Abstract Book for IHY workshop Bangalore India

In 1957 a program of international research, inspired by the International Polar Years of 1882-83 and 1932-33, was organized as the International Geophysical Year (IGY) to study global phenomena of the Earth and geospace. The IGY involved about 60,000 scientists from 66 nations, working at thousands of stations, from pole to pole to obtain simultaneous, global observations on Earth and in space. There had never been anything like it before. On the fiftieth anniversary of the International Geophysical Year an international program of scientific collaboration will be conducted called the International Heliophysical Year (IHY). Like it predecessors, the IHY will focus on fundamental global questions of Earth and space science.

The goals of the IHY are to:

1. Develop the basic science of heliophysics through cross-disciplinary studies of universal processes.

2. Determine the response of terrestrial and planetary magnetospheres and atmospheres to external drivers.

3. Promote research on the Sun-heliosphere system outward to the local interstellar medium - the new frontier.

4. Foster international scientific cooperation in the study of heliophysical phenomena now and in the future.

5. Preserve the history and legacy of the IGY on its 50th Anniversary.

6. Communicate unique IHY results to the scientific community and the general public.

The IHY will help us develop a deeper understanding of physical processes in the solar system through a program of comparative study of universal processes that affect the interplanetary and terrestrial environment. The study of energetic events in the solar system will pave the way for safe human space travel to the Moon and planets in the future, and it will serve to inspire the next generation of space physicists.

The United Nations Basic Space Science Initiative (UNBSSI): A Historical Introduction

H. J. Haubold*

*United Nations Office for Outer Space Affairs

Vienna International Centre

A 1400 Vienna, Austria

hans.haubold@unvienna.org

Pursuant to recommendations of the Third United Nations Conference on the Exploration and Peaceful Uses of Outer Space (UNISPACE III) and deliberations of the United Nations Committee on the Peaceful Uses of Outer Space (UNCOPUOS), annual UN/European Space Agency workshops on basic space science have been held around the world since 1991. These workshops contributed to the development of astrophysics and space science, particularly in developing nations. Following a process of prioritization, the workshops identified the following elements as particularly important for international cooperation in the field: (i) operation of astronomical telescope facilities implementing TRIPOD, (ii) virtual observatories, (iii) astrophysical data systems, (iv) con-current design capabilities for the development of international space missions, and (v) theoretical astrophysics such as applications of non-extensive statistical mechanics. Beginning in 2005, the workshops are focusing on preparations for the International Heliophysical Year 2007 (IHY2007). The workshops continue to facilitate the establishment of astronomical telescope facilities as pursued by Japan and the development of low-cost, ground-based, world-wide instrument arrays as led by the IHY secretariat.

Wamsteker, W., Albrecht, R. and Haubold, H.J.: Developing Basic Space Science World-Wide: A Decade of UN/ESA Workshops: Kluwer Academic Publishers, Dordrecht 2004.

http://ihy2007.org

http://www.unoosa.org/oosa/en/SAP/bss/ihy2007/index.html

http://www.cbpf.br/GrupPesq/StatisticalPhys/biblio.htm

IHY/UNBSS Program: Success Stories

N. Gopalswamy*, J. Davila, B. J. Thompson, and H. J. Haubold

*Solar System Exploration

Code 695, NASA-GSFC

Greenbelt, MD 20771, USA

gopals@ssedmail.gsfc.nasa.gov

The United Nations Office for Outer Space Affairs, through the IHY secretariat and the United Nations Basic Space Science Initiative (UNBSSI) is assisting scientists and engineers from all over the world in participating in the International Heliophysical Year (IHY) 2007. A major thrust of the IHY/UNBSSI program is to deploy arrays of small, inexpensive instruments such as magnetometers, radio telescopes, GPS receivers, etc. around the world to provide global measurements of ionospheric and heliospheric phenomena. The small instrument program is a partnership between instrument providers, and instrument hosts in developing countries. The lead scientist will provide the instruments (or fabrication plans for instruments) in the array; the host country will provide manpower, facilities, and operational support to obtain data with the instrument typically at a local university. Existing data bases and relevant software tools can be identified to promote space science activities in developing countries. Extensive data on space science have been accumulated by a number of space missions. Similarly, long-term data bases are available from ground based observations. These data can be utilized in ways different from originally intended for understanding the heliophysical processes. This paper provides an overview of the IHY/UNBSS program, its achievements and future plans.

International Living With a Star (ILWS) Program and IHY-2007

M. Guhathakurta*

*Earth-Sun System Division (DF)

Science Mission Directorate

NASA Headquarters

Washington DC 20546, USA

madhulika.guhathakurta@nasa.gov

Abstract yet to be received

IHY-2007: Coordinated Investigation Programs (CIPs)

B. J. Thompson*, et al.

*Code 671, NASA-GSFC

Greenbelt, MD 20771, USA

barbara.j.thompson@nasa.gov

The IHY has established a set of primary scientific objectives and goals. To accomplish these goals, a wide range of Coordinated Investigation Programs (CIPs) will transpire throughout the IHY timeframe, driving towards a more complete understanding of heliophysical universal processes. The CIPs are the basic "building block" of IHY science - they are proposed by members of the IHY community, and are approved and coordinated by the IHY discipline coordinators. The aim is that the program remains under the control of the proposer(s) with the IHY CIP process providing a means of publicising the proposed work, co-ordinating access to and use of the necessary resources, and a forum for discussing the results. There are currently over 50 CIPs in the IHY database, with many more being proposed.

Heliophysics in the United States of America

R. W. Smith*

*Geophysical Institute, UAF

903 Koyukuk Drive, P. O. Box 757 320

Fairbanks, AK 99775-7320, USA

roger.smith@gi.alaska.edu

jmc@gi.alaska.edu

The IHY program extends from the sun to the heliopause, or from the troposphere to the center of the sun, depending on your viewpoint. The US has cooperating observatories, CIPs and interested individuals willing to participate. On the other hand, there has been very little dedicated funding for the event even though NASA now claims a heliophysics program. Seen from the US viewpoint, this disappointment in funding is moderated by the fact that there are several existing programs that are well organized to collect data relevant to IHY needs. These include national programs such as CEDAR, GEM and SHINE as well as international coordinated groups such as CAWSES, eGY and IPY. Funding is adequate in each of these areas. Given that observational activity is funded and planned to happen, the most important remaining need is to communicate and demonstrate our original Universal Processes approach.

Our task is to show how the Universal Processes approach adds important synthesis to the scientific process in programs that are happening. Hence we need to be present at workshops organized by CAWSES, CEDAR, GEM and SHINE to make our message relevant and stimulate studies focused on Universal Processes.

Equally important is our emphasis on education and outreach. In the US we are planning special summer schools on IHY and special curriculum to be used in middle and high schools. We hope to produce a major documentary movie to air on television. In both outreach and in the arenas of professional science, our main aim is communication and demonstration of the new science of heliophysics.

Session 02: 14:00 – 16:00, Nov. 27, 2006

IHY Activities in India

P. K. Manoharan*

*Radio Astronomy Centre

Tata Institute of Fundamental Research

Udhagamandalam (Ooty) 643 001

Tamil Nadu, India

mano@ncra.tifr.res.in

This talk will review the plans and status of the available instrumentation and facilities for the India IHY program and discuss the collaborations with other countries. Some of the ongoing international collaborative researches related to the IHY program and their results will be highlighted.

IHY Activities in Africa: Current Status and Future Developments

A. B. Rabiu*, and E. E. Balogun

*Department of Physics

Federal University of Technology

Akure, Ondo State, Nigeria

tunderabiu@yahoo.com

The International Heliophysical Year (IHY) has already gained a global acceptance as international research cooperation. This paper assesses the current status of IHY; its organization, activities and challenges in Nigeria and THE African continent as a whole. The tremendous impact and successes of the program is highlighted. Two successful annual workshops have been held at different locations with wide national representation. A few facilities already installed or secured are presented for probable exploration and forging of partnership in research. On-going research involvement with SCINDA, AWESOME and MAGDAS are presented. With the passing of the dip equator through the country, Nigeria is presented as a region for ground observation and measurements of geo- and helio-physical variables. Ways by which Nigerian scientists are taking advantage of the opportunities embedded in the international program are exposed. Benefits of IHY including training, collaboration, workshop participation and publications, are explored.

IHY Activities in the Balkan - Black Sea - Caspian Sea Region

K. Georgieva*

*Solar Terrestrial Influences Laboratory

Bulgarian Academy of Sciences (STIL-BAS)

Bl3 Acad.G…Bonchev Street

Sofia 113, Bulgaria
kgeorg@bas.bg

katyagerogieva@msn.com

The regional network of the countries in the Balkan – Black sea – Caspian sea region for space weather studies was created in June 2005 with the goal to coordinate the participation of the countries in the program of the International Heliophysical Year and to promote in the future the collaboration between them in basic space sciences. This talk will summarize the activities of the network and will present the research projects which have been proposed.

IHY activities in West Asia: Research and Education in Astronomy and Space Sciences for Arab Countries

H. M. K. Al-Naimiy*

*College of Arts and Sciences

Sharjah University

P. O. Box 272 72, Sharjah, UAE

alnaimiy@sharjah.ac.ae

alnaimiy2@yahoo.com

Astronomy and Space Sciences (ASS) are important fields of research, study, knowledge and culture. They have been the cradle of both eastern and western sciences. We all know, from education and psychology, about the effective teaching and learning of ASS. Unfortunately, a small percentage of this knowledge is actually used in teaching at schools, universities level and any other academic institutions in the Arab countries. The challenge is to provide effective professional development for ASS educators and researchers at all levels, from elementary school to university.

ASS is the most appealing subject to young students and very important tool to convey scientific knowledge? Once students have understood the importance of science, they might be more easily pursued to continue their education in science and technology. The aim of this paper is to show the importance of the formal and informal ASS research, and education, giving an example of a possible curriculum, projects, and comments on the activities that have been carried out in a few Arab countries.

We feel the need for a new communication channel among the Arab people based on our common scientific ground. ASS is, in this respect, the best possible choice in the vast cultural heritage of the Arab basin.

The final purpose is scientific and economical. Building modern and good observatories, planetariums and research centers in the region jointly by Arab astronomers and space scientists is essential and will be an excellent step toward developing astronomy and astrophysics (for research, education and knowledge).

IHY Activities in South Africa

A. Hughes*

*School of Pure and Applied Physics

King George V Avenue

Durban 4001, South Africa

HUGHES@ukzn.ac.za

A brief overview of the organization of the South African Research Community and details of relevant on-going research in South Africa and Antarctica will be elaborated.

Session 03: 16:00 – 17:40, Nov. 27, 2006

Solar Magnetic Waves and Oscillations

R. Erdelyi* (von Fay-Siebenburgen)

*Solar Physics and Upper-Atmosphere Research Group (SPARG)

Department of Applied Mathematics

Univeristy of Sheffield, Hicks Building

Hounsfield Road, Sheffield S3 7RH, UK

robertus@sheffield.ac.uk

Recent solar and space satellite missions (e.g. SOHO, Trace) and high-resolution ground-based observations (e.g. Swedish Solar Telescope, Dutch Open Telescope) have opened new avenues for 21st century plasma physics. With unprecedented details a very rich and abundant structure of the solar atmosphere is unveiled. Revolutionary observations clearly confirmed the existence of MHD waves and oscillations in a wide range of solar atmospheric magnetic structures, commonly described in the form of solar flux tubes. The objectives of this review are to give an up-to-date account of the theory of MHD waves and oscillations in solar and astrophysical magnetic wave-guides. Since magnetic structuring acts as excellent wave guides, plasma waves and oscillations are able to propagate from sub-surface solar regions through the solar atmosphere deep into the interplanetary space. Observations and theoretical modeling of waves can provide excellent diagnostic tools about the state of solar plasma. Key examples of the various types of MHD waves and oscillations will be discussed both from observational and theoretical perspectives and the concept of atmospheric (coronal) and magneto-seismology will be introduced. The lecture will also contain a few short exercises in order to highlight the important points of the applications of solar MHD wave theory.

Measurement of Solar Diameter

K. R. Sivaraman*, S. S. Gupta, and A. V. Ananth

*Indian Institute of Astrophysics

Koramangala, Bangalore 560 034

Karnataka, India

siva@iiap.res.in

We have used the photographic images of the Kodaikanal observatory archives to measure the solar diameter. These images obtained with a 6-inch refractor form part of an ongoing programme of synoptic observations that commenced in 1914. The reduced diameter measures (annual means) completed for 4 half solar cycles show that the solar radius is anti correlated with the sunspot activity.

Signatures of Large Flares on Photospheric Magnetic and Velocity Fields

A. Ambastha*

*Udaipur Solar Observatory

Physical Research Laboratory

P. O. Box 198, Udaipur 313 001

Rajasthan, India

ambastha@prl.res.in

a_ambastha@rediffmail.com

We have studied spatial and temporal evolution of some flare productive active regions using high cadence photospheric magnetograms and Dopplergrams. In addition, chromospheric H-alpha filtergrams have been used to identify flux emergences, large proper motions and development of velocity flows in relation to the flare sites. Magnetic flux and velocity changes have been found at these sites before and after large flares. The 3-D power spectra of p-mode oscillations have been obtained using ring diagram technique. These spectra are then used to look for helioseismic response of the flares on the amplitude, frequency and width of the p-modes. In the flaring active region, p-mode power enhancement and a steep gradient in the meridional velocity are found as compared to the quiet regions. A comparison of flaring active regions has been carried out with less productive active regions.

Fine Scale Magnetic Fields in and Around a Decaying Active Region

K. Sankarasubramanian*, and M. Hagenaar

*Space Astronomy and Instrumentation Division

ISRO Satellite Center, Airport Road

Vimanapura Post, Bangalore 560 017

Karnataka, India

sankark@iisac.gov.in

A very high resolution spectro-polarimetric observation of a decaying spot was observed with the Diffraction Limited Spectro-Polarimeter (DLSP). The spatial resolution achieved in this observation is close to the diffraction limit (0.18arcsec) of the Dunn Solar Telescope operated by the National Solar Observatory at Sacramento Peak, Sunspot, New Mexico. The fine scales present inside the decaying active region as well as surrounding areas of the active region will be presented. There are two interesting phenomenon observed which will be described in detail. They are: (i) There are opposite polarity loops present all around the spot and some of them do connect the main spot and the surrounding magnetic features, (ii) Canopy like structures are likely to be present in the umbral dots as well as in the light bridges present providing evidence for field-free intrusion. The conclusion from the time variation of the intensity structures of this spot is that the spot is disrupted in to several fragments by the formation of light bridges and the fragmented magnetic fields later disappear under the visible photosphere.

Forecasting Cycle 24 with a Solar Dynamo Model

Jie Jiang, P. Chatterjee*, and A. R. Choudhuri

*Department of Physics

Indian Institute of Science

Bangalore 560 012

Karnataka, India

piyali@physics.iisc.ernet.in

A challenge before solar physicists right now is to forecast the strength of the next solar cycle (Cycle 24). Several contrary forecasts have already been made. Most of the forecasts are based on various precursor methods. Only one forecast is based on a dynamo model (Dikpati and Gilman 2006). Since we find some aspects of this work questionable, it is desirable to have another independent forecast based on a dynamo model. We are carrying out an analysis based on our dynamo model, using a methodology different from what was used by Dikpati and Gilman (2006). We shall present the methodology of our approach and, most probably, we shall also have some results by the time of the IHY meeting.

Session 04: 09:00 – 11:00, Nov. 28, 2006

Dynamics of the Magnetized Solar Chromosphere

S. S. Hasan*

*Indian Institute of Astrophysics

Koramangala, Bangalore 560 034

Karnataka, India

hasan@iiap.res.in

This review focuses on dynamics of the magnetized solar chromosphere. In the quiet chromosphere we distinguish between the magnetic network on the boundary of super-granulation cells, where strong magnetic fields are organized in mainly vertical magnetic flux tubes, and inter-network regions in the cell interior, where magnetic fields are weak and dynamically unimportant.

Observations have firmly established the presence of oscillations in the solar chromosphere. Both the network and inter-network media show bright points (BPs), which are prominent in the emission peaks in the cores of the Ca II H and K lines. However, the dynamical and spectral properties of network and inter-network BPs are quite different. In the latter the chromospheric velocity power spectrum is dominated by oscillations having power in the 5-7 mHz range, which can essentially be regarded as acoustic waves, whereas the network exhibits low-frequency oscillations with periods 7-20 min. The qualitative properties of inter-network BPs are reasonably well understood, including their formation in upward propagating acoustic shocks that encounter downward-flowing gas. On the other hand, the physical processes that heat the magnetic network have not been fully identified. Are network BPs heated by wave dissipation and if so, what is the nature of these waves? These and other aspects relating to the dynamics and energy transport mechanisms will be discussed in detail. Furthermore, a critical assessment will be made on the challenges facing theory and the direction for future investigations, particularly in the light of the new space experiments, will be highlighted.

Lessons from SUMMER/SOHO Solar Ultraviolet Spectrograph

K. Wilhelm*

*Max-Planck-Institut für Sonnensystemforschung(MPS)

37191 Katlenburg-Lindau

Germany

wilhelm@mps.mpg.de

Our understanding of the high-temperature solar atmosphere is to a large extent based on spectroscopic observations of emission lines and continuum radiation in the vacuum-ultraviolet (VUV) wavelength range of the electromagnetic spectrum. The VUV radiation is produced by transitions of atoms and ions, or to some extent, of molecules. The atomic and ionic emission lines have formation temperatures between 10,000 K and several million Kelvin, representative of the chromosphere, the transition region and the corona. The molecular lines and the continua originate in cooler regions of the Sun. Radiation at VUV wavelengths is strongly absorbed by the Earth's atmosphere and can only be detected with instruments on sounding rockets and spacecraft above the atmosphere. Detailed studies of the spectral radiances together with atomic physics data furnish information on the electron density and temperature of the solar atmosphere, as well as on elemental abundances, whereas Doppler line-shift measurements show bulk plasma motions, turbulence, and ion temperatures. Research in this field will be presented using measurements of the Solar Ultraviolet Measurements of Emitted Radiation (SUMER) instrument on the ESA/NASA Solar and Heliospheric Observatory (SOHO). In addition, the instrumental technique will be briefly introduced as well as the scientific use of the data obtained over a period of ten years.

Contribution of Solar Chromospheric Fine Scale Features to UV Irradiance Variability

R. Kariyappa*,, L. Damé, and W. K. Tobiska

*Indian Institute of Astrophysics

Koramangala, Bangalore 560 034

Karnataka, India

rkari@iiap.res.in

The Sun is the primary source of energy responsible for governing both the weather and climate of Earth. For that reason alone one would expect that changes in the amount and type of energy Earth received from the Sun could alter weather and climate on the Earth. The variations in the UV irradiance are produced by surface manifestation of solar magnetic activity. Considering the variations in the solar UV flux may cause significant changes in the Earth’s climate, understanding the physical origin of UV irradiance changes is an extremely important issue in Solar and Space Physics.

We have segregated the (i) plages, (ii) magnetic network, and (iii) intranetwork + the background regions from the Call K spectroheliograms of 1980 and 1992, observed at the National Solar Observatory at Sacramento Peak, using their histograms taken for the full-disk. The different parameters like the intensity and area of the chromospheric features, the full-disk intensity (spatial K index), and the full width at half maximum (FWHM) of the histograms have been derived from the images. The spatial K index, FWHM, and the intensity of various features have been compared to the UV irradiance measured in the Mgll h and k lines by the Nimbus7 and NOAA9 satellites and it has been found that they are correlated with the Mgll h and k c/w ratio. We established, for the first time, from the results of 1992 images and of 1980 that the FWHM can be used as a good index for measuring and describing the chromospheric activity in the K-line. The results of both 1980 and 1992 images show an anticorrelation between the intensity and area of the network elements, which confirm the earlier findings derived entirely from different data set from Kodaikanal Call K spectroheliograms analyzed for the center of the solar disc in a quiet regions for a longer time interval of 1951 to 1983 (Kariyappa and Sivaraman, 1994). During solar minimum the network is fainter but covers a larger area than during solar maximum. These results suggest that the variations in both the intensity and area of the various chromospheric features have to be taken into account in irradiance models.

Multi-Wavelength Study of Active Region Loop Dynamics

D. Banerjee*

*Indian Institute of Astrophysics

Koramangala, Bangalore 560 034

Karnataka, India

dipu@iiap.res.in

Observations have revealed the existence of weak transient disturbances in extended coronal loop systems. These propagating disturbances (PDs) originate from small scale brightenings at the footpoints of the loops and propagate upward along the loops. In all cases observed, the projected propagation speed is close to, but below the expected sound speed in the loops. This suggests that the PDs could be interpreted as slow mode MHD waves. Interpreting the oscillation in terms of different wave modes and/or plasma motions always depend on the line of sight as we observe in the limb or on the center of the disk. The JOP 165 campaign will address some of these questions. MDI and TRACE photospheric and UV imaging of TRACE and SPIRIT have been acquired simultaneously with high temporal and spatial coverage along with the spectroscopic data from CDS. EIT was operated in the shutter-less mode to achieve high Cadence. Some of the off-limb active region dynamics and oscillations observed during this JOP campaign will be focused in this presentation. Plasma condensations and temporal variations in active region loops will be also addressed.

Multi Application Solar Telescope (MAST): A Versatile Tool for Studying the Physics of Solar Eruptions

P. Venkatakrishnan*

*Udaipur Solar Observatory

Physical Research Laboratory

P. O. Box 198, Udaipur 313001

Rajasthan, India
paravenk@yahoo.com

pvk@prl.res.in

Contemporary solar research is progressing along several fronts. Solar magnetism and its role in powering solar eruptions is one basic theme. Quantitative evaluation of the different manifestations of the free energy available for eruption is one major task. This requires vector magnetograms of a large number of active regions monitored closely in time with high polarimetric accuracy. The second task is to obtain greater clarity about various triggering mechanisms for the eruptions. This requires observations of line-of-sight magnetic fields and velocity fields with high spatial resolution. Both tasks need mutually exclusive requirements leading to the concept of the multi application telescope. In this talk, I outline the various steps, like site characterization, optical design, adaptive optics development and schemes for back-end instrumentation that culminated in the present concept of MAST. I will emphasize the constraints posed by availability of and access to technology which played a significant role in deciding the concept. I conclude by highlighting certain unique features of MAST which can provide special insights into a few scientific problems.

Chromosphere and Transition Zone Dynamics and Heating: Need for Future Space Missions

L. Damé*

*Service d' Aéronomie du CNRS

BP 3, 91371 Verrières-le-Buisson

Cedex, France

luc.dame@aerov.jussieu.fr

SOHO and TRACE observations have clearly shown that even the very quietest part of the solar chromosphere is very structured and dynamic with brightenings and waves. Diagnostics from this region are very difficult because spectral lines are neither formed in LTE nor under optically thin conditions that prevail higher in the Transition Zone. The gas goes from being dominated by the gas pressure in the photosphere to being dominated by the magnetic pressure in the upper chromosphere, involving steep gradients to obtain significant dissipation or heating. The ionization balance of important elements is furthermore out of equilibrium. A proper understanding thus demands very high spatial resolution with accurate measurements of velocity and line width, uninterrupted in Space, across a broad range of temperature ("heights"), to distinguish between wave heating and reconnection events in the chromosphere and Transition Zone. Complex modeling, that ideally should include non-LTE radiative transfer in 3D including the dynamic driving in the convection zone, non-equilibrium ionization, magnetic fields, the transition region and the corona, will be necessary to understand these observations. We will discuss various aspects of this very complex problem and insist on ground measures and, above all, Future Space Missions which should better address Doppler information, temperature coverage and discrimination and, most important, very high spatial resolution to progress on the way to a fully comprehensive view of chromospheric and coronal heating.

Session 05: 11:20 – 13:00, Nov. 28, 2006

Observation of CME Source Regions by Coronal Emission-Line Dopplergrams

T. Sakurai*, K. Hori, I. Suzuki, and K. Ichimoto

*National Astronomical Observatory of Japan

Osawa, 2-21-1 Mitaka City

Tokyo 181 8588, Japan

sakurai@solar.mtk.nao.ac.jp

Although observations with SOHO/LASCO show the behavior of CMEs beyond 2.5 solar radii, connection between LASCO CMEs and their source regions in the lower corona observed with SOHO/EIT or Yohkoh/SXT is not trivial. One way to fill the gap would be to supplement the Doppler shift information of the moving CME mass. Such an instrument was built and has been operated since 1997 July at the Norikura Solar Observatory (2876 m above sea level) of NAOJ. The instrument we call NOGIS (NOrikura Green-line Imaging System) is made of a 10 cm-aperture coronagraph and a tunable birefringent filter. NOGIS can provide both intensity and Doppler velocity images of 2 MK plasmas using the coronal green-line emission at 5303 Angstrom of Fe XIV. An intensity image is made by subtracting the sky background (taken at far wings) from the line-center image. A Doppler image is constructed by subtracting a blue-wing image from a red-wing image. The line-of-sight velocity up to 25 km/s can be obtained with an accuracy of about 0.6 km/s. NOGIS covers a field of view of 1.03 - 1.33 solar radii in a full frame mode, or a local small area in a partial frame mode with higher cadence of about 1 minute. So far we have analyzed two CME events which showed favorable orientations of the regions against the plane of the sky (1999 May 7 and 2003 June 2). In both events, interaction between two magnetic flux systems (loops in the case of 1999 May 7 and arcades in the case of 2003 June 2) was observed.

Magnetic Nature of Coronal Loops

J. Singh*

*Indian Institute of Astrophysics

Koramangala, Bangalore 560 034

Karnataka, India

jsingh@iiap.res.in

It is generally believed that magnetic pressure is much higher than the gas pressure in the coronal loops and these loops are isothermal in nature. We have made systematic observations of all the 4 strong coronal emission lines in the visible and near infrared part of the spectrum for about 8 years. Two emission lines were chosen at a time to make the raster scans of steady coronal region. We have studied the variation of line widths of these lines and intensity ratios as a function of height. The relationship between the widths of these lines and intensity ratio indicates that the steady coronal loops are not magnetically isolated. These findings put restrictions on coronal loops models and indicate that magnetic pressure in coronal loops may be much less than assumed. These results strongly suggest that magnetic field in the corona need to be measured accurately.

GMRT and Solar Radio Observations

S. Ananthakrishnan*, P. Subramanian, and F. Madsen

*National Centre for Radio Astrophysics

Tata Institute of Fundamental Research

Pune University Campus, Post Bag 3

Ganeshkhind, Pune 411 007

Maharashtra, India

sudha.anan@gmail.com

ananth@ncra.tifr.res.in

We, briefly describe the Giant Metrewave Radio Telescope (GMRT) which is one of the most sensitive radio instruments in the world, operating in the frequency range 150-1450 MHz. Although it is a high resolution aperture synthesis array for observing compact and extended galactic and extra galactic sources, we show that it is a very useful instrument for observing the Sun in the above frequency range. We have used it for observing flares, noise storms and coronal holes. In particular, we describe the recent GMRT 150 MHz observations of a coronal hole with a dynamic range of >20 dB. A comparison of the radio map with a resolution of about a minute of arc with the EUV data from SOHO/EIT and the corresponding SXR data from GOES SXI instruments shows that the total extension of the coronal hole is similar and the systematic shift in the position of the mid-points of the maps allows us to make an estimate of the average distance/height between the three emission regions, by assuming the shifts to be due to simple projection effects.

Variations in the Global Solar Radio Flux During the Extreme Solar Eruptions of October – November 2003

K. R. Subramanian*

*Indian Institute of Astrophysics

Koramangala, Bangalore 560 034

Karnataka, India

subra@iiap.res.in

We study the variations of the global solar radio flux obtained at 15400, 8800, 4995, 2995, 2800, 1415, 610 and 245 MHz during the extreme solar eruptions of October – November 2003. By least square fitting of above frequencies and the corresponding observed radio fluxes, the value of the spectral indices were derived assuming the variation of the radio flux with frequency of the form S ~ f^α. The values of the spectral indices were less during periods of solar storms compared to quiet periods showing non-thermal contribution to the global radio flux. The value of the spectral index correlates negatively with the solar flare index.

Electron Acceleration in Solar Noise Storms

P. Subramanian*, et al.

*Indian Institute of Astrophysics

Koramangala, Bangalore 560 034

Karnataka, India

psubrama@iiap.res.in

We report high resolution, high dynamic range meter wavelength observations of noise storm sources in the solar corona. These observations were made by combining visibilities from the Giant Meterwave Radio Telescope (GMRT) in Pune, India, and the Nancay RadioHeliograph (NRH) in Nancay, France. These observations have the potential to place firm upper limits on the brightness temperature of noise storm sources. We have therefore carried out theoretical work on the energetics of non-thermal electron acceleration in noise storm sources. We have derived rigorous estimates for the overall efficiency of the overall noise storm emission process, beginning with non-thermal electron acceleration and culminating in the observed radiation.

Session 06: 14:00 – 15:40, Nov. 28, 2006

SOXS for IHY–2007 and Beyond

R. Jain*

*Physical Research Laboratory

Navrangpura, Ahmedabad 380 009
Gujarat, India
rajmal@prl.res.in

We present on the utilization of existing mission namely Solar X-ray Spectrometer (SOXS) for observing the full disk Sun in the X-ray waveband in 4-56 keV. SOXS has been functioning satisfactorily since June 2003 though for a limited period of 2-3 hours daily. SOXS mission has so far observed more than 400 flares of varying intensity and a few of them are found to be associated with CMEs. We present recent results from SOXS observations that combined with optical and radio wavebands, which reveal loop-loop interaction as potential mechanism for those flares occurred with remote brightening. We also present study of microflares observed by SOXS mission and found that microflares are potential candidates for coronal heating. SOXS mission is expected to continue during ascending phase of solar cycle 24.

Sun-Earth Connection Studies at KASI

Y.-J. Moon* et al.

*Korea Astronomy and Space Science Institute (KASI)

61-1, Whaam-Dong, Yuseong-Gu

Daejeon 305-348, South Korea

yjmoon@kasi.re.kr

We introduce our recent Sun-Earth connection studies which have been done in solar and space weather research group at KASI. In a series of papers, we have examined the physical characteristics of geoeffective halo CMEs that produced geomagnetic storms. First, we investigated the probability of geoeffective CMEs depending on its solar surface location and speed using SOHO/LASCO CMEs from 1997 to 2003. Second, we examined the relationship between several CME physical parameters (e.g., earthward direction, density, mass, location) and geomagnetic storms for very fast halo CMEs (VCME > 1300 km/s). In particular, we suggested a new earthward direction parameter that is defined as a ratio, the shorter front from the solar center to the longer one. Third, we examined the relationship between the field orientation in a CME source region and a geomagnetic storm using a coronal flux rope model as well as its dependence on ICME classification (magnetic cloud or ejecta). Major results are as follows. 1) The most probable areas whose geoeffectiveness fraction is larger than the mean probability (0.4), are 0<L<30 for slower speed CMEs (<800km/s), and 30<L<60 for faster CMEs (>800 km/s). 2) The CME direction has much better correlations with the Dst index than other parameters for very fast halo CMEs. 3) The relationship between the field orientation and the geomagnetic storm for magnetic cloud is much better than that for ejecta, implying that the field orientation of the magnetic clouds is well conserved through the heliosphere. We also briefly introduce several ongoing studies: (1) earthward direction as an important geoeffective parameter, (2) solar wind effect on the propagation of IP shocks, and (3) satellite drag effect during strong solar/geomagnetic activities and the comparison between the drag derived density and the MSIS-90 model. Finally, we present some future plans in the Sun-Earth connection field.

Propagation and Dissipation of MHD Waves in Coronal Holes

B. N. Dwivedi*

*Department of Applied Physics

Institute of Technology

Banaras Hindu University

Varanasi 221005, Uttar Pradesh, India

bholadwivedi@yahoo.com

bholadwivedi@gmail.com

In view of the landmark result on the solar wind outflow, starting between 5 Mm and 20 Mm above the photosphere in magnetic funnels, we investigate the propagation and dissipation of MHD waves in coronal holes. We underline the importance of Alfvén wave dissipation in the magnetic funnels through the viscous and resistive plasma. Our results show that Alfvén waves are one of the primary energy sources in the innermost part of coronal holes where the solar wind outflow starts. We also consider compressive viscosity and thermal conductivity to study the propagation and dissipation of long period slow longitudinal MHD waves in polar coronal holes. We discuss their likely role in the line profile narrowing, and in the energy budget for coronal holes and the solar wind. We compare the contribution of longitudinal MHD waves with high frequency Alfvén waves.

Observational Clues to the Origin of the Fast Solar Wind

M. D. Popescu*, J. G. Doyle, and D. Banerjee

*Armagh Observatory

College Hill BT61 9DG

Armagh, Northern Ireland, UK

mdp@arm.ac.uk

It is well known that the fast solar wind originates from coronal holes, but its source close to the solar 'surface' has been a matter of debate even in today's era of modern solar observations. Recently, it has been suggested that the fast solar wind outflow starts at about 10 kilometers per second in coronal funnels, which are located at the edges of the chromospheric magnetic network inside coronal holes.

We present further evidence that the outflow might also originate from above 'explosive event' sites. These jets have a lifetime of about 5 minutes and are often seen reoccurring at the same location over intervals of typically 20-30 minutes.

Although the expelled jets might actually extend high in the Sun's atmosphere, they are not seen in the intensity on the disk. Some of the transparent features might nevertheless appear as macrospicules at the Sun's edge. This observation itself is shedding new light onto another long-standing question regarding the nature of macrospicules.

These results about the small-scale structures of coronal holes and their consequence on explaining the nature of the fast solar wind have been derived due to an innovative way of extracting information from the spectral data offered by SOHO’s highest resolution detector, SUMER. The 'secret' of our technique lies in understanding plasma properties from the signature it leaves in the shape and widths of the spectral lines.

Short Scale Magnetic Turbulence In The Solar Wind

V. Krishan*

*Indian Institute of Astrophysics

Koramangala, Bangalore 560 034

Karnataka, India

vinod@iiap.res.in

The solar wind is a great paradigm for investigating magnetohydrodynamic turbulence. It is shown that the frame work of Hall magnetohydrodynamics (HMHD), which can support three quadratic invariants and allows nonlinear states to depart fundamentally from the Alfvenic, is capable of reproducing in the inertial range the three branches of the observed solar wind magnetic fluctuation spectrum the Kolmogorov branch k^-5/3 steepening to k^{-α₁} with α₁ ≈ 3-4 on the high frequency side and flattening to k^-1 on the low frequency side. These fluctuations are found to be associated with the nonlinear Hall-MHD Shear Alfven waves.

Session 07: 16:00 – 17:00, Nov. 28, 2006

On the Slow-Rise Phase of Eruptive Quiescent Solar Prominences

N. Srivastava*

*Udaipur Solar Observatory

Physical Research Laboratory

P. O. Box 198, Udaipur 313001

Rajasthan, India
nandita@prl.res.in

The observations taken in He 304 Å reveal that these images are extremely useful to trace prominences because of the relatively sharper spine which is better visible in 304 Å than in H-alpha. In this paper, we have studied several eruptive quiescent prominence images recorded by EIT in He 304 Å during January 2000 - July 2003 in an attempt to identify the precursors of CMEs that are associated with eruptive prominences. Our analyses show that erupting prominences evolve through a pre-eruptive phase and an eruptive phase which are characterized by lower velocities of several km/s and eruptive velocities of several tens to hundreds of km/s, respectively. The analyses also show that during the pre-eruptive phase, a prominence rises at a constant acceleration ranging between 4-12 cm/s² and not at constant velocity as reported by previous workers. The values of acceleration are found to be lower in comparison to that measured during the eruptive phase which ranges between 10-80 m/s². A comparison of height-time profiles of various features of prominences and associated CMEs provides information on their role in the eruption process. We suggest that the characteristic slow rise of eruptive prominences might be considered as reliable amongst all CME precursors. The kinematics of slowly rising filaments/prominences also helps in understanding the nature of propagation of the associated CMEs. We further investigated if the filaments which rise slowly are the ones which are associated with a slow expansion of the corona and/or slow outward motion before the phase of rapid mass expulsion. Such distinctions are extremely useful in identifying the eruption of CMEs directed toward the Earth, when they are associated with erupting filaments.

Coronal Mass Ejections in the Heliosphere

N. Gopalswamy*

*Solar system exploration

Code 695, NASA-GSFC

Greenbelt, MD 20771, USA

gopals@ssedmail.gsfc.nasa.gov

Coronal mass ejections (CMEs) are the most energetic events in the heliosphere. They carry large amounts of coronal magnetic fields and plasma with them and driving large-scale interplanetary shocks. The CMEs and shock have significant consequences at various locations in the heliosphere, including the production of intense geomagnetic storms and large energetic particle events. CMEs form merged interaction regions in the heliosphere, which act as magnetic barriers for the galactic cosmic rays entering the heliosphere. After a brief summary of the observed properties of CMEs at the Sun, I discuss the properties of the interplanetary CMEs (ICMEs) and their connection to shocks, radio bursts, solar energetic particles and modulation of galactic cosmic rays.

Solar Wind Studies: Transients and Steady-State Flows

P. K. Manoharan*

*Radio Astronomy Centre

Tata Institute of Fundamental Research

Udhagamandalam (Ooty) 643 001

Tamil Nadu, India

mano@ncra.tifr.res.in

This paper reviews the regular monitoring of the Interplanetary Scintillation (IPS) of a large number of radio sources at the Ooty Radio Telescope. These measurements provide images of the inner heliosphere and they are useful to study the conditions of the steady-state solar wind and the transients caused by the coronal mass ejections (CMEs) in the `Sun-Earth' space. The result indicates that the radial evolution of the CME speed is determined by its initial speed as well as by its interaction with the preceding transients/background solar wind. This study enables the empirical prediction of arrival of CME at 1 AU. The comparison of the observed and predicted arrivals enhances our understanding of the interaction between the CME and the ambient solar wind flow. The scintillation result on the steady-state solar wind and its changes with the solar cycle will also be discussed.

Session 08: 17:00 – 18:40, Nov. 28, 2006

Solar Energetic Particle Events and Geomagnetic Storms

G. S. Lakhina*, R. Rawat and S. Alex

*Indian Institute of Geomagnetism

Plot No. 5, sector 18, New Panvel

Kalamboli Road, Navi Mumbai 410218

Maharastra, India

gslakhina@rediffmail.com

lakhina@iigs.iigm.res.in

The solar energetic particle (SEP) events are the energetic outbursts as a result of acceleration and heating of solar plasma during solar flares and coronal mass ejections (CMEs). The SEP events are characterized by abrupt enhancements in the proton flux in the energy range of keVs to MeVs as measured by spacecraft at 1 AU. On impacting the earth's magnetosphere, the SEP events can lead to a sudden disturbance of the earth's magnetic field, known as Geomagnetic storms. In the present study, the effects of some strong SEP events of the present solar cycle on various magnetic storm processes are investigated by using the Solar flare and CME data from GOES-8 and SOHO, interplanetary plasma and magnetic field data from ACE and Wind, and the ground magnetic field data from Alibag and Tirunelveli magnetic observatories. The main focus will be to highlight the low latitude geomagnetic signatures produced by these SEP events. The SEP events with the persistence of high level of proton flux after the shock are found to be associated with intense magnetic storms. The role of SEP events in the prediction of intense geomagnetic storms will be discussed.

Solar Influence on Ionosphere and Radio Communications

B. M. Reddy*

*National Geophysics Research Institute

Uppal Road, Hyderabad 500 007

Andhra Pradesh, India

borramreddy@rediffmail.com

When we are discussing solar influence on Ionosphere, it will be helpful to remember that less than one-thousandth of the solar energy being intercepted by the planet Earth is responsible for its production and dynamics. This includes the solar wind energy intercepted by a much larger magnetosphere. But it is this small fraction of energy (in the X-rays, EUV and solar wind) that undergoes violent fluctuations during the course of a solar cycle and during such solar events as flares and Coronal Mass Ejections (CMEs).The consequences of these events are now generically dubbed as “Space Weather”.

The problems created by extreme space weather events encompass a wide variety of applications of human interest. These include difficulties to satellite operations, ionosphere-reflected H.F Communications, GPS operations and even power grids and gas pipelines. I will restrict my presentation to H.F communications and to certain science elements such as anomalous plasma temperature variations measured by satellites. Particular attention will be given to increases in electron temperatures during magnetic storms in the night time when there is no photo-electron heat input. As this has a bearing on the present theory of electron thermal conduction associated with increase in neutral densities during storms, a detailed analysis will be presented using satellite data. Also the presentation will include examples of H.F communication failures especially at night time, contrary to what is expected at low latitudes. This has serious implications to the communication scenario in India in view of the high Atmospheric Radio Noise at the lower bands of the H.F. Spectrum.

Radar Studies of Ionospheric Plasma Irregularities

P. B. Rao*

*National Remote Sensing Agency

Department of Space

Balanagar, Hyderabad 500 037

Andhra Pradesh, India

rao_pb@nrsa.gov.in

High power high resolution VHF radars have proven to be powerful diagnostics to study ionospheric plasma irregularities, a space weather phenomenon of immense importance in view of its impact on space communication and navigation. The VHF radars at Jicamarca, Peru and Trivandrum, India have contributed greatly over the past four decades in arriving at the current understanding of the basic characteristics of the equatorial spread-F (ESF) and equatorial electrojet (EEJ) irregularities and the underlying plasma instability processes. Recent advances, involving high resolution radar observations of equatorial plasma irregularities, include the detection of supersonic plasma bubbles rising to heights beyond 1000 km, 150 km echoes and kilometric scale waves. The new and more recent developments in plasma irregularity studies came from the middle and upper atmosphere (MU) radar at Shigaraki, Japan and the mesosphere – stratosphere – troposphere (MST) radar at Gadanki, India. The new types of plasma irregularity structures observed by this mid- and low latitude VHF radars cover the well known quasi- periodic (QP) waves, tidal ion layers, kilometric scale waves and structures in the collision dominated lower E region. The paper presents an overview on the recent advances in the radar technique and the above mentioned new developments in observation and theory of the equatorial and low latitude ionospheric plasma irregularities.

Physical Processes underlying the Equatorial Effects of Solar Wind Dynamic Pressure (P_d) Variations

J. H. Sastri*

*Indian Institute of Astrophysics

Koramangala, Bangalore 560 034

Karnataka, India

jhs@iiap.res.in

In this talk, I shall endeavor to present a concise review of recent work concerning the equatorial geomagnetic and ionospheric effects of variations in solar wind dynamic pressure, P_d at the sub-solar magnetopause. Though the equatorial effects are the primary concern here, the global perspective will be retained to provide an overall picture of the coupling processes involving the magnetosphere-high latitude ionosphere-low latitude ionosphere domains. Two types of P_d changes are dealt with here. The first one is the sudden step-like increase in P_d representative of interplanetary shocks and other discontinuities in the solar wind that lead to the well-known geomagnetic storm sudden commencements (SSC) and sudden impulses (SI). These abrupt changes in P_d are documented to also initiate, at times, magnetospheric substorms and long-period ( 1hour) magnetospheric and ionospheric oscillations. Variation in P_d on time scales longer that of shocks and discontinuities are the other type. Awareness of the geomagnetic field response to this type of P_d changes is fairly recent and experimental evaluation of the physical situation that prevail at auroral and equatorial regions where the contribution of ionospheric currents may be expected to be as significant as those of magnetopause currents is indeed at a nascent stage now. In contrast, SSC and SI have been extensively studied over the decades using ground and space-borne magnetometers and a credible phenomenological model based on them has been developed, as also numerical modeling. Nonetheless, several fundamental and important questions remain to be settled. Foremost among these are: (1) the origin of the bi-modal response of the equatorial daytime H-field to sudden magnetospheric compressions induced by shocks with the resulting SSC taking two distinct forms, namely, with and without a preliminary reverse impulse (PRI) which occur more or less with equal frequency and (2) the mechanism of extension of the PRI from high latitudes to the dayside dip equator (propagation through the Earth-ionosphere waveguide or following the so-called ‘Tamao path’?). It is argued that to achieve progress in resolving these and other issues, in addition to the existing meridional magnetometer networks, the longitudinal network of equatorial magnetometers (run as a part of Circum-pan Pacific Magnetometer Network, CPMN by Kyushu University, Japan) needs to be strengthened as regards spatial coverage and GPS- time synchronization. New initiatives aimed at establishment of longitudinal networks of well chosen passive diagnostics of the ionosphere medium are also needed for the dip equatorial region. These requirements can be realized under the aegis of International collaborative and cooperative programs such as IHY.

Interplay Between the Equatorial Geophysical Processes

R. Sridharan*

*Space Physics Laboratory

Vikram Sarabhai Space Centre

Trivandrum 695 022, Kerala, India

r_sridharan@vssc.gov.in

r_sridharanspl@yahoo.com

With the sun as the main driving force, the Equatorial Ionosphere- thermosphere system supports a variety of Geophysical phenomena, essentially controlled by the neutral dynamical and electro dynamical processes that are peculiar to this region. All the neutral atmospheric parameters and the ionospheric parameters show a large variability like the diurnal, seasonal semi annual, annual, solar activity and those that are geomagnetic activity dependent. In addition, there is interplay between the ionized and the neutral atmospheric constituents. They manifest themselves as the Equatorial Electrojet (EEJ), Equatorial Ionization Anomaly (EIA), Equatorial Spread F (ESF), Equatorial Temperature and Wind Anomaly (ETWA). Recent studies have revealed that these phenomena, though apparently might show up as independent ones, are in reality interlinked. The interplay between these equatorial processes forms the theme for the present talk.

Session 09: 09:00 – 10:20, Nov. 29, 2006

Effect of Solar Variability on the Evolution of Equatorial Spread F

A. Bhattacharyya*

*Indian Institute of Geomagnetism

Plot No. 5, sector 18, New Panvel

Kalamboli Road, Navi Mumbai 410218

Maharastra, India

abh@iigs.iigm.res.in

Equatorial spread F (ESF) is a nighttime phenomenon of the equatorial and low latitude ionospheres. Its genesis is the growth of a generalized version of the Rayleigh-Taylor instability on the bottom-side of the equatorial F region. Ostensibly, conditions favorable for the growth of the instability are always present during post-sunset hours. However, the day-to-day variability in the occurrence and spatio-temporal characteristics of the electron density irregularities associated with ESF continues to elude explanation. Investigation of this phenomenon is of relevance from the practical point of view as well; since the intermediate scale length (~100m to a few km) irregularities associated with ESF, scatter incident radio waves of VHF or higher frequencies to produce fluctuations or scintillations in amplitude and phase of such radio signals recorded on the ground. Detrimental effects of ionospheric scintillations on satellite based communication and navigation systems such as GPS are particularly severe in the equatorial anomaly region. Solar variability has been observed to influence the ESF phenomenon. Effects of different aspects of solar variability on the evolution of ESF irregularities is explored here, on the basis of observations of ionospheric scintillations produced on radio wave signals by the intermediate scale ESF irregularities.

Long-Term Variabilities of Planetary-Scale Waves in the Mesosphere-Lower Thermosphere (MLT) Region

S. Gurubaran*

*Equatorial Geophysical Research Laboratory

Indian Institute of Geomagnetism

Krishnapuram, Maharajanagar

Tirunelveli 627 011, Tamil Nadu, India

guru_iig@rediffmail.com

gurubara@iigs.iigm.res.in

The mesosphere-lower thermosphere (MLT) region is an important critical transition region that dynamically couples the middle atmosphere (20-100 km) with the upper atmosphere and ionosphere. This is the region where atmospheric gravity waves often achieve convectively unstable amplitudes and thereby dissipate, generate turbulence and deposit heat and momentum in the mean flow. Turbulence influences chemistry through the transport and distribution of long-lived chemical species such as NO. Tidal oscillations of 24-hour (diurnal) and 12-hour (semi-diurnal) periods are generated by water vapor and ozone insolation absorption in the troposphere and stratosphere and propagate through the mesopause into the lower thermosphere. Tides represent a major source of temperature and wind variability in the tropical mesopause region and are also capable of generating turbulence and depositing heat and momentum above 85 km. Other planetary-scale waves propagating through the mesosphere and contributing to its energy and momentum budgets are the global-scale normal modes, namely, the quasi-2-day and 16-day waves, the 6.5-day wave and the equatorially trapped wave mode, namely, the 3.5-day ultrafast Kelvin wave.

Through several collaborative studies making use of the existing MLT radar network, the IHY2007 programme would provide enough opportunities to examine how the above dynamical processes behave in longer time scales and influence the climate of the middle atmosphere. Long-term data sets on important planetary-scale wave parameters would also address the important issue of Sun/Earth connections induced by a possible planetary wave response to solar variability.

This talk is intended to motivate and promote such collaborative studies aimed to understand the processes responsible for the long-term variabilities of planetary-scale waves and their role in the climate of the middle atmosphere.

Radar and Lidar Probing of The Atmosphere

D. Narayana Rao*

*National Atmospheric Research Laboratory

Po.Box 123, Tirupati 517 502

Andhra Pradesh, India

profdnrao@narl.gov.in

Abstract yet to be received

A Tomographic Reconstruction Technique Applied to the GPS TEC Data

E. Y. Kassie*

*Institute of Geophysics and Planetary Physics

UCLA, P. O. Box 951567, 3845 Slichter Hall

CA 90095-1567, Los Angeles, USA

ekassie@igpp.ucla.edu

ekassie@ucla.edu

An image of the dayside low-energy ion outflow event that occurred on 16 December 2003 was constructed with ground- and space-based GPS (Global Positioning System). Total Electron Content (TEC) data and ion drift meter data from the DMSP (Defense Metrological Satellite Program). A tomographic reconstruction technique has been applied to the GPS TEC data obtained from the GPS receiver on the Low Earth Orbit (LEO) satellite FedSat. The two dimensional tomographic image of the topside ionosphere and plasmasphere reveals a spectacular beam-like dayside ion outflow emanating from the cusp region. These outflows are associated with heating due to low-energy precipitating electrons. The transverse components of the magnetic field in the NewMag data show the presence of FAC (field aligned current) sheets, indicating the existence of low energy electron precipitation in the cusp region. The DMSP ion drift data show upward ion drift velocities and upward fluxes of low energy ions and electrons at the orbiting height of the DMSP spacecraft in the cusp region. This study presents the first image of the flux tube structure of ionospheric ion outflows from 0.13 Re up to 3.17 Re altitude.

Session 10: 10:40 – 12:10, Nov. 29, 2006

Generalized Measure of Entropy, Mathai's Distributional Pathway Model, and
Tsallis Statistics

A. M. Mathai*, and H. J. Haubold

*Centre for Mathematical Sciences

Pala Campus, Arunapuram

Pala 686 574, Kerala, India

cmspala@gmail.com

mathai@math.mcgill.ca

The well-known pathway model of Mathai (2005) mainly deals with the rectangular matrix-variate case. In this paper the scalar version is shown to be associated with a large number of probability models used in physics. Different families of densities are discussed, which are all connected through the pathway parameter α, generating a distributional pathway. The idea is to switch from one functional form to another through this parameter and it is shown that basically one can proceed from the generalized type-1 beta family to generalized type-2 beta family to generalized gamma family when the real variable is positive and a wider set of families when the variable can take negative values also. For simplicity, only the real scalar case is discussed here but corresponding families are available when the variable is in the complex domain. A large number of densities used in physics are shown to be special cases of or associated with the pathway model, including Maxwell-Boltzmann, Fermi-Dirac, and Bose- Einstein distributions. It is also shown that the pathway model is available by maximizing a generalized measure of entropy, leading to an entropic pathway. Particular cases of the pathway model are shown to cover Tsallis statistics (Tsallis, 1988) and the superstatistics introduced by Beck and Cohen (2003).

Test of Non-extensive Statistical Mechanics by the Solar Sound Speeds Measured in Helioseismology

Du Jiulin*

*Department of Physics

School of Science, Tianjin University

Tianjin 300072, China

jiulindu@yahoo.com.cn

jldu@tju.edu.cn

To check the validity of the theory of non-extensive statistical mechanics, we have investigated the non-extensive degree of the solar interior and have tried to find the experimental evidence by helio-seismological measurements that q is different from unity. We are able to derive a parameter for providing a lower limit to the non-extensive degree inside the sun that can be uniquely determined by the solar sound speeds measured by helioseismology. After calculating the parameter by using the solar sound speeds, we get the lower limit of (1-q)0.1902 for all solar radii between 0.15R and 0.95R and (1-q)0.4 for the out layers, 0.75R r 0.95R. Thus, the result that the non-extensive parameter q is significantly different from unity in the sun has received the support by the experiment measurements for the solar sound speeds in helioseismology.

Systematics of Dynamo Action in a Shell Model for Magnetohydrodynamic Turbulence

G. Sahoo, and R. Pandit*

*Centre for Condensed Matter Theory

Department of Physics

Indian Institute of Science

Bangalore 560 012, Karnataka, India

rahul@physics.iisc.ernet.in

We carry out high-resolution studies of the dynamo effect in a shell model for magnetohydrodynamic (MHD) turbulence at low magnetic Prandtl numbers (as low as 10⁵). We present the stability diagram for the formation of a turbulent dynamo in this MHD shell model in magnetic Prandtl number and magnetic Reynolds number plane. Our systematic numerical studies show that a fractal-like boundary separates the dynamo and no dynamo regimes in this plane.

Session 11: 12:10 – 13:10, Nov. 29, 2006

CALLISTO – Radio Spectrometer

C. Monstein*

*ETH Zurich, Astronomical Institute

Scheuchzerstrasse 7

CH 8092 Zurich, Switzerland

monstein@astro.phys.ethz.ch

CALLISTO, a low cost radio spectrometer, will be distributed all over the world at different longitudes for continuous observation of the solar-radio activity at meter- and decimeter wavelengths. All data will be collected at ETH Zurich via the Internet to produce a 24^th overview between 45MHz and 870MHz. All participants will have full access to all data captured within this project. The concept and technical detail of CALLISTO and hopefully some first results will be presented. A full operational spectrometer will also be presented during the meetings.

Chain-Project and Installation of Flare Monitoring Telescopes in Developing Countries

S. Ueno*, et al.

*Kwasan & Hida Observatories, Graduate School of Science

Kyoto University, Kurabashira, Kamitakara

Takayamashi, Gifu-Ken 506-1314, Japan

ueno@kwasan.kyoto-u.ac.jp

The Flare Monitoring Telescope (FMT) was constructed in 1992 at the Hida Observatory in Japan to investigate the long-term variation of solar activity and explosive events. It has been part of the international coordinated observations program (STEP) since 1991. The FMT consists of five solar imaging telescopes and one guidescope. The five telescopes simultaneously observe the full-disk Sun at different wavelengths around H-alpha absorption line or in different modes. Therefore, the FMT can measure the vector velocity field of moving structures on the full solar disk without the visual effect. We want to monitor solar flares and erupting filaments continuously as much as possible by using several of such characteristic telescopes. We are then planning to execute the "Continuous H-alpha Imaging Network (CHAIN)-project". As part of this project, we are examining the possibility of installing the telescopes in developing countries with acquiring the necessary funds from the United Nations. More precisely, we are currently examining Peru as a candidate country where a telescope will be installed. Moreover, there are a lot of items that should be investigated in various respects in advance, such as the natural environment, the human environment and the method of clerical work procedure, etc. In this talk, we introduce characteristics of the FMT, some scientific results and our plans of installing the FMT in Peru.

Space Weather Activities at SERC for IHY : Magnetic Data Acquisition System (MAGDAS)

K. Yumoto* and MAGDAS/CPMN group

*Space Environment Research Center (SERC)

Kyushu University

6-10-1 Hakozaki Higashi-ku

Fukuoka, Japan

yumoto@serc.kyushu-u.ac.jp

arnoldyuki@serc.kyushu-u.ac.jp

One purpose of Solar Terrestrial Physics (STP) research in the twenty-first century is to support human activities in Space from the aspect of basic research. The scientific aim of the STP community is the creation of new physics: (1) couplings of the complex and composite systems and (2) macro-and-micro-scale couplings in the Solar-Planetary system. The intention is to construct a new Network of Stations for ground-based observations and for simulations/empirical modeling.

The Space Environment Research Center (SERC), Kyushu University, is currently deploying a new ground-based magnetometer network, in cooperation with about 30 organizations around the world, in order to study the complex Sun-Earth system for space weather. SERC conducts MAGDAS (MAGnetic Data Acquisition System) observation at 50 stations in the CPMN (Circum-pan Pacific Magnetometer Network) region, and conducts frequency modulated continuous wave (FM-CW) radar observation along the 210° magnetic meridian during the IHY/IPY/eGY/ ILWS/CAWSES periods. From these network observations, we will clarify:

(1) The dynamics of plasmaspheric changes during space storms and substorms,

(2) Electromagnetic responses of magnetosphere-ionosphere-thermosphere complex system to various solar wind changes, and (3) penetration mechanisms of DP2-ULF range disturbances from the solar wind into the equatorial ionosphere.

In the present paper, we will first introduce our real-time data acquisition and analysis system of MAGDAS/CPMN, which was deployed in 2005 and 2006, and preliminary results from the MAGDAS project. This project is actively providing the following:

(1) Monitoring the global 3-dimensional current system to know the electromagnetic coupling of high-latitude and Sq current systems, and

(2) Monitoring of the plasma density to understand space plasma environment change during space storms. We will also present our FM-CW radar system at L=1.26 to deduce the electric field from the ionospheric plasma drift velocity. From 24hr monitoring of the ionospheric drift velocity with 10-sec sampling by the FM-CW radar observation, we can understand how the polar electric field penetrates into the equatorial ionosphere.

Session 12: 14:10 – 15:30, Nov. 29, 2006

Geophysics Integrated Studies in the Sun Earth System: A Cooperative Project of Vietnam, Europe, and Africa

C. Amory-Mazaudier* et al.

*CETP/CNRS, 4 Avenue de Neptune

94107 Saint-Maur-des-Fossés, France

christine.mazaudier@cetp.ipsl.fr

lhminh@igp.ncst.ac.vn

The Hanoi Institute of Geophysics (Vietnam) will participate to international Heliophysical Year. This paper presents Vietnam‘s participation into this International cooperative project : the Vietnamese network of magnetometers, meteorological stations, ionosondes and GPS receivers involved in campaigns of measurements, the research field selected for the training of young Vietnamese scientists, and the Institutes involve in this training. This paper also presents some particularities of geophysical parameters in Vietnam : the strong amplitude of the equatorial electrojet observed by satellite data and confirmed by magnetic observations at the ground level presented for the first time to the international community, the monsoon signature etc. Finally the differences between the Asian sector and the African sector lead to the development of comparative studies between Asia and Africa.

Expanding the SCINDA Sensor Network for the IHY- 2007

K. M. Groves*

*AFRL/VSBXI, 29 Randolph Road

Hanscom, AFB, MA 01731, USA
keith.groves@hanscom.af.mil

The first communications satellites were launched in the early 1960s to support the needs of a small and specialized user community. Since that time the number of systems has expanded dramatically so that a majority of the world’s population now benefits from the communication and navigation services available. As the use of space-based RF systems has increased, the impacts of ionospheric disturbances have become more significant. The most serious effect of these disturbances is known as scintillation, a phenomenon caused by small-scale variations in electron density (irregularities) along the propagation path that result, principally through diffraction, in rapid amplitude and phase fluctuations of the radio wave. Substantial mid- latitude disturbances are generally associated with infrequent magnetic storm events, but significant irregularities form routinely at both high and low latitudes. At equatorial latitudes, the occurrence of post-sunset Spread F is of special concern because the region affected comprises more than 30% of the earth’s surface and the effects on VHF and UHF radio wave propagation are severe. To better characterize this phenomenon and now cast its occurrence, the Air Force Research Laboratory (AFRL) has developed a ground-based sensor system to autonomously monitor scintillation using available satellite beacons such as geostationary satellite communication signals and GPS. Known as the Scintillation Network Decision Aid (SCINDA), the system performs real-time on-site calculations of scintillation parameters, zonal drift velocity and total electron content (TEC) and retrieves the data from low-latitude stations via the internet at regular intervals. Fourteen sites have been established thus far and the network is expected to double over the next two years with expansion across Africa and Asia. The African sector is of special interest because very limited historical ground-based observations exist while recent satellite data suggest global activity may actually peak over the continent. The goal is to establish new monitoring sites in time to support the International Heliophysical Year (IHY) 2007 and maintain the sensors operation through the next solar maximum in 2011-12.

Preliminary Observations of Ionospheric Structures using Ground Receivers and the COSMIC Radio Beacon

T. W. Garner*, T. L. Gaussiran II, and G. S. Bust

*Space and Geophysics Laboratory

Applied Research Labs

P. O. Box 8029

The University of Texas at Austin

Austin, Texas 78713-8029, USA

garner@arlut.utexas.edu

With the launch of the Constellation Observing System for Meteorology, Ionosphere and Climate (COSMIC) satellite constellation, a new era has begun for low-Earth-orbiting (LEO) satellite beacon research has begun. Each COSMIC satellite carries a radio beacon that can emit at 1066, 400, and 150 MHz. Coherent Ionospheric Doppler Receivers (CIDR) deployed at mid-latitudes observe the electron content and phase scintillation in the 400 and 150 MHz channels. In addition to high (Alaska and Greenland) and low (Peru) latitude systems, CIDRs are deployed in Austin, Texas, a chain across southern New York, Millstone Hill, and Wallops Island. This study presents preliminary observations of different ionospheric structures using CIDR receivers and the COSMIC radio beacon.

VLF Remote -Sensing of the Lower Ionosphere with AWESOME Receivers: Solar Flares, Lightning-induced Electron Precipitation, Sudden Ionospheric Disturbances, Sprites, Gravity Waves and Gamma-ray Flares

U. S. Inan*, M. Cohen, P. Scherrer, and D. Scherrer

*Stanford University

Stanford, California, 94305, USA

inan@stanford.edu

Stanford University Very Low Frequency (VLF) radio receivers have been used extensively for remote sensing of the ionosphere and the magnetosphere. Among the phenomena that can be uniquely measured via VLF receivers are radio atmospherics, whistlers, electron precipitation, solar flares, sudden ionospheric disturbances, gravity waves, sprites, and cosmic gamma-ray flares. With the use of simple square air-core magnetic loop antennas of a couple of meters in size, the sensitivity of these instruments allows the measurement of magnetic fields as low as several tens of femtoTesla per root Hz, in the frequency range of ~300 Hz to 50 kHz. This sensitivity well exceeds that required to detect any event above the ambient atmospheric noise floor, determined by the totality of lightning activity on this planet. In recent years, as cost of production, timing accuracy (due to low cost GPS cards), and data handling flexibility of the systems has improved, it has become possible to distribute many of these instruments in the form of arrays, to perform interferometric and holographic imaging of the lower ionosphere. These goals can be achieved using the newest version of the Stanford VLF receiver, known as AWESOME: Atmospheric Weather Educational System for Observation and Modeling of Electromagnetics. In the context of the IHY/UNBSS program for 2007, the AWESOME receivers can be used extensively as part of the United Nations initiative to place scientific instruments in developing countries. Drawing on the Stanford experiences from setting up arrays of VLF receivers, including an interferometer in Alaska, the Holographic Array for Ionospheric and Lightning research (HAIL) consisting of instruments at 13 different high schools in mid-western United States, a broader set of ELF/VLF receivers in Alaska, and various receivers abroad, including in France, Japan, Greece, Turkey, and India, a global network of ELF/VLF receivers offer possibilities for a wide range of scientific topics, as well as serving as a means for educational outreach. Most recently, AWESOME receivers were placed in several North African countries, including Tunisia, Algeria, and Morocco. The new AWESOME version is substantially lower in cost, and easier to set-up and use. Nevertheless, the receivers offer the same ultimate levels of resolution in time, sensitivity and dynamic range, as well as ease of handling of data that is used by researchers conducting cutting edge ionospheric and Space Weather research. In this context, the placement of these systems at underdeveloped host countries provides an open-ended potential for exploration, limited only by the imagination and drive of the users.

Session 13: 16:00 – 17:00, Nov. 29, 2006

Southern Hemisphere Magnetic Variations Improved Coverage and South Atlantic Magnetic Anomaly (SAMA) Monitoring by the Installation of a Small Magnetometer Network on the Brazilian Territory

J. H. Fernandez*, et al.

*University of Taubaté – UNITAU,

R, Ângela Atuati 151

Parque São Luiz Jundia, São Paulo, Brazil

henrique@unitau.vr

At the present time the magnetic planetary indices, specially the K_p (A_p) index, are basically North Hemisphere indices since the ample majority of the magnetic observatories that generate the indices are located above the Equator.The improving necessity in the coverage of the planetary indices leads to the installation of new and modern equipment in the Southern Hemisphere. Brazil has a special location in terms of being the site for the installation of such equipment. The South Atlantic Magnetic Anomaly (SAMA) is over the South Brazilian region at this moment and there are several groups from research institutes and universities, in Brazil, that can operate and maintain the equipments, carry out the data analysis and put the available data on the Internet.

Space weather is a modern term to denote physical conditions in space around the Earth that are ultimately determined by solar activity. Space weather manifests itself through various physical phenomena such as enhanced intensity of hard radiation, increased strength of electric and magnetic fields and elevated magnitude of electric currents, to name only a few. A "magnetic storm", which may also be called a "space storm", is a rather violent phase of space weather and is often caused by solar outbursts such as flares and coronal mass ejections. Solar outbursts create disturbances of the solar wind that may impact the Earth environment with a delay of a few days after their eruption from the Sun.

Also at the present time the Kp world network is composed of 13 magnetic observatories, 11 northern and two southern stations. The K indices are defined everywhere, but are most significant at sub-auroral latitudes. In the proposed project several magnetometers in the network could contribute to the generation of the planetary average giving a more realistic character to the index.

Main scientific goals:

- Improvement in the monitoring of the Southern Hemisphere magnetic variations

- Local and continuous monitoring of the South Atlantic Magnetic Anomaly (SAMA)

- Magnetosphere/atmosphere interaction

- Equilibrium mechanisms of the Van Allen Radiation Belts (Trimpi events versus geomagnetic activity)

In this presentation we will defend the implementation of a small network of magnetometers on the Brazilian territory (Figure 1) and we will show some important benefits that it could bring to the current space physics research, specially having in mind the implementation of the IHY-2007.

High Latitude Energetic Particle Boundaries: The SAMPEX Database

S. G. Kanekal*, and D. N. Baker

*Laboratory for Atmospheric and Space Physics (LASP)

University of Colorado

12234, Innovation Drive

Boulder CO 80303, USA

shrikanth.kanekal@lasp.colorado.edu

The size of the polar cap or the open field line region depends, upon the difference in reconnection rates at the dayside between the IMF and the geomagnetic field, and those occurring in the magnetotail. The dayside merging adds flux to the open field region increasing the polar cap size and the magnetic flux in the lobes of the tail, thereby causing energy to be stored in the magnetosphere. Night side reconnection, geomagnetic storms and substorms dissipate this energy removing flux and shrink the polar cap. The dynamics of the polar cap can therefore be useful in the study of the energy dynamics of the magnetosphere.

Energetic particles delineate magnetospheric regions, since their motions are governed by the geomagnetic field. Convection and corotation electric fields control the drift of low energy particles whereas magnetic field gradient and curvature are the dominant factors for higher energy (> ~30 keV) particles. High latitude energetic particle boundaries are related to the polar cap and therefore useful in determining the size of the open field line regions

We will provide a long database of energetic particle boundaries in the polar regions using instruments aboard SAMPEX, the first of the Small explorer (SMEX) spacecraft. It was launched on July 3, 1992 into a low earth polar orbit. There are four particle detectors, HILT, LICA, PET and MAST on board which point toward the zenith over the poles of the Earth. These detectors measure electrons, protons and ions ranging in energy from tens of keV to a few MeV.

This database will comprise the latitudinal (geographic, magnetic and invariant) and longitudinal (geographic and magnetic local time) positions of energetic particle boundaries in the polar regions. The database will cover a time period from launch to about mid 2004. It will therefore cover a significant portion of the solar cycles 22 and 23.

Together with interplanetary data obtainable from public databases, such as the NASA OMNI database the SAMPEX energetic particle database can be used to relate Earth's magnetospheric response to the interplanetary drivers such as solar wind speed, density and magnetic field.

Prospects for GDL and SSW

R. A. Schwartz*

*SSAI, NASA/GSFC, Code 612.1

Greenbelt, MD 20771, USA
richard.schwartz@gsfc.nasa.gov

rschwartz@pop600.gsfc.nasa.gov

We demonstrate that great progress has been made in developing GDL as an alternative for using Solar Software IDL programs. We shall give an up to date status on the prospects for using this free software as an alternative for the more costly RSI/IDL.

Session 14: 09:00 – 10:40, Nov. 30, 2006

Coordinated Investigation Program: IPS and Callisto at Ooty

P. K. Manoharan*

*Radio Astronomy Centre

Tata Institute of Fundamental Research

Udhagamandalam (Ooty) 643 001

Tamil Nadu, India

mano@ncra.tifr.res.in

In this presentation, the concept of Coordinated Investigation Programs (CIP) will be introduced and some examples presented. The interplanetary scintillation (IPS) measurements available from different observatories through CIP during 2007-2008 and for the later period will be discussed. The operation of the Callisto, the solar radio spectrograph hosted at the Radio Astronomy Centre, will be discussed with some examples.

Very Low Frequency (VLF) studies of Ionospheric/Magnetospheric Electromagnetic phenomena in Indian Low Latitude Region using AWESOME Receivers

R. Singh*, B. Veenadhari, and S. Alex

*Indian Institute of Geomagnetism

Plot # 5, Sector 18

Kalamboli Highway, New Panvel

Navi Mumbai 410 218, India

rsingh@iigs.iigm.res.in

Ground based observations of whistler mode ELF/VLF (300 Hz 30 kHz) waves are considered as an important remote sensing tool for the investigation of upper atmosphere and magnetosphere. These VLF waves find their origin in various natural and artificial phenomena, the natural sources include thunderstorms, lightning and associated phenomena. Despite of the fact that conjugate region of India having less
lightning activity as it lies in Indian Ocean and also the height of the magnetic field lines connecting the conjugate regions lies in the ionosphere/atmosphere, lot of interesting VLF activity through the magnetosphere is observed in Indian low latitude region. Sub-ionospheric VLF transmissions propagating inside the Earth-ionosphere wave-guide is also being widely used for investigating sudden ionospheric perturbations in lower part of the ionosphere. For this purpose we propose to monitor VLF signals continuously at several locations in Indian sector with the help of AWESOME VLF receivers from Stanford University. AWESOME receivers are capable of collecting both broadband (used for the study of natural signals) and narrowband (sub-ionospheric VLF signals corresponding to VLF transmitters) data. The obtained data will enable us to understand the generation and propagation mechanism of radio atmospherics from lightning flashes, magnetospheric whistlers, VLF emissions and other naturally occurring phenomena. Narrowband sub-ionospheric VLF signals and ground based geomagnetic data in Indian low latitude region will help us to study sudden ionospheric disturbances associated with transient phenomena like solar flares, geomagnetic storms, cosmic gamma-ray flares, etc.

Space Environmental Viewing and Analysis Network (SEVAN) - A Network of Neutron Monitors in Bulgaria

K. Georgieva*

*Solar terrestrial influences laboratory

Bulgarian academy of sciences (STIL-BAS)

Bl3 Acad.G…Bonchev Street

Sofia 113, Bulgaria
kgeorg@bas.bg

katyagerogieva@msn.com

A network of middle to low latitude particle detectors called SEVAN (Space Environmental Viewing and Analysis Network) aims to improve fundamental research of the space weather conditions and provide possibilities to perform short and long-term forecasts of the dangerous consequences of the space storms. The network will detect changing fluxes of the most species of secondary cosmic rays at different altitudes and latitudes, thus constituting powerful integrated device in exploring solar modulation effects. Recently two more countries have decided to host cosmic ray monitors - Bulgaria and Croatia.

Preparation of IHY-2007 in Indonesia: Local Observational Facilities, International Collaborations, and the Use of International Data

T. Djamaluddin*

*National Institute of Aeronautics and Space (LAPAN)

Jl. Dr. Djundjunan 133, Bandung 40173

West Java, Indonesia

t_djamal@bdg.lapan.go.id

t_djamal@hotmail.com

Since 1980, the National Institute of Aeronautics and Space (LAPAN) has been carrying out integrated observations of solar activities, geomagnetic disturbance, and ionospheric parameters, as well as other solar-terrestrial relationship research. International collaboration, especially with Japan in the field of solar physics, geomagnetism and equatorial atmosphere and with Australia in the field of ionosphere and upper atmosphere, help us in increasing national capacity building. The international data available on the Internet also helps us in comparing our local data with the global one or in fulfilling our needs of data due to lack of facilities, ground based or space based data. Some results will be reviewed. Preparation for IHY-2007 will also be discussed.

Space and Atmospheric Physics Education and Research at North Carolina A&T State University

J. R. Nair, G. Smith and A. Kebede*

*Department of Physics

North Carolina A&T State University

Greensboro, NC 27411, USA

lmak27455@yahoo.com

gutaye@ncat.edu

In this communication we discuss the new undergraduate and graduate space and atmospheric physics program at NC A&T State University. The program is designed to train future generation space scientists to meet the workforce needs of NASA, aerospace industries and academic institutions. In order to fortify this effort, we have initiated collaboration with US Air Force, GSFC and University of Michigan. We plan to contribute to the current scientific issues associated with TEC variations, scintillations and disturbances, and the morphology/manifestations of Ionospheric Spread F phenomena, and their variations with locations, specifically over low and mid-latitudes. In order to facilitate research we plan to install a magnetometer, a coherent beacon receiver and GPS receivers. In the long run the space science research community and K12 students and teachers will use of these facilities. We will discuss our recent experience during the IHY-SCINDA 2006 workshop, in Sal Cape Verde, as well as the plans of the upcoming IHY-Africa workshop, November 5-9, 2007 Addis Ababa Ethiopia.

Session 15: 11:00 – 12:45, Nov. 30, 2006

Astronomy in Syria

A. T. Al-Mousli*

*General Organization of Remote Sensing (GORS)

P. O. Box: 12586, Damascus, Syria

gors@mail.sy

Syria has been involved in the field of astronomy since 1997, when Prof. F.R. QUERCI, France, visited Syria and made a presentation on the International NORT project; (NORT: the Network of Oriental Robotic Telescope), which was a selected project of the sixth United Nations/ European Space Agency Workshop on Basic Space Science (document no. A/AC.105/657 dated 13/12/1996). NORT aims to establish a robotic telescope network on high mountain peaks around the Tropic of Cancer, from Morocco in the west to the desert of China in the east. The purposes for establishing this network are technical and educational. The General Organization of Remote Sensing (GORS) has carried out a pilot study using remote sensing techniques and has selected four sites in order to determine the best location for the astronomical observatory the within NORT programme. Following this project, GORS decided to establish an office for astronomical studies, one of the earliest works of GORS in astronomy was an initiative to establish a planetarium within the GORS campus, to accommodate approximately 120 observers. A contest to choose the best planetarium design, for the Arab World, took place at GORS.

A Solar Station for Education and Research on Solar Activity at a National University in Peru

J. K. Ishitsuka*

*Instituto Geofisico del Peru (IGP)

Calle Badajoz 169, Urb Mayorazgo IV

Etapa, Ate, Lima 3, Peru

pepe@hotaka.mtk.nao.ac.jp

pepe@geo.igp.gob.pe

Beginning in 1937, the Carnegie Institution of Washington made active regional observations with a spectro-helioscope at the Huancayo Observatory. In 1957, during the celebration of the International Geophysical Year Mutsumi Ishitsuka arrived at the Geophysical Institute of Peru and restarted solar observations from the Huancayo Observatory. Almost 69 years have passed and many contributions for the geophysical and solar sciences have been made. Now the Instituto Geofisico del Peru (IGP), in cooperation with the Faculty of Sciences of the Universidad Nacional San Luis Gonzaga de Ica (UNICA), and with the support of the National Astronomical Observatory of Japan, are planning to construct a solar station refurbishing a coelostat that worked for many years at the Huancayo Observatory. A 15 cm refractor telescope is already installed at the university, for the observation of sunspots. A solar Flare Monitor Telescope (FMT) from Hida Observatory of Kyoto University could be sent to Peru and installed at the solar station at UNICA. As the refurbished coelostat, FMT will become a good tool to improve education and research in sciences.

Radiative Transfer Model in the Atmosphere and Experimental Solar Data of Yaounde Location

E. G. Dountio*, D. Njomo, E. Fouda,and A. Simo

*Ministry of Scientific Research & Innovation

Institute for Geological & Mining Research

Energy Research Laboratory (MINRESI/IRGM/LRE)

P.O. Box 4110, Yaounde-Longkak, Cameroon

eguemene@yahoo.com

The Sun is the primary source of energy supplying the Earth. This energy absorbed by the various components of the atmosphere, the oceans, the vegetation and Earth’s surface, is at the origin of the forces that control the climatic changes, the general circulation of the atmosphere, the temperature of the atmosphere and that of the oceans and the ionization of atmospheric gases, etc. The solar energy received on Earth’s surface is also directly used in technological applications such as solar heaters, solar dryers and other solar distillers, and the photovoltaic generators, etc. The calculation of the thermal performances of these apparatuses can be well made only if the spectral and even angular distribution of the solar irradiation arriving on the ground surface is well known. Moreover, the well known characteristics of the solar radiation arriving on the ground could inform us about the atmospheric phenomena that influenced its transfer, and consequently provide a better correction of the sensors response while receiving a signal from outer space in its direction, or the correction to be made on the response of a sensor while receiving data from a terrestrial sender.

Only a few measurement stations of solar radiation are currently running and are not well managed, particularly in developing countries where the maintenance of a park of pyranometers on the ground is difficult and expensive. Moreover, where these measurements exist, they are rarely carried out for various wavelengths and/or angles.

Such data are on the other hand accessible by numerical calculation, by solving the radiative transfer equation (ETR) in the atmosphere. One of the major factors attenuating the solar radiation received on the ground is scattering by clouds. The non- homogeneous nature of the clouds justifies the difficulty shown by the researchers to insert realistic profiles of clouds in radiative transfer models in a parallel stratified atmosphere [1, 2]. Several recent studies showed that this non-homogeneity has significant impacts on the transmitted radiation, calculated either for the thick and continuous clouds [3] or for dispersed clouds [4, 5]. Such structures must be studied with a multidimensional radiative transfer model, as for example the one of Stephens [6] judiciously exploited recently by Evans [7], which breaks up the angular part of brightness into spherical harmonics while the space part is simply discretizised by finite differences. We intend here to make a comparison between results of this model and the experimental data collected in Yaounde [8-13]. This is in order to detect its forces, weaknesses and the possible improvements that could be done to guarantee a prediction free from any significant variation with reality.

The first part is devoted to the description of the model. In the second part, we present the results of the model as well as the values resulting from experimental measurements. The last part discusses these results.

High Resolution Spectral Analysis for Irregularly Sampled Helioseismic Data

N. Seghouani*

*Department of Astronomy & Astrophysics

CRAAG, Chemin de l’Observatoire

BP 63 Bouzareah, Algiers, Algeria

nseghouani@yahoo.com

Astronomical ground based data are very often irregularly sampled due to many factors such as: diurnal effect, weather conditions, etc. The analysis of such data cannot be performed with classical tools (such as periodigram) and new adapted methods are required. After presenting some of these techniques, we will focus on a regularized approach of the spectral analysis problem, which gives very good results in the case of band limited and narrow peaks spectrum. We will also show that with this approach we can achieve high-resolution spectra. Indeed, in classical Fourier analysis, spectral resolution is inversely proportional to the observation time T. Considering the spectral analysis problem as an inverse problem and introducing the “a priori” knowledge of band limited and narrow peak spectrum, this limit (1/T) can be exceeded and thus we can achieve highly resolved spectra, even with irregularly sampled data. This technique will be first applied to relevant simulated data, then to helioseismic data.

Additional talk: “Brief description of solar projects in Algiers Observatory”

A brief description of all projects developed in our department and that are related to the sun: helioseismology, solar data analysis (pipelines description), solar activity, VLF project, solar astrolabe (for solar diameter measurement), site testing for day-time observations, and the project of solar observatory in the Tamanrasset area.

Indication of Solar Signal in Indian Ocean Dipole (IOD) Phenomena over Indonesia

J. T. Nugroho*, and C. Y. Yatini

*National Institute of Aeronautics and Space (LAPAN)

Jl. Dr. Djundjunan 133, Bandung 40173

West Java, Indonesia

jalu@bdg.latan.go.id

It has been proposed before that dipole mode phenomena, can cause climate variability in the tropical Indian Ocean region. From empirical evidence, it also has been suggested that solar activity plays a role in affecting climate globally as well as regionally. Here, we support these opinions by reporting that the IOD, in general, has a good correlation with cloud cover especially for western Indonesia (with the Monsoon’s climate pattern) from April 1976 to January 1996, which is indicated by correlation coefficient r=0.64. By using wavelet analysis we also find that solar signals appear strongly on IOD over the December-February period (or wet season in the Monsoon’s climate pattern).

A Developed Numerical Mapping Technique

N. M. R. Al-Ubaidi*

*Department of Astronomy and Space

College of Science

University of Baghdad

Baghdad, Iraq

najatmr10@yahoo.com

An automated mapping technique for representing the hourly behavior of the ionosphere was presented by Rush in 1976. The technique is based on updating the predicted monthly median maps of ionospheric parameters with hourly observations. The procedure was accomplished by computing the differences between the predicted medians and the hourly values of ionospheric parameters that are observed at specific locations on the globe. This technique provides the basis for extending and extrapolating the influence of an observation from the observing location to the region surrounding the observing location. This method is very complicated, so in our research we used another newly developed method. The designed and implemented program in our work for a new mapping technique method was suggested and used to draw the maps based on updating the monthly median of ionospheric parameters predicted with geographic coordinates.

Determination of the Coefficient of Correlation Between Radiation and Relative Humidity, and Determining Equation of the Line of Best Fit Using Statistical Methods

J. O. H. Ndeda*, A. B. Rabiu, L. H. M. Ngoo, and G. O. Ouma

*Department of Physics

Jomo Kenyatta University of Agriculture and Technology (JKUAT)

P.O. Box 62000-00200, Nairobi, Kenya

jndeda6060@yahoo.com

This paper investigates the inter-relationship between solar radiation intensity RD and relative humidity RH in Kenya using daily data obtained at five meteorological stations; Nairobi (1.3°S, 36.75°E), Kericho (0.37˚S, 35.72˚E), Kisumu (0.10˚S, 34.75˚E), Mombasa (4.03˚S, 39.65˚E) and Garissa (0.48˚S, 39.63˚E) during the solar minimum year 1986. Statistical methods were employed and the coefficients of correlation, r obtained range from –0.16094 to -0.6758618 between the two variables for the five stations. The linear equation relating the solar radiation intensity RD to relative humidity RH is obtained using linear regression analysis as RH = 109.1091-1.5997RD for the Nairobi station. Jandel scientific and Megastat software analyses gave fairly similar trends of results for Nairobi and other stations, and for all the seasons except for those of Garissa station. Obviously there exists a negative interdependence between solar radiation intensity and relative humidity such that the relative humidity decreases as solar radiation increases and vice versa. This observation is explicable in terms of the dynamics of atmospheric heating and advection traceable to solar activity.

Session 16: 14:00 – 15:30, Nov. 30, 2006

The Gap in Global Ionospheric and Heliospheric Measurements over Africa: Our Proposals for IHY-2007

A. Mahrous*

*Department of Physics

Faculty of Science

Helwan University, Ain Helwan

Cairo, Egypt

ayman.mahrous@gmail.com

One of the main goals of IHY is to promote space science activities in developing countries. We summarize the current status and perspectives of ionospheric and heliospheric projects in several African countries. The study concerns the GPS receivers, ionosondes, magnetometers and their contribution to the global worldwide measurements. A case study of some energetic events shows the necessity of establishing central stations in Africa to cover the data break in this region of the world. Finally, we discuss the proposals and challenges of IHY 2007 in both educational and space science research, as well as, the framework of the future strategy for the development of space science in Africa.

Space Sciences Education and Outreach Project of Moscow State University

S. Krasotkin*

*Theoretic and Applied Space Physics Department

Moscow State University

Skobeltsyn Institute of Nuclear Physics (SINP/MSU)

1-2 Leninskie Gory, 119992 Moscow, Russia

sergekras@rambler.ru

sergekras@mail.ru

The space sciences education and outreach project was initiated at Moscow State University in order to incorporate modern space research into the curriculum popularize the basics of space physics, and enhance public interest in space exploration. On 20 January 2005 the first Russian University Satellite “Universitetskiy-Tatyana” was launched into circular polar orbit (inclination 83 deg., altitude 940-980 km). The onboard scientific complex “Tatyana“, as well as the mission control and information receiving centre, was designed and developed at Moscow State University. The scientific programme of the mission includes measurements of space radiation in different energy channels and Earth UV luminosity and lightning.

The current education programme consists of basic multimedia lectures “Life of the Earth in the Solar Atmosphere” and computerized practice exercises “Space Practice” (based on the quasi-real-time data obtained from “Universitetskiy-Tatyana” satellite and other Internet resources). A multimedia lectures LIFE OF EARTH IN THE SOLAR ATMOSPHERE containing the basic information and demonstrations of heliophysics (including Sun structure and solar activity, heliosphere and geophysics, solar-terrestrial connections and solar influence on the Earth’s life) was created for upper high-school and junior university students. For the upper-university students there a dozen special computerized hands-on exercises were created based on the experimental quasi-real-time data obtained from our satellites. Students specializing in space physics from a few Russian universities are involved in scientific work. Educational materials focus on upper high school, middle university and special level for space physics students. Moscow State University is now exte