTLS amplification of Solar signal

The solar signal in atmospheric interannual variability is well tracked till the stratosphere. However, it is still not clear how this signal propagate into the troposphere and does it affect Earth’s climate. The mechanism suggesting downward propagation of solar effect from the stratopause levels could account for strato- tropospheric teleconnections at middle to high latitudes, but is not applicable for very low latitudes, where the atmospheric angular momentum is almost constant. Some model experiments concerning tropical upwelling, point out the limitations of the concept of extratropical pump and downward control and contribution of stratospheric - tropospheric heating to the net tropical upwelling [Plumb and Eluszkiewicz-1999, Scott-2002].

Meanwhile, different sources of measurements show that at high solar activity the Upper Troposphere and Lower Stratosphere (UTLS) are warmer than at low solar activity. Based on this result and taking into account above-mentioned modelling, we propose an additional amplifying mechanism of the solar influence on climate. In brief:

1) the warmer tropical UTLS at solar maximum affects vertical propagation of equatorial waves, altering the duration of westerly QBO phas

2) the equatorial upwelling (enhanced in solar max), on its turn is modulated by QBO. This means that westerly phase of QBO will decrease the equatorial upwelling and respectively Brewer-Dobson circulation, but easterly phase of QBO will force additionally Brewer-Dobson cell.

Recent analysis of interannual variations of stationary planetary wave activity [W. Chen, M.Takahashi and H-F. Graf, 2003] serves as indirect conformation of this hypothesis.

____________
Chen W., M. Takahashi and H-F. Graf, JGR, 108, D24, 4797, doi:10.1029/2003JD003834, 2003.
Plumb R. and J. Eluszkiewicz, J.Atmos. Sci., 56, 868-890, 1999.
Scott R., J.Atmos. Sci., 59, 2745-2759, 2002.

Solar activity and global warming revisited

Georgieva Katya
Solar Terrestrial Influences Laboratory - Bulgarian Academy of Sciences E-MAIL:kgeorg@bas.bg

It has been found that while in general the changes in surface air temperature follow closely the changes in solar activity proving the solar influences on climate, in the last few decades solar activity has remained more or less constant while temperature has continued to increase implying that in this period solar activity has only a minor contribution to the global warming attributed to human activity.

When comparing long-term changes in solar activity to long-term changes in various terrestrial parameters, the solar activity index commonly used is the sunspot number as it has the longest data record. But sunspots reflect only the solar activity originating from closed magnetic field regions – solar flares, coronal mass ejections, magnetic clouds – drivers of sporadic geomagnetic activity. The regions of open magnetic field - coronal holes, sources of high speed solar wind and drivers of recurrent geomagnetic activity – are not accounted for in the sunspot index. If we analyze the relative contribution of different solar activity agents to the geomagnetic activity we see that in the last decades the impact of coronal holes has increased which is reflected in geomagnetic activity indices but not in sunspot index, and this is the reason for the decreasing correlation between sunspot number and geomagnetic activity. The long-term trends in geomagnetic activity and temperature are highly correlated in the whole period for which we have data. Therefore, geomagnetic activity indices accounting for disturbances caused by all solar activity, not only the one originating from closed magnetic field regions, is more appropriate for evaluating solar influences on terrestrial processes, while using the sunspot number alone as a measure of solar activity leads to the underestimation of the role of solar activity for the global warming in the recent decades.

Long-period trends in global seismic and geomagnetic activity and their relation to rate of change of solar activity.

Odintsov, S.⁽¹⁾., Ivanov-Kholodny, G.⁽¹⁾., Georgieva, K.⁽²⁾., Kirov, B.^(2)
(1) Pushkov Institute of Terrestrial Magnetism, Ionosphere and Radio Wave Propagation,
Russian Academy of Sciences (IZMIRAN), E-MAIL:sodin@izmiran.ru
⁽²⁾ Solar-Terrestrial Influences Laboratory at the Bulgarian Academy of Sciences

In the present paper we are comparing the century-scale trends and decadal variations in seismic activity, and are looking for a relation to century-scale and decadal changes in solar and geomagnetic activity. Also we use the rate of change of the sunspot numbers, both from year to year in the 11-year solar cycle, and in different cycles. The rate of change of the sunspot numbers is compared to the total yearly seismic energy from the global NOAA-NEAC catalogue. Besides, the variations in the solar wind speed are compared to the seismic processes on the Earth. The possible mechanisms of solar activity influences on seismic activity are also discussed.

         

Influence of Solar Activity on Sudden Cardiac Death and in other Processes on the Earth

Gigolashvili Marina ^(1,3), F. Halberg⁽²⁾, G. CornИlissen⁽²), E. Babaev), G. Ramishvili⁽¹⁾
K. Janashia ⁽⁴⁾, F. Mustafa, L. Tvildiani⁽⁴⁾, V. Kukhianidze ^(1)
(1)Georgian National Astrophysical Observatory of Georgian Academy of Sciences E-MAIL:marinagig@yahoo.com
⁽²⁾ University of Minnesota, Minneapolis, MN, USA;
⁽³⁾ Shamakhy Astrophysical Observatory, Azerbaijan National Academy of Sciences, Azerbaijan;
⁽⁴⁾ Tbilisi State Medical University, Georgia.

The operation of biological systems at all levels of organization has periodic oscillatory character. An origin and nature of fluctuations in biological systems are various. In many cases rhythmic processes presents reflection of auto oscillations in physical systems. According to modern understanding the variations of natural magnetic fields are main biotrophic synchronizers. Therefore understanding of a role and importance of rhythms in vital processes allows expecting every possible infringement in organism, to discover their mechanisms and to develop effective means for the prevention and correction of these infringements.

The complex research of rhythmic variations on the Sun, in space and on the Earth will allow us to study spatial-temporary organization of different systems.

Geo-effective heliophysical variations and human physiological state

Dimitrova Svetla
Solar Terrestrial Influences Laboratory - Bulgarian Academy of Sciences E-MAIL:svetla_stil@abv.bg

A group of 86 volunteers was examined on each working day in autumn 2001 and in spring 2002. These periods were chosen because of maximal expected geomagnetic activity. There were 26 persons in the group on a drug treatment, mainly because of hypertension. Systolic and diastolic blood pressure and heart rate were registered. Pulse pressure was calculated. Data about subjective psycho-physiological complaints of the persons examined were also gathered. Altogether 2799 recordings were obtained and analysed. MANOVA was employed to check the significance of the influence of three factors on the physiological parameters under consideration. The factors were as follows: geomagnetic activity estimated by H-component of the local geomagnetic field and divided into five levels, gender – males and females, presence of medication. Post hoc analysis was performed to elicit the significance of differences in the factors’ levels. The average arterial blood pressure, pulse pressure and the percentage of the persons in the group with subjective psycho-physiological complaints were found to increase significantly with the increase of geomagnetic activity. The maximal increment of systolic and diastolic blood pressure is 10-11% and for pulse pressure 13.6%. Analyses revealed that females and persons on a medication are more sensitive to the increase of geomagnetic activity than respectively males and persons with no medication.

Investigation of radiation dose distributions in a human phantom onboard ISS for estimation of the radiation risk to crewmembers in space flights

Radiation exposure of crewmembers on manned space flight has been recognised as an important factor in the planning and design of such missions. Indeed, the effects of ionising radiation on crew health, performance and life expectancy are a limitation to the duration of man's sojourn in space. Predicting the effects of radiation on humans during a long-term space mission requires: i) accurate knowledge and modeling of the space radiation environment, ii) calculation of primary and secondary particle transport through shielding materials and though the human body, and iii) assessment of the biological effect of cosmic particles, especially HZE particles.

The International Space Station (ISS) internal radiation environment is complex, with incident external space radiation field modulated by widely varying amounts of shielding and internal material, including the astronaut's bodies. Depth-dose curves in space flight are known to be a result of GCR and trapped radiation contribution. At some periods SCR are the most essential component of space radiation. For the estimation of the organ doses, and thus the radiation risk, measurements in human phantoms are essential.

Described is the method and dosimetric telescope Liulin-5 developed for investigation of the radiation environment dynamics within the Russian spherical tissue-equivalent phantom on ISS. Liulin-5 experiment will be a part of the international project MATROSHKA-R on ISS. The MATROSHKA-R project, launched in 2004, is aimed to study the radiation doses distribution at the sites of critical organs of the human body, using models of human body-anthropomorphic and spherical tissue-equivalent phantoms. The aim of Liulin-5 experiment is long term investigation of the depth - dose distribution inside the spherical tissue-equivalent phantom, mounted in different places of the Russian Segment of ISS. Liulin-5 is planned to be flown on the ISS in 2006 year.

Galactic cosmic rays modulation by two different heliospheric magnetic field patterns

Kobylinski Zbigniew
University of Podlasie, Dept. of Renewable Energies, Siedlce, Poland, present:: RIAAM, Maragha, Iran
E-MAIL:zbigniewkobylinski@yahoo.com

The steady state 3D transport equation of galactic cosmic rays (GCR) with drift included is numerically solved in two cases: the clasic Parker pattern of heliospheric magnetic filed and the Fisk's type of magnetic field in the spherically symmetric heliosphere bounded at the distance of 100 AU. In the calculations the parallel and perpendicular diffusion coefficients are proportional to 1/B, anti-symmetric element of the diffusion tensor has the form derived by Forman et al. under the ssumption of week-scattering. At high latitudes where Fisk field would be weak the isotropic diffusion is assumed, other regions of the heliosphere is filled up by Fisk field. We assume also that two circular coronal holes are localized near the poles with the central points that are offset from the rotation axis by the angle of 10 degrees. The computed distributions of cosmic ray density, gradients and modulated spectra are presented and compared with the results for Parker field. The calculated spectra are compared with experimental data (IMP8, LEAP, AMS and CAPRICE). The best fit can be obtained when the index of the power of rigidity in diffusion coefficient formula is less than 0.8. It is shown that the drift effects in the Fisk model should play an important role in GCP modulation, similar to the drift significance in Parker standard field and on the contrary to modifications of this model proposed by Jokipii and Kota and Smith and Bieber. Both these modification significantly reduce the dift effects.

Field-aligned current response to ICME on 11 April 1997 as seen by INTERBALL-Au satellite at mid-altitude cusp magnetosphere

We present magnetograms suggestive for unusual field-aligned currents (FACs) appearance in mid-altitude cusp of the magnetosphere at height 20000km. In fact FACs are different as compared with Potemra model nevertheless that current direction may coincide with the classical system. We demonstrate: (1) an appearance of two or more current sheets with opposite polarities in the dusk flank of the cusp; (2) appearance of FAC system in a comparatively large magnetic field depletion or diamagnetic cavity. The examination of energetic particles gives evidence to suppose a simultaneous formation of another event БЂ"cusp energetic particle (CEP) in the region of FACs field-aligned currents and diamagnetic cavity. As far as we know cases like the present one giving a relationship of diamagnetic cavity and FACs were not reported till now in the framework of INTERBALL mission. The obtained results might be useful in solving the fundamental problem - the origin of accelerated particles in the upstream of the magnetosphere.

Vostok and Thule Polar Cap Index variations and Polar Cap Potential during Spring Equinox conditions

Ground based magnetometer measurements with close location to the North and South magnetic poles at Thule and Vostok stations respectively, provide so called Polar Cap Index (PCI) of geomagnetic activity, which represents the level of solar wind magnetosphere interaction processes over both polar caps. In this work we use data for the PCI taken from both stations and observed Polar Cap Potentials (PCP) from DMSP-F13 satellite to study relative correlation between PCI/PCP changes. We compare DMSP-F13 PCP data taken from the SSIES instrument onboard the satellite, which cover ±20 days close to spring equinox 1998 with corresponding ground based observations of PCI for the same period. Some asymmetries that we observe between North and South PCI/PCP correlation are discussed.

Solar Cycle 24 Forecasts

The forecasts of the solar cycle 24 activities using the neural network method were made. For the sunspot relative number, R, June 2006 as the next minimum epoch with a value around 18 and, December 2009 as the next maximum epoch with a value of around 145 were obtained. Using the Ohl’s method the predicted next R maximum is 138, not far from the previous forecast of 145. For the 2800 MHz solar radio flux, the next minimum epochs with an approximate value of 75, on May 2006, and the next maximum epoch with a value of about 195, on December 2009, were forecasted. The time phase of both minima and maxima agrees nicely which gives us hope in a good behaviour of our approach. The forecasts of the geomagnetic aa and Dst indices were also done with the same pre-processing (gaussian monthly smoothed mean) and the same neural net for the same forecast horizon. The aa forecast gives for late 2008 an absolute minimum value around 11 and the Dst forecast gives for mid 2008 a local maximum around –19. The opposite phase behaviour of the two indices is clearly maintained over the forecast interval.

THE SOLAR ROTATIONAL ACTIVITY VARIATIONS DURING THE 23th SOLAR CYCLE

The study of the solar activity variability has been of great interest since its discovery. On the one hand it is important for the understanding of the Sun as an active star and on the other hand – for the investigations of the solar-terrestrial connections.

The solar magnetic field reverses approximately every 22 years, and manifests the 11-year solar cycle, in which the Sun changes its activity from its maximum value to the minimum one. The activity variations, developed by the sun surface rotation in connection with the nonsymmetrical distribution of active regions over the solar disc appear in a shorter time scale. As it is well known, these variations have periods of about 27 days. The solar surface rotates with different velocity, depending on the latitude. The differential solar rotation period, observed from the Earth, varies from 26.75 days at the solar equator up to approximately 29 days at higher latitudes. However the observed periodicity is generally in a wider range: from 20 up to 36 days. This wider spread is a result of the combination of both active-region evolution and solar rotation.

A simple empirical solar activity model is proposed, which describes the obtained behaviour by harmonic oscillations with simultaneous amplitude and phase modulation.

The solar rotational periodicity is analyzed using wavelet. It is demonstrated, that the model describes well the separate episodes of the active region evolution. Both kinds of modulations are the consequence of activity region growth or decay and hence, they are a result of a variable pattern of spots and active regions on the solar surface.

      

PHOTOMETRIC AND SPECTROMETRIC INVESTIGATIONS OF THE SOLAR CORONA AND ATMOSPHERIC EFFECTS DURING THE MARCH 29, 2006 TOTAL SOLAR ECLIPSE

A great part of the information about large-scale structure of the solar corona comes from solar observations during total solar eclipses. Тhe space coronagraphs overoccult the sun, omitting from view exactly the inner and coronal reasons well imaged at total solar eclipses. The total eclipse of the Sun on 2006 March 29, will be visible from within a narrow corridor, which transverse half the Earth. We foresee observations from the territory of Turkey. The aims of observations are:• Photometric investigation of the White corona structure and polarization.• Investigation of the structure of monochromatic emission corona in green (Fe XIV, 5303A) and red (Fe X, 6374A) line, Halfa, and the thermal corona in the 2 - 5 micrometers region of the Infrared spectrum

• • Investigation of the change in stratospheric O3 and NO2 content.
• • Determining of the dynamics of basic microclimatic parameters of the 10 m ground atmospheric layer.

The following methods will be used: Taking of photograph of the corona (telescope-refractor 100/1000mm, spectrozonal photoemulsions, polarization and infrared barrier filters), registration of the investigated emissions (telescope-refractor 150/1600mm, high sensitive photo-emulsions, narrow band filters), methods of the Differential Optical Absorption Spectroscopy, measuring of the microclimatic parameters with automatic meteorological statio processing and analysis of the photographs and data, seeking for wave structures in the O3 и NO2 concentration, comparison with other measurements during an eclipse.

The results we expect are: Determining of the Solar corona characteristics, finding of regularities in the O3 and NO2 behaviour in conditions of reduced solar radiation, and clarifying the dynamical and photochemical processes in the stratosphere and climate of the ground atmosphere.

Ionospheric data assimilation for modelling thermospheric-ionospheric storms

The disturbances of the upper atmosphere and plasma densities induced by geomagnetic storms are simulated using theoretical data assimilative model (TDAMI). Data assimilation procedure is used to adjust the values of vertical plasma drift (W) and N2/O ratio to the real measurement of foF2 and hmF2 in a meridional chain of VI stations. The derived correction coefficients for W and concentrations of neutral constituents (O, N2 and O2) are used to calculate spatial/time response of thermosphere and ionosphere on geomagnetic storms. Comparison with DE-B N2/O ratio data for 3 geomagnetic storms in September 1983 shows relatively good quantitative agreement. The model's simulations of maximum electron density (Nm) are compared with real plasma distribution created from all available Northern Hemispheric VI measurements of foF2 ionospheric parameter. The relative errors of the model vary in the range ±15% during the most hours of the disturbed period. In the hours of maximum ionospheric disturbances, TDAMI model gains improvement more than 70-80% compared to climatological ionospheric models.

The effect of solar activity on the drag perturbations of artificial satellite orbits

The results of the analysis of atmospheric drag various artificial satellites during the increased solar activity are submitted.

Three intervals are considered: October-December 2003, June and November 2004.

The correlation analysis of a degree of satellite drag and such factors as a flow of solar radiation on 10.7, flow of protons 1 MeV, area of active areas etc is carried out.

The aerodynamic drag is most effective in perigee of satellite orbit. It allows to estimate reaction of Earth atmosphere at different latitudes, as many objects are considered.

STUDY OF ATMOSPHERIC TRACE GAS AMOUNTS AT THE STARA ZAGORA GROUND BASED STATION

Since the end of August 1999 twilight daily measurements of scattered zenith sky radiation for determination of trace gas amounts deploying GASCOD instrument are carried out at Stara Zagora. The instrument was developed at the Institute of Atmospheric Science and Climate, Bologna. Reference spectra are obtained at midday. The instrument, appearing UV-VIS spectrometer, registers the zenith sky spectra automatically and 410 nm to 460 nm spectral interval is used to retrieve NO₂ and O₃ slant column amounts (SCA) by application of the DOAS methodology. The spectral analysis uses minimum least squares fitting of the cross sections at the expected absorbers to logarithm of the twilight spectrum and a reference spectrum.

The accumulated time series show the well-known typical seasonal variations, caused by the solar insulation. The residual time series of the removed semi-annual seasonal cycles from the measured original series show many different variations, with short periods up to inter annual variations. Single spikes of SCA are detected and we consider them as a result of overpassing weather fronts and/or lightening. Variations of SCA with time scale up to about 10 days are the consequence of weather cyclones. Some short-term variations of NO₂ and O₃ SCA are a result of intensive stratospheric-tropospheric exchange. Other residual time series periods are caused by Rossby waves, by overpassing of the polar vortex filaments. The inter-annual variations may be affected by QBO and NAO. Applying wavelet analysis of the obtained NO₂ slant column amount data series, and the total O₃ amount obtained by the GOME instrument, during the 23-rd solar cycle maximum, it is found time intervals with periods of 27 days on the time scale. Applied cross-correlation analysis demonstrated a phase lag of some days of the NO₂ and O₃ response to the 27-days solar cycle.

Calculated vertical column amounts of NO₂ are used for validation of satellite measurements e.g. SCIAMACHY NO₂ data.

      

O₂ Absorption Measurements and Modeling. Connection to the Troposphere Temperature

Ground-based measurements of the A(0,0) and b(1,0) bands of the O₂ atmospheric system are carried out using a spectrometric system designed for direct solar spectrum measurements in the region 3000 – 8000 Å, with a spectral resolution of about 0.3 Å.

Theoretical modeling of the O₂ absorption is performed presuming plane-parallel atmosphere, divided into equal homogeneous parallel layers, and applying line-by-line calculations. The A and b bands intensities are computed at different altitudes and zenith angles. The comparison of the modelled spectra to the detailed measured ones shows that the absorption calculation method is reliable.

The ground-based spectrometric measurements afford opportunities to obtain information for the atmospheric parameters, including the temperature and its change with the height. Up to now methods for temperature profile retrieval using ground-based measurements have not been developed. The creation of such a method would be a contribution to the atmospheric studies because of the importance of the temperature, and the cheaper implementation of the needed measurements as well. The temperature profile can be retrieved resolving the non-linear system equations for the equivalent widths of the rotational O₂ lines. Such system equations for the equivalent widths are obtained in both cases - of weak and strong absorption, are linearized and the systems are resolved towards the temperature in the separate layers, using an iteration method. The solution stability is studied with respect to the deviation of the input initial temperature values from the real ones, as well as with respect to the error in determining the equivalent widths. The system equations are found to be ill-conditioned, and the solution is highly sensitive to the input data. In order to provide the solution stability and a better convergence, a regularization algorithm has to be applied. The application limits of the weak and strong absorption equations are studied.

      

The challenge of the fluorescence imaging to the remote sensing of the vegetation ecosystems

The vegetation ecosystems are of the most significant components of the terrestrial biosphere and their disbalance can leads up to catastrophic consequences for the humanity. Nowadays the remote sensing of specific vegetation signature by space-born instruments, based on the spectral reflectance, is the only technique allowing large scale (regional or global), repeated observations. However, they provide information mainly related to the total quantity of vegetation and the concentration of its constituents. The efforts to answer the requirements for fast and reliable environmental control leaded to defining new criteria for estimation of the vegetation vitality, based on the imaging of plant fluorescence. Numerous investigations of the inverse relation between fluorescence intensity and photosynthesis activity (Kautsky effect) have been carried out in laboratory conditions. They proved the possibility the fluorescence signal to be successfully used for estimation of the plant biostatus. But the transfer of this experience in the area of remote sensing requires new investigations oriented to the registering of Sun excited fluorescence in natural conditions. The great challenge is how the high informative, but week fluorescence signal to be separated from the daylight and to be measured. In this relation, the scientific activity of a research group in STIL – BAS is focused on study of the influence of various natural factors on the fluorescence intensity using special bio chamber, designed by the researcher’s team. A conception for developing of system for simultaneous spectral and fluorescence imaging for ground-based monitoring of the vegetation vitality is created.

“USER FRIENDLY” SATELLITE DATA BASE SYSTEM OPERATING WITH MULTIPLE SOURCES OF DATA

Multipurpose Satellite Database System (MSDS) had been created under DEMETER (Detection of Electro-Magnetic Emissions Transmited from Earthquake Regions) microsatellite project. Various kinds of input search parameters from internal and external data sets can be used in a statistical basis over the whole amount of DEMETER data. Few examples of the output graphics opportunities are given to illustrate the usability of the MSDS by means of DMSP-F15 data.

The project of complex research of influence on an ionosphere helio- and geophysical factors in Vranch region

Aspects of simultaneous using of a radio-astronomical method of ionosphere sounding and other methods of ionosphere monitoring ( Doppler spectrum measurement of radio stations signals, GPS-monitoring) are considered. On the basis of these methods we are developing the program of complex researches of ionosphere response to various kinds of the influences which generate by helio- and geoactivity.

For realization of these researches, Vranch region (Romania) is chosen. This unique zone contains a local seismic source. The adjoining territory has low seismic activity. Such contrast facilitates detection of seismic effects in an ionosphere. The disposition of Vranch zone is convenient for execution of remote researches with participation of the Black Sea region countries

ON THE POSSIBILITY FOR EARTHQUAKE RESEARCH AND PREDICTION NETWORK IN BALKAN- BLACK SEA REGION

The prediction of the local time "when" an earthquake would happened is based on the connection between geomagnetic "quakes" and the next incoming minimum or maximum of tidal gravitational potential. The probability time window for the predicted earthquake is +/-1 day for the minimum and +/-2 days for the maximum. The preliminary statistic estimation on the basis of distribution of the time difference between predicted and occurred earthquakes for a 5 year period for Sofia region is given.

The possibility for local "when, where" Earthquake prediction is based on the accurate, with special space and time scales, monitoring of the electromagnetic field under, on and over Earth surface. The periodically upgraded information from Seismic hazard maps is essential.

Base platform of micro-satellite for the monitoring of potentially dangerous and catastrophic phenomena

Now in IKI RAS the development of micro-satellite "Chibis" for the monitoring of potentially dangerous and catastrophic phenomena in atmosphere and ionosphere and on Earth’s surface is carried out. Micro-satellite "Chibis" may be launched to orbit as the payload of "Progress" spaceship or by launch of conversion rockets to near-polar orbits.

Set of scientific instruments should be installed on micro-satellite "Chibis", including:

· TV-camera of optical region.

· Spectrometer for the measurement of &#105 &#105 2 total content.

· Low frequency flux-gate magnetometer.

· High frequency flux-gate magnetometer.

· Analyzer of electromagnetic radiation.

· Detector of ionosphere plasma.

It is supposed that on this satellite flight testing of modern scientific equipment, several observational methods and new service systems should be performed.

Main characteristics of micro satellite "Chibis"

Mass of scientific equipment Height of circular orbit Active life duration Orientation system: Type Accuracy of attitude determination Accuracy of pointing Data transmission system Spacecraft-Earth Memory size of &#105 &#105 Information, received from spacecraft Power consumption 40 kg12,5 kg~ 480 km Not less than 1 year Electromechanical, Magnetodynamic, Gravitational. Up to 2 arc minutes+ 3-15 arc minutes128 kbit/s8 Mbytes~ 50 Mbytes /day~ 50 W (all time)

It is planned to carry out flight control and data receiving, including images and spectra, in IKI RAS space communication station located in Tarusa, Kaluga region.

Methods of space monitoring of Sun-Earth connections with the use of micro-satellite platform.

Space monitoring offers great possibilities for the detection and estimations of potentially dangerous and catastrophic phenomena on the Earth's surface, in the atmosphere, traced to the ionosphere and to the magnetosphere. On the basis of tasks named above the model composition of the useful scientific payload of the `Chibis` micro-satellite is determined in the Space Research Institute of RAS

Research program for the`Chibis` micro-satellite is include:

A.Monitoring the atmosphere: the control of distribution and trends of greenhouse gases (CO2), the detection of the large ejections of dangerous substances into the atmosphere. Circulation of CO2 and of carbon generally in the atmosphere, the ocean and the biosphere to the high degree is controlled by natural factors and another activity of humanity.

B. Monitoring of the forest fires, other dangerous phenomena and objects on the Earth.

The use of micro-satellite with the contemporary onboard equipment will make it possible to create regional warning system with high technical characteristics

C. Space weather: observation of the state of the ionosphere, the radiation belts, solar wind.

It is at present widely acknowledged that studies in physics of sun-earth not only give important fundamental results, but also on the reliability of operation of modern technical systems and on the biosphere (including humans).

For the reception of these data the user can establish the compact Centre reception of micro-satellite telemetry data in itself. First of all it is necessary that this information operationally would enter to the State organizations and to person, who make decisions.

At present between IKI RAS and IKI BAS is signed Protocol about the intentions of the creation of micro-satellite "BalkanSat` for the space monitoring of potentially dangerous and catastrophic phenomena. IKI BAS conducts now the negotiations with the scientists of the Balkan countries about the formation of scientific program.

INVESTIGATION OF THE SOLAR DIFFERENTIAL ROTATION BY MEANS OF LONG-LIVED FEATURES OF THE SOLAR MAGNETIC FIELD

The differential rotation of large-scale magnetic features by using the Solar Synoptic Charts during 1965-1976 years is investigated. The variations of rotation rate of the large-scale formations of the Sun both in northern and southern hemispheres, in various latitudinal intervals are revealed. The large rotation rate of magnetic formations is received for patterns having the same sign, as sign of a global magnetic field. The change of rotation rate of researched magnetic features on all latitudinal intervals coincides with sign reversal of the global magnetic field.

CORONAL MASS EJECTION OF 28 JUN 2000: COUPLING OF THE CME EVOLUTION AND THE FLARE ENERGY RELEASE

We study the initiation and development of the limb coronal mass ejection (CME) of 28 Jun 2000, utilizing observations from Mauna Loa Solar Observatory (MLSO), the Solar and Heliospheric Observatory (SOHO), the Geostationary Operational Environmental Satellite (GOES) and Yohkoh. Also, we analyze the relation between dynamics of the CME and the energy release in the associated flare.

A complicate stucture (prominence and bright overlying arcades) is clearly recognizable in the low corona during the pre-eruption phase of slow rise. This provided measurements of kinematics of verious features from the very beginning of the eruption up to the post-acceleration phase which was followed up to 32 solar radii. Such events are observed only occasionaly, and are of great importance for the comprehension of the nature of forces driving CMEs. The acceleration maximum was attained at the radial distance of 1,3R_Sun from the Sun's center and ceased beyond 4 solar radii.

Observations provide clear evidence that CME eruption is causing a global restructuration of the magnetic field in the outer and inner corona. Furthermore, kinematics and morphological properties of this CMEs show possibility that various features of CME have diferent driver.

STRUCTURE AND PHYSICAL PARAMETERS OF THE CORONA SUBSTANCE DURING THE AUGUST 11, 1999 TOTAL SOLAR ECLIPSE

The solar corona images in white light are obtained by a large-aperture camera (200/1000 mm) and telescope – refractor, using black and white professional photographic film. Intensities of the red and green coronal lines are measured by specially constructed astrographs with 63 mm aperture of the objective and 840 mm focal length. Interference filters ( 6350A and 5350 A) were placed just before the main focal points.

The structure of the solar corona has been investigated within the three previously determined boundaries (in solar radii R): inner – up to 1.3R, middle – 1.3 - 2.3 R, and outer – 2.3R. The electron concentration of the coronal substance at distances up to 3 solar radii has been determined using the photographic observational data. Variations of the electron concentration depending on the distance to the Sun and the electron temperature have been investigated. The coronal ions’ kinetic temperature at different heliographic latitudes has been determined by the radial gradient of the electron concentration.

The solar corona brightness distribution is obtained as a function of the heliographic latitude and longitude as well as the distance to the solar limb.

The solar corona integrated brightness has been determined in the polar and equatorial regions.

Different structures of the solar corona in the region of forbidden line emission of the multiply ionized iron atoms - Fe XIV and Fe X – have been determined. The ratio of green and red line intensities necessary for determining the temperature of the inner corona has been calculated.

DERIVATION OF HELIOPHYSICAL SCIENTIFIC DATA FROM AMATEUR OBSERVATIONS OF SOLAR ECLIPSES

The appearance and evolution of rare astronomical phenomena such as total solar eclipses have an exceptional effect on amateur astronomy development. T he basic scientific aims and observational experiments included in a complex observational programme "Total solar eclipse’99" are described in the work. Results from teaching of TSE observation in the Public Astronomical Observatory in Stara Zagora and their selection for participation in different observational teams are also discussed. During the final stage of training a special system of methods for investigation of the level of pretensions (the level of ambition as to what he/she feels capable of achieving in the context of problem solving/observation) of the students is applied.

Results obtained from the observational experiments are interpreted mainly in the following themes:
· Investigation of the structure of the white-light solar corona and evolution of separate coronal elements during the total phase of the eclips
· Photometry of the white-light solar corona and specific emission line
· Meteorological, actinometrical and optical atmospheric investigation
· Astrometry of the Moon during the phase evolution of the eclips
· Biological and behaviorist reactions of highly organized colonies (ants and bats) during the eclipse.

It is also shown that data processing, observational results and their interpretation, presentation and publishing in specialized and amateur editions is a peak in the independent creative activity of students and amateur astronomers. This enables students from the Astronomy schools at PAOP to develop creative skills, emotional – volitional personal qualities, orientation towards scientific work, observations and experiments, and build an effective scientific style of thinking.

Galactic and Anomalous Cosmic Rays and 11-Year Solar Modulation in Heliosphere

The proposed model generalizes the differential D(E) and integral D(>E) spectra of galactic (GCR) and anomalous (ACR) cosmic ray protons and heavier elements during the 11-year solar cycle. The model takes into account the CR modulation by the solar wind in the heliosphere. The measurements with the BESS spectrometer, IMAX experiment and IMP-8 spacecraft for galactic cosmic rays and SIS spectrometer for anomalous component are examined with numerical solutions of the model equations. We consider accelerated mechanisms and we analyze variations of the parameters during the solar activity for outer and Earth planets. The radial gradient G₀ of GCR is relatively small in the inner heliosphere. After a transition region between 10 and 20 AU, G₀ increases to a much larger value that remains constant between ~25 and 80 AU. This shows that the contribution of GCRs and ACRs to the ionization of the atmospheres of outer planets Uranus, Neptune and Pluto will be increased drastically. We discuss here the errors in the predictions of the model and we compute the limits on estimated model parameters.

Application of continuous wavelet analysis to comparative studies of geomagnetic records from Swider and network of stations during the period 1937-1967

Recently the whole data base of hourly means of the Kalinowski's geomagnetic observatory at Swider (geog. lat 52.12, geog. long. 21.35), Poland, has been transfered to electronic form by Kobylinski, Trebicka and Izdebska (2004). The station has been in operation since 1921 till 1967. This long series have approximately constant calibration. Measurements were performing by the same devices during the whole period. This observatory practically worked continuously also during the difficult period of the second world war as the exception in this part of Europe.

We use the daily sums of local k index derived from Swider records of H component in order to compare with planetary K-index and determine the stability and quality of the data in the period of their availability 1937-1967. We studied the variability of these data by means of correlative, regression and continuous wavelet analyses. We observe generally a good agreement between the data in long time scale and we discuss some short time differences between the data that have the local character.

The wavelet technique is useful for such purposes and give more information than other statistical analyses.

Self-consistent model of he system magnetosheath-magnetosphere

A new self-consistent numerical model of the system magnetosheath- magnetosphere was developed based on the "modular approach" of modeling the geospace system. This approach permits a freedom in modeling different regions, applying for each region the most appropriate to its physical nature or to the purposes of the specific consideration model approach. The self-consistency between the regions is usually ensured via the boundary conditions. In this case the magnetosheath is modeled in the frame of the 3D gasdynamic approah. The magnetoshere magnetifc field model is a generalization of existing data based Tsyganenko models, derived by numerical solution of the Chapman Ferraro problem at each time step of the whole problem solution. The bow shock wave as well as the magnetopause is derived self-consistently as a part of the solution. The model provides in particular the possibility for studying some peculiarities of the magnetosheath flow, caused by specific realistic 3D magnetopause geometry. The magnetosphere module provides a flexible straightforward tool for testing possible contributions of different local models and approaches (including combinations of data and physics based ones) of different magnetospheric processes. This may be very convenient in particular for its application to data interpretation procedures.

         

Global ionospheric potential as a part of the global atmospheric electric circuit

A new numerical model of the global ionospheric electric potential distribution is considered as a step towards a self-consistent description of the global circuit. The 2D spherical thin shell approach used In this model is obtained reducing the 3D approach of the electrodynamics problem, posed in coordinate system, aligned with the geomagnetic field and based on a realistic global conductivities distributions. The model comprises the global computational region, which includes both conjugate ionospheres as separate sub-domains. Field-aligned currents between magnetically conjugate points (with not necessarily equal potentials) are permitted. The special role of the equatorial ionosphere is obtained as a part of the global model. Consideration of different driving sources of the ionospheric potential distribution is possible. Some estimates are presented of the influences of the both polar regions field aligned current systems, ring currents, neutral winds. The attention is especially focused on the possible influence of the global thunderstorm activity regions and its possible relation to the Carnegie curve variation of the vertical electric field near the Earth’s surface with Universal time.

         

MAIN FEATURES OF ATMOSPHERIC QUASI-ELECTROSTATIC FIELDS DUE TO LIGHTNING DISCHARGE

The most important features of the strong quasi-electrostatic fields, generated in the region ionosphere-ground after a single lightning discharge, due to succeeding redistribution of capacitive spatial charges, are studied in this work. The investigation of these fields is of great importance, particularly since they are considered to be responsible for generation of red sprites over thunderstorms. As experiments show, these quasi-electrostatic fields can cause, more often than sprites, electron heating and conductivity modifications in the mesosphere and ionosphere as well. The temporal behavior and relaxation time of the quasi-electrostatic fields are studied. For this purpose an analytical model under assumption of curl-free electric field is proposed. Isotropic conductivity in the region of interest is assumed. Computations are made for the time-course of the quasi-electrostatic fields up to the lower ionosphere. The dynamics of spatial charges in this region, responsible for the quasi-electrostatic fields, is analyzed also. It is shown that considerable charge density at different tropospheric heights resists in a second time-scale. The quasi-electrostatic fields reach their maximum at a time close to the local relaxation time. Up to the ionosphere this maximum is of an order of V/m per 1 Coulomb of a charge transported by lightning. The field decreases immediately after reaching its maximum in the mesosphere. At stratospheric and tropospheric altitudes its maximum forms a plateau, which becomes wider at lower heights. The relaxation of the quasi-electrostatic field at altitudes above 40 km is essentially slower than the local relaxation time of an electrical charge.

SUBAURORAL ION DRIFT (SAID) VELOCITY BEHAVIOUR AS INFERRED FROM DYNAMICS EXPLORER-B AND INTERCOSMOS “BULGARIA-1300” DATA

Rapid westward subauroral ion motion in the nighttime auroral oval during geomagnetically disturbed conditions had been first reported by ion drift measurements carried out on "Cosmos–184" satellite. The observed narrow band ion drift velocity jets at evening magnetic local times on the equatorward boundary of the auroral oval often exceed few km/s drift speed. In the present paper we use ion drift velocity data from Dynamics Explorer-2 (DE-2) and Intercosmos "BULGARIA-1300" (ICB-1300) satellites. DE-2 was launched on August 3 1981 with an inclination of 90°, perigee of 300km and apogee 1000km. On board plasma diagnostics instrumentation had been addressed to study upper atmosphere dynamics as a manifestation of the ionosphere-magnetosphere interaction processes in the Earth's ionosphere. ICB-1300 was launched on August 7 1981 on a near circular orbit with an orbital inclination of 82° , initial apogee 906km and perigee 825km under the same scientific objectives with a similar scientific instrumentation. Both satellites were in active operation almost of two years period. Here, DE-2 Ion Drift Meter (IDM) and Retarding Potential Analyzer (RPA) data together with ICB-1300 Electric Field Experiment (IESP-1) and Spherical Ion Trap
(P-6) data are used. In the present work we examine subauroral ion drift (SAID) velocity behavior as inferred by ion drift data from both DE-2 and ICB-1300 satellites in respect to the geomagnetic activity at different magnetic local times (MLT). Relative changes in invariant latitude position of SAID jets vs. AE index show a larger equatorward shift of almost 9.8^o ILAT in a 2100-2200 MLT sector (AE=1000). Corresponding statistics for dusk MLT sector show a 3.4^oILAT equatorward shift of the SAID position and a 6.4 ^o for earlier morning MLT hours respectively.

Rocket Measurements of the Direct Solar Lyman-alpha Radiation Penetrating in the Atmosphere

The resonance transition 2P-2S of the atomic hydrogen (Lyman-alpha emission) is the strongest and most conspicuous feature in the solar EUV spectrum. Due to the favorable circumstance, that the Lyman-alpha wavelength (121.5 nm) coincides with a minimum of the O2 absorption spectrum, the direct Lyman-alpha radiation penetrates well in the mesosphere. The interaction of the Lyman-alpha with the atmospheric constituents produces the NO molecules ionization, thus generating the ionospheric D-layer, and the water vapour photolysis, being one of the main H2O loss processes. The Lyman-alpha radiation transfer depends on the resonance scattering from the hydrogen atoms in the atmosphere and on the O2 absorption. Since the Lyman-alpha extinction in the atmosphere is a measure for the column density of the oxygen molecules, the atmospheric temperature profile can be calculated thereof.

Rocket measurements of the direct Lyman-alpha radiation vertical profile in the summer mesosphere and thermosphere (up to 120 km), at high latitudes, will be carried out in June 2006. The Lyman-alpha flux will be registered by a detector of solar Lyman-alpha radiation, manufactured in the Stara Zagora Department of the Solar-Terrestrial Influences Laboratory (STIL). Its basic part is an ionization camera, filled in with NO. The scientific data analysis will include raw data reduction, radiative transfer simulations, temperature retrieval as well as co-analysis with other parameters measured near the polar summer mesopause.

This project is a scientific cooperation between STIL-BAS, Stara Zagora Department and the Atmospheric Physics Group at the Department of Meteorology (MISU), Stockholm University, Sweden. The joint project is part from the rocket experiment HotPay I, in the ALOMAR eARI Project, EU’s 6th Framework Programme, Andoya Rocket Range, Andenes, Norway.

Influence of the solar activity on the total ozone content

A response of the atmosphere ozone to solar radiation variability has been studied using the total ozone content (TOC)data,taken from the satellite experiment GOME on ERS-2 and data from ground-based spectrophotometer "Foton"placed at the Stara Zagora (42⁰ 25’ N, 25⁰ 37’ E)station (Bulgaria)during 2000-2003. The sunspot daily numbers W and solar radio flux at 10.7 cm (F10.7) have been taken as parameters characterizing the solar activity.

The impact of the solar activity on TOC has been studied analyzing the ozone response to sharp changes of parameters W and F10.7. Some of examined cases showed a positive correlation between TOC and W and F10.7 (to an increase of W and F10.7 corresponded an increase of TOC) and negative correlation in other case was found.

Day-to- day variability in airglow and temperature by SATI-3 SZ data in Stara Zagora Station.

Day to day variations in the molecular oxygen nightglow emission rate and rotational temperature observed at the Stara Zagora site by the Spectral Airglow Temperature Imager (SATI-3 SZ) are discussed. Separate observations with wave like structures are presented.

Solar and space physics in Greece

I will report on the current status of solar and space physics research in Greece. Opportunities for the development of future collaborating with Balkan/Black Sea countries in the framework of the IHY 2007 will also be discussed.

         

Solar Physics in Belrade: Recent results and plans

Solar physics research in Belgrade carried out in frame of project Solar spectral irradiance variability at Astronomical Observatory and at Department of Astronomy of Faculty of Mathematics. Research program includes observations of the solar irradiance high-resolution spectra in several spectral regions. Recently an unusual high variation of the MnI 539.47 nm spectral line with solar activity has been recognized. A large part of our research in solar physics is oriented toward the understanding of the physical origin of this variability and their introduction in plasma diagnostic. This investigation will provide necessary information for construction of a solar irradiance spectrometer that could be used for solar activity monitoring. We plane to extend our research program by magnetohydrodynamic investigation of solar phenomena.

Regional Network for the Space Weather research

Space-based systems provide critical infrastructure that support the quality of life on Earth. Because of humanity’s increasing dependence on space-based systems, spacecraft that can survive and operate through all space environment conditions are required. It is not possible to achieve cost-effective, "all weather" space systems without accurate knowledge of the Space Weather. Space Storms lead to loss of data, degradation of capability, service outages, and, in extreme cases, the loss of satellite.

Aragats Space Environmental Center monitors:

• Measure as much as possible secondary CR fluxes with different energy thresholds;
• Monitor not only changing count rates, but also correlations between changing CR fluxes;
• Measure directional information;
• Use same detectors for both SW and high energy CR studies;
• Perform simulation of the time-series registered by the ASEC monitors;
• Correlate surface and space-born detectors data assessable from the Internert;
• Be part of world-wide networks;
• Provide forecasting and alerts on severe conditions of the Space Weather;
• Design and fabricate particle monitors detecting various species of cosmic rays.

• Most of technical progress in 21 century will come from Space Operations;
• New Space vision has Space Weather research and forecasting as a vital element for Space Operations;
• Information from networks of surface based detectors measuring secondary cosmic rays are compatible to data from space-born particle detectors and can be used for the reliable and timely SW forecasting;
• Developing countries should be a part of such networks to participate in the exploration of the Solar System and Universe;
• Necessary equipment is rather cheap and can be installed in scientific and educational institutions, schools, to make Space Research and Physics interesting and important for new generations.

The Space Weather detectors of new generation now under construction in CRD can serve as a good basis for the implementation of the regional scientific and forecasting network including Armenia, Georgia, Azerbaidjan, Iran, Turkey, Emirates, Dubaj and other countries. Installation and networking expenses will not exceed $50,000 and will permit the developing countries produce data vitally necessary for the space operations, those making links to the science and technology of 21^st century.

SPACE WEATHER INFLUENCE ON TECHNOLOGICAL, BIOLOGICAL AND ECOLOGICAL SYSTEMS: SOME MAJOR RESULTS OF COMPLEX INVESTIGATIONS CONDUCTED IN AZERBAIJAN

Solar energetic events and geomagnetic storms play a significant role in the Space Weather phenomenon which, in turn, is one of the important components of the Solar-Terrestrial Physics. Space Weather is determined by the most varied interactions between the Sun and interplanetary space, and the Earth. Space weather changes can negatively affect not only technological, but also biological systems, including human life and health. Our increasingly technology-dependent world is getting more sensitive to solar and geomagnetic activity, to changes in these activities and their manifestations on the Earth. For getting more and better knowledge about solar and geomagnetic storms’ potential effects on the above-mentioned systems, particularly in mid latitudes, we have initiated investigations on these problems within the Group on study of solar-terrestrial relations and space weather effects in the Azerbaijan National Academy of Sciences. These investigations cover monitoring, analysis and theoretical studies of space weather effects as well as application of obtained results. We are studying the possible influence of space weather factors in the following research areas: space weather influence on technical, engineering and ecological systems (scintillation of communication and navigation microwave radio signals, oil production activity, functioning of oil-gas transportation pipelines, electric power grids, climate, traffic accidents, beekeeping, etc.) and space weather effects on human life and health (virus-epidemic diseases, influenza, human brain functional state, cardiovascular diseases, ophthalmologic diseases, acupunctural indexes, thalassemia, etc.). Part of major and recently obtained results of these complex investigations on possible influence of periodical solar and geomagnetic activities, as well as non-periodic large solar energetic events on certain technological and ecological systems is provided in this paper which is based on the original research works. it is TRUNCATED

Stara Zagora ground-based station for atmosphere optical investigations (42.4N, 25.7E)

The ground-based station in Stara Zagora, Bulgaria has provided optical observation since 1969. In the last years the investigations are provided in collaboration among of grond-based stations situated at middle latitudes under the international projects.

In the paper are presented optical instruments in Stara Zagora ground-based station, their possibilities and research objectives.

Possible contribution of the Geospace Hydrodynamics Laboratory, Institute of Mechanics, BAS to the IHY activities

The efforts of the Geospace Hydrodynamics Laboratory, IMech, BAS, Sofia were recently concentrated on the developing of several physics based Geospace models with essential involvement of existing data based models and with introduced elements of data assimilation techniques.

A new self-consistent numerical model of the system magnetosheath – magnetosphere represents an attempt to return to the "modular–approach concept" in a qualitatively new level, providing quite powerful instrument for modeling these regions and data interpretation there on relatively low "computational cost".

A new global numerical model of the ionospheric electrodynamics is an attempt for a new approach for resolving the discrepancy between the spherical geometry of the ionosphere itself, and correspondingly, the global conductivity distributions from one side, and the natural to the electrodynamic problem magnetic field lines geometry from other side. The special role of the near-equatorial region arises as a logical consequence of this consideration. The model takes into account the interhemispheric interconnection, as well the influence of the neighboring regions: magnetosphere, including magnetopause and ring currents, atmospheric electricity.

A space-weather oriented techniques were developed for a near real time interpretation of the ACE (SWEPAM and MAG) plasma and magnetic field data in the L1 point, detection and identification of the strong discontinuities in the solar wind. An algorithm is a combination of a Rankin Hugoniot MHD analysis, minimum variance and wavelet.

We hope that the Laboratory will be able to contribute to some future international IHY projects, applying and developing further the ability of modeling and data interpretation.

         

PUBLIC ASTRONOMICAL OBSERVATORIES AND PLANETARIA – POSSIBILITIES OF OBSERVATIONS, EDUCATION AND PUBLIC OUTREACH

Principles of building the content and activity of the extra-curriculum Astronomy programme are presented in the work. In Bulgaria they are mainly in the system of Public Astronomical Observatories and Planetaria. Structure and activity of the specific educational forms there are united in schools, lectures, demonstrations, expeditions etc. Their influence on students is focused mainly on their knowledge and skills development, as well as on their motivation of learning and discovery in the field of astronomy and cosmic physics.

Publlic Astronomical Observatories and Planetaria have made a programme for the International Heliophysical Year planned for 2007. It includes:

• · Observation
• · Educational activities – What is IHY, IGY innovations and discoveries, IHY themes, organization and working group
• · Public outreach – presentations, show observations, films, discussions, media.

The role of amateur research observations of the photosphere (every day), solar corona (during total solar eclipses) and different manifestations of solar-terrestrial interactions is shown.A scheme of PAOP educational forms, by which the IHY programme will be realized is presented. Their didactical effectiveness is discussed in the conditions of permanent teaching on astronomy students, amateur astronomers and citizens with a great interest in contemporary achievements of astronomy and cosmic physics.

International Geophysical Year 1957/1958 - achievements and shortcomings

In the period of the International Geophysical Year an unprecedented in its scope monitoring was performed of many solar and geophysical processes. Evidences were identified for the effects on solar activity on geophysical processes which fostered the development of solar-terrestrial physics. The analysis of the achievements and shortcomings of the International Geophysical Year will be useful in will be useful in the planning of the forthcoming International Heliophysical Year.

Review of Solar-Terrestrial Connections Investigations in STIL-BAS

The Solar-Terrestrial Influences Laboratory carries out fundamental and applied research in the field of solar-terrestrial physics, in situ, and the remote investigation of geospace, planets and interplanetary space, optical atmosphere emissions and space biology. The scientific activities of STIL stay in a very close touch with the general BAS scientific priorities and with large national and international scientific programs and projects in the field of solar-terrestrial influences.

STIL-BAS contributes to the development of hardware and software products for scientific instrumentation on board rockets, satellites, planetary probes and manned space flights. Scientific teams participate in data and image processing and interpretation as well as in modelling of physical processes in solar-terrestrial influences.

Given is a short review of past, present and planned research in STIL-BAS aimed at creating methods and tools for investigation and forecasting space environmental conditions - space weather - that are hazardous to both space-borne and ground-based systems and human's everyday life, and assessment of the actual risk.

         

Caspian Sea and Black Sea Regions IHY Conference on Solar and Solar-Terrestrial Physics

Brief information will be given on the planned "Caspian Sea and Black Sea Regions IHY Conference on Solar and Solar-Terrestrial Physics" to be held in June 2007 in Azerbaijan under patronage of Azerbaijan National Academy of Sciences. Main coordinator will be the Shamakhy Astrophysical Observatory named after N.Tusi. There are preliminary agreements of several organizations as co-organizers of forthcoming Conference, such as the Institute of Physics of the Azerbaijan National Academy of Sciences, Georgian National Astrophysical Observatory named after academician Kharadze, Institute of Terrestrial Magnetism, the Ionosphere and Radio-wave Propagation named after Pushkov of the Russian Academy of Sciences, Solar-Terrestrial Influences Laboratory "Acad. D. Mishev" of the Bulgarian Academy of Sciences, etc. There are different ways under consideration for financing of the Conference including grant proposals, donations, helps of local authorities, etc.

Building of regional WEB site for the International Heliophysical Year

The key objectives are as follows:

• to serve as WEB interface for the regional center of the Balkan, Black Sea and Central European countries initiatives in the framework of the International Heliophysical Year;
• to maintain a data base of data, analyses and discussions
• to collect and provide information on available relevant and up-to-day WEB resources;
• to compile and disseminate information on research and educational activities in the field of International Heliophysical Year;
• to provide possibility for faster publishing of pilot results with the purpose to perform quick WEB-based discussions;
• to perform a synthesis of research results for the public;