International SCOSTEP Newsletter, March 1999

SCOSTEP ACTIVITIES
EPIC Chair's Report of 1998
ISCS Working Group 2 Activity
Report to IUGG on SCOSTEP Activities 1996-1999

NEWS ITEMS/OPPORTUNITIES
European-US Cooperative Projects Possible
Scientific Radar Instrumentation

PUBLICATIONS
Solar Light Brochure Received
New ICSU "Blue Book" Issued
Special Issue of JGR-Atmospheres on Mesosphere Inversion Layer
Initial Systems in Navigation and Geophysics
ESA Contractor Report on Modeling of FREJA Charging Events
Proceedings of a Meeting on Database and Data Analysis
AL/AU Predictions for 2/17 CME Activity Interval
The Journal of Atmospheric and Solar-Terrestrial Physics (JASTP) now Accepts Electronic Submission

MEETING REPORTS
Solar Physics Planning Group (SPPG) of the European Space Agency
VII Symposium of Solar-Terrestrial Physics
ITM (Ionosphere Thermosphere Mesosphere) Future Planning Opportunities

FORTHCOMING MEETINGS
Sun-Earth Connection Strategic Planning Workshop
Fifth Annual K-12 Education Workshop
EGS ST11: Theory and Simulation of Solar System Plasmas
Second Announcement Space Weather: Research to Operations III
SPRING AGU SESSIONS
Special Session SM02: New Perspectives in Dynamics and Coupling in Inner Magnetospheric Physics
Special Session SM03: Probing Magnetic Storm and Substorm Connections with Global Imaging
Special Session SM06: Space Weather- Observations, Models, and Products
2nd TIGER Symposium (Thermospheric/Ionospheric Geospheric Research)
SHINE-99 (Solar and Heliospheric Interplanetary Environment)
Joint CEDAR-GEM-SHINE Sessions
Workshop on Auroral Plasma Dynamics: Akebono Ten Years Later
SCOSTEP Meetings in England
SPACE WEATHER EURO NEWS
Inter-Association Symposium JSA06: Space Weather Forecasting and Effects
First Announcement 2nd PAPCO Data Analysis Workshop
First Announcement for Cluster II Workshop
Third Announcement International Workshop on Radio Methods for Studying Turbulence
URSI/COSPAR International Reference Ionosphere Workshop
Ninth Workshop on Technical and Scientific Aspects of MST Radar (MST9)

INTERNATIONAL COUNCIL FOR SCIENCE (ICSU)
President: W. Arber
Secretary General: H. A. Mooney
Executive Director: J. F. Stuyck-Taillandier
ICSU Secretariat, secretariat@icsu.org
http://www.icsu.org

SCOSTEP SECRETARIAT
http://www.ngdc.noaa.gov/stp/SCOSTEP/scostep.html
Scientific Secretary: J. H. Allen, Program Assistant: C. M. Hanchett
c/o NOAA/NGDC, 325 Broadway, Boulder, Colorado 80303
Telephone (1 303) 497-7284, Fax (1 303) 497-6513, email: jallen@ngdc.noaa.gov
Publication Coordinator: Belva Edwards, C, bmedward@staff.uiuc.edu

SRAMP STEERING COMMITTEE
Chairman: D. N. Baker, baker@orion.colorado.edu
Members: S. Basu, B. J. Fraser, E. Friis-Christensen, Y. Kamide, H. Koskinen, A. H. Manson, H. Matsumoto, P. Newman, G. Ya. Smolkov, ex officio: J. M. Forbes, S. Fukao, M. Hagan, V. N. Obridko, G. Shepherd, R. A. Vincent, S. T. Wu

EPIC STEERING COMMITTEE
http://www.kurasc.kyoto-u.ac.jp/~epic
Co-Chairmen: S. Fukao, fukao@kurasc.kyoto-u.ac.jp, R. A. Vincent, rvincent@physics.adelaide.edu.au, J. M. Forbes, forbes@zeke.colorado.edu
Members: M. A. Abdu, L. Gray, A. Matthews, R. F. Woodman, H. Wiryosumarto

SRAMP SUBGROUP: SPACE WEATHER
http://aoss.engin.umich.edu/intl_space_weather/sramp/
Chairman: H. Koskinen, hannu.koskinen@fmi.fi
Members: D. Boteler, J. K. Chao, J. Kozyra, R. Schwenn, X H. Singer, T. Tanaka, O. Troshichev, P. Wilkinson.

ISCS STEERING COMMITTEE
http://cspar.uah.edu/www_root/ documents/iscs/
Co-Chairmen: S. T. Wu, wus@cspar.uah.edu, V. N. Obridko, obridko@lars.izmiran.troitsk.su
Members: T. Kosugi, P. K. Manoharan, B. Schmieder, M. A. Shea, S. Tsuneta, T. Watanabe

The SCOSTEP Secretariat invites contributions of information about publications or databases of special interest to scientists involved in the range of solar-terrestrial disciplines that comprise SCOSTEP and its programs. In general, we do not have time or opportunity to review whole works, but will rely on the involvement of contributors with related research or monitoring of STP phenomena. Probably, it will be best if contributions from Working Groups are sent through the Chairs/Co-Chairs of the Projects. At the least, they should receive a copy of the materials.

Editor's Note: Please refer to the Meeting Report in International SCOSTEP Newsletter, Vol. 1. No. 4, December 1998 (pages 4-5.) Joe Allen, SCOSTEP Scientific Secretary, wrote this very complimentary review of the meeting and the Proceedings publication which documented it. The principal meeting organizer was Prof. Y. Kamide and he was co-Editor of the Proceedings. However, he did not write the review although, unfortunately, his name was inadvertently shown at the end of the article. I apologize for any appearance that Prof. Kamide may have been the source of this review. The admiration for the Proceedings was clearly expressed by Joe Allen.

EPIC (Equatorial Processes Including Coupling) is one of four post-STEP programs sponsored by SCOSTEP. The equatorial region is the source of many unique atmospheric processes that couple the entire atmosphere vertically from the bottom to the top and horizontally from the equator to the poles. Despite its importance for global change, however, the equatorial atmosphere is not well studied and its coupling processes are poorly understood. The overall scientific objective of EPIC is to understand equatorial processes on all spatial and temporal scales occurring in the middle atmosphere and upper atmosphere/ionosphere, as well as their vertical coupling with atmospheric regions above and below. Coupling in the horizontal with the atmosphere/ionosphere at extratropical latitudes and between regions around the equator also needs to be studied.

During the SCOSTEP-sponsored MAP (1982-85) and STEP (1990-97) periods, several groups pioneered observational and theoretical investigations concerning these processes. However, there has been very little integration of these investigations because of the lack of core international institutions in equatorial and tropical regions dedicated to that task. EPIC should become the core program for studies of coupling processes in the equatorial atmosphere/ionosphere.

EPIC will operate during the period 1998-2002. It will be chaired by Prof. S. Fukao in collaboration with Co-chairmen of Dr. J. M. Forbes and Dr. R. A. Vincent. The program is composed of three working groups:

The EPIC Steering Committee is formed by the above-mentioned scientists and Drs. L. Gray, R. F. Woodman, and H. Wiryosumarto.

The first EPIC business meeting was held in Uppsala, Sweden during the General Assembly of the IAGA (International Union of Geodesy and Geophysics) on August 6, 1997. At the meeting the EPIC Steering Committee recognized the necessity of motivating diverse science communities to work toward an interdisciplinary goal of interest. It was decided to adopt the following theme, which is related to almost all scientific questions raised to date, and can be pursued with the collaboration of all members: Convective Processes and Influence on the Atmosphere-Ionosphere System. Later an informal gathering was held in Taipei, Taiwan, during the AGU/Western Pacific Geophysics Meeting on July 22, 1998.

After the meeting in Uppsala the Chair started an EPIC homepage, which can be accessed by the following address: http://www.kurasc.kyoto-u.ac.jp/~epic.

A description of the project and information on EPIC and its related activities are available from the homepage. In order to improve communication for the project, the following e-mail groups have also been established Steering Committee: epic-sc@kurasc.kyoto-u.ac.jp Members: epic-wg@kurasc.kyoto-u.ac.jp .

As discussed at the meetings, it was agreed that EPIC should be closely synchronized with various related experimental campaigns. In the western Pacific region, for example, there are ongoing programs such as GAME/GEWEX (Asian Monsoon Experiment/Global Energy and Water Cycle Experiment), BIBLE/IGAC (Biomass Burning and Lightening Experiment/International Global Atmospheric Chemistry), PREASA (Pacific Region Equatorial Anomaly Studies in Asia), and WestPac (Western Pacific Network.) There are also a number of satellite missions related to EPIC: TRMM (November, 1997), ROCSAT (Early 1999), TIMED (May, 2000), and ADEOS2 (Fall, 2000.)

It is unfortunate that little organized effort has yet been initiated for other matters addressed at the Uppsala meeting. No doubt, the most urgent is to have a kick-off meeting as soon as possible to discuss coordination of EPIC activities. Thus, the Steering Committee has decided to hold an extended EPIC Steering Committee meeting in Hawaii during March 15-17, 1999. It was also decided that an EPIC session will be included in the IAMAS/ICMA-IAGA Div. II joint symposium, which will be held during the IUGG meeting in Birmingham, England on July 19-30, 1999. Also planned is an EPIC symposium in 2000, though details are not yet decided.

In order to improve EPIC activities, the Steering Committee is keen to have any advice and suggestions from anyone interested in this program.

1. The EPIC Steering Committee (SC) has recognized the necessity of motivating diverse science communities to work toward an interdisciplinary goal of interest, and decided to adopt the following theme, which is related to almost all scientific questions raised before, and can be pursued with the collaboration of all members: Convective Processes and Influence on the Atmosphere-Ionosphere System .

2a. Initiate a series of "intensive observation period (IOPs)" synchronized with various satellite missions such as TRMM, TIMES, CRISTA, and ROCSAT.
2b. Organize workshops and symposia at suitable intervals. The EPIC SC will propose an IAMAS/ICMA - IAGA Div. II joint symposium to IUGG'99.
2c. Collaborate with other post-STEP programs.
2d. Encourage EPIC science in developing countries.
2e. Outreach, such as education, promotion of societal benefits, and documentation of results and techniques like the MAP Handbook series.

3a. To set up the following three interdisciplinary Working Groups as the Task Force for promotion of EPIC:
- Dynamical Coupling
- Electrodynamical Coupling
- Chemical Coupling
Originally, the Chair proposed to set up five working groups including: Modeling/Data Assimilation and Network/Data Archiving. However, these two working groups are closely related to the above three and have been decided to be merged. The Chairpersons for the three working groups are J. M. Forbes, M. A. Abdu, and A. Matthews, respectively.
3b. To recommend that R. A. Vincent act as the SCOSTEP representative on the SPARC-SSC and S. Fukao be the ex-officio representative on SRAMP.
3c. To create an EPIC web site by RASC Kyoto University.

1. The Chair reported the current status of EPIC to the SCOSTEP Bureau meeting held in the National Central University at Chung-Li, Taiwan, on July 19, 1998.

2. An informal gathering was held in the Taipei Convention Center during the AGU/Western Pacific Geophysics Meeting in Taipei on July 22, 1998. The Chair reported current status of EPIC and approximately twenty participants exchanged their views.

1. The Chair has honestly to confess that very little has been done so far except that the first version of EPIC home page is now available on his website at http://www. kurasc.kyoto-u.ac.jp/~epic and also, relevant e-mail addresses were made available:

2. An organized effort has not yet been initiated for other matters which were requested at the Uppsala meeting. No doubt, the most urgent matter is to have a kick-off meeting as soon as possible to discuss coordination of EPIC activities. Thus, the Steering Committee has decided to hold an extended Steering Committee meeting of EPIC in Hawaii during March 15-17, 1999. The Steering Committee is keen to have any advice and suggestion that provide direction of EPIC.

3. Personally, the Chair has been keeping in contact with the concerned scientists of satellite missions TRMM (November 1998), TIMED (May 2000), CRISTA (Space shuttles), ROCSAT (December 1998), and ADEOS2 (Fall, 2000.) EPIC should organize collaborative campaign observations with these satellites.

4. Also, we are aware that various campaigns such as GAME, BIBLE, PRESA, and WestPac are going on in the Western Pacific sector. Many similar campaigns may be conducting in other sectors. It is planned by R. A. Vincent to organize a space-supported campaign Convection Excited Gravity Wave Experiment(CEGWE) during November 2000 to November 2001. EPIC should make efficient links with these efforts.

5. No doubt, modelings are crucially important to connecting fragmental observational data, and making a complete concept of Convective Processes and Influence on the Atmosphere-Ionosphere System.

6. The Chair is keen to know what kinds of activities which might have a link with EPIC are going on in the equatorial regions.

The ISCS Working Group 2 Web pages have been updated to include the topics of large-scale chains and numerical modeling, by Chertok and Podgorny, respectively. The rest of the text has been updated. So, the use of the ISCS framework is growing. I have had a couple of other groups approach me about inclusion and could add a topic or two in the near future. S.T., you might like to add something to the Numerical modeling bit - such as a link to any site you have. Don, you may have something to add to the site as well.

Of major importance for Working Group 2 are meetings in The Hague (EGS) and Birmingham (IUGG), this year. Two specific sessions are being advertised. For the EGS session (session ST12.02 on CMEs) the ISCS is listed as a co-sponsor. We have some good abstracts submitted.

This is a report on the activities of SCOSTEP (Scientific Committee for Solar-Terrestrial Physics) for the period 1996 - 1999. SCOSTEP is a scientific committee of the International Committee of Scientific Unions (ICSU) and is responsible for; 1) the conduct and sponsoring of international meetings in the scientific area of solar-terrestrial physics and 2) the coordination and organization of international scientific programs in solar-terrestrial physics. The substance of this report was extracted from material generously made available by J. H. Allen, the Scientific Secretary of SCOSTEP.

In August 1997 the 9th Quadrennial Solar-Terrestrial Physics (STP) Symposium was held in Uppsala, Sweden, jointly with the IAGA 8th Scientific Assembly and IAMAS-MAC scientific sessions. The Symposium was highlighted by review sessions in the discipline areas of the six Working Groups of the SCOSTEP Solar-Terrestrial Energy Program (STEP), a seven-year-old program that ended in December 1997. Approximately 300 participants daily attended the week-long Symposium. The site of the next Quadrennial STP Symposium in 2001 has not yet been determined. Leading candidates at this time are Boulder, Colorado (USA) and Innsbruck, Austria, with Hanoi (site of IAGA's 9th Scientific Assembly in 2001) a less likely choice.

At the Uppsala Symposium, SCOSTEP helped organize a special evening session for consideration of international space weather issues. Approximately 500 participants from the international ST community attended the discussions. A key result of this special session was a request to SCOSTEP from the participants to lead an oversight effort to provide a coordinated international space weather program. This effort has become one of the major post-STEP activities undertaken by SCOSTEP.

As mentioned above, SCOSTEP's large, international scientific program, STEP, came to its scheduled end in December 1997. Its seven-year history was marked with numerous satellite launches, new ground-based observations, and the participation of thousands of scientists in hundreds of international campaigns and monitoring efforts to record significant aspects of the integrated Sun-Earth system. It has resulted in a greatly expanded understanding of the Sun-Earth system that is directly impacting the developing international Space Weather Program. Financial support from several participating countries allowed an international STEP newsletter to be assembled by SCOSTEP and distributed to some 4000 scientists worldwide. The December 1997 newsletter signaled the official end of STEP.

Four new post-STEP programs have begun five-year terms. They are: I) STEP Results, Applications, and Modeling Program (SRAMP); II) Equatorial Processes Involving Coupling (EPIC); III) Planetary Scale Mesosphere Observing System (PSMOS); IV) International Solar Cycle Study (ISCS). Organizational activities (workshops, commun-ications, meetings of opportunity, etc) have begun in all four of these programs. The SCOSTEP activity in the international space weather arena is at the present time included as an designated sub-element of the SRAMP effort. Activity and interest in the space weather area is rapidly increasing. It is this reporter's opinion that the international space weather work will evolve into a major SCOSTEP program in its own right.

SCOSTEP continues to participate directly in the ICSU Committee on Science and Technology in Developing Countries (COSTED). SCOSTEP plays a unique role in this area because of its organization and coordination of major international scientific programs dealing with the Sun-Earth system and its effects on the world's populations. It routinely invites and encourages the participation of developing countries in these international programs. As a result of this experience SCOSTEP will be an important contributor to the capacity building program being initiated by ICSU.

The results of the external review of ICSU has stimulated SCOSTEP to begin a detailed evaluation of its long-term future. The SCOSTEP Bureau has formed a special sub-group specifically to look into this issue. SCOSTEP's goals, its relation to other international solar-terrestrial organizations, and the unique characteristics of its contributions to the international scientific scene will be considered in detail. While not stated explicitly, it is expected that the sub-group will discuss the relevance of SCOSTEP's goals and activities to its 29 subscribing Adherents. Plans are to have the sub-group report at the next Bureau meeting at the IUGG General Assembly in Birmingham, July 1999. This Bureau meeting will be very important for not only will SCOSTEP's long-term future be discussed, but a new President and Vice-President will be elected to lead the organization into the next millennium.

SCOSTEP maintains an extensive WWW homepage on the internet. The address is http://www.ngdc.noaa.gov/ stp/SCOSTEP/scostep.html. It has proven to be very convenient for easy access to SCOSTEP's organization and activities. All interested parties are encouraged to access the site and communicate with the SCOSTEP secretarial offices.

TITLE: Opportunities for Collaboration between American and European Scientists (see below for a sample opportunity.)

ABSTRACT: By the end of February 1999, the Fifth European RTD Framework Program (FP5) which provides funding to European researchers will be initiated. This program will provide USOA subscribers with a wealth of opportunities to form collaborative research partnerships with European scientists.

Once the European Commission starts to publish Requests For Proposals, U.S. Opportunity Alert will send out new announcements every Friday to you for a thirty-day introductory period. Upon completion of this period, you will be given the chance to upgrade your subscription to our premium service, U.S. Opportunity Alert (http://www.usalert.com), to ensure that you continue to receive these announcements as well as those from corporations, foundations and every major agency within the federal government.

To learn more about how you can take advantage of the valuable research opportunities made available by this new European Union program, we have provided two important documents:

U.S. Opportunity Alert is constantly expanding to provide you with the most comprehensive and targeted research and education funding opportunity alert service in the nation. To register for U.S. Opportunity Alert, please visit http://www.usalert.com/foa.asp

Today's Transatlantic Information Service - a joint service provided by RAMS and KoWi - has found 1 new opportunity or information that match your USOA personal research interests profile.

TITLE: EU - USA: Cooperation in Higher Education and Vocational Education and Training - 4th call for proposals

ABSTRACT: In 1995, the European Community and the United States of America concluded an agreement for cooperation in higher education and vocational education and training. On January 12, 1999 the 4th call for proposals for joint projects was published under this program. The program is a small-scale initiative supporting a limited number of original projects which will center on transatlantic student mobility.

Participation requirements: Each joint consortium must contain a minimum of three active partners on each side, including at least two partner higher education or training institutions on each side located in different Member States of the European Community and different states of the USA including Puerto Rico. (For the USA, the two institutional partners may come from autonomous campuses in the same state in exceptional circumstances.) The third and subsequent partners may be other education and training institutions or other relevant organizations (e.g., businesses, NGOs, chambers of commerce, research institutions.) Funding will be provided for a maximum of 3 years. European partner will be funded by the European Commission, DG XXII(Education) and may expect to receive approximately 100,000 Euro per project. US partner will be funded through the FIPSF and may expect to receive $130,000 per project. Further information is available at: http://europa.eu.int/en/ comm/dg22/dg22.html.

KoWi - KEYWORDS (based on GRANTS THESAURUS (c) RAMS): 0500000 Education SI/ps:53951.

Genesis Software specialises in scientific radar instrumentation and software for observing the Earth's atmosphere and for observing meteors as they enter the atmosphere. Our principal products include Meteor Radar Systems, Atmospheric Radar Systems, Ionospheric Radar Systems, Wind Profilers, Radar Data Acquisition Systems and associated software. New developments in these areas follow.

We produce a wide range of MF/HF and VHF atmospheric radar systems and more than twenty-five atmospheric radar systems installed worldwide incorporate our systems. Extensive information on these products can now be found on our web site at: http://www.gsoft.com.au/ products.html.

Of particular interest is our new generation of HF/VHF atmospheric radar systems and sub-systems. Based on our many years of experience, this new product range provides unprecedented performance and ease-of-use for ground-based observations of the atmosphere. Information on HF/VHF atmospheric radar systems can be found at: http://www. gsoft.com.au/vhf.html.

For HF/VHF observations of ionospheric phenomena, we offer broad-band, frequency agile systems covering the 10 to 60 MHz frequency band. New information on these extremely flexible systems is now available on our web site at: http://www.gsoft.com.au/ionospheric.html.

Our SKiYMET meteor radar is becoming widely deployed both for astronomical and for atmospheric applications. Last

November, several SKiYMET systems undertook highly successful observations of the Leonid Meteor Storm. SKiYMET systems observing the Leonids included a triple-frequency system operating in northern Australia and a VHF system in southern Australia. The unique triple-frequency system operated simultaneously on three different frequencies in the HF/VHF band. Several new systems will be installed this year and these include systems specifically for MLT observations, such as a system to be deployed at Kiruna in northern Sweden. Genesis Software operates its own SKiYMET system on a continuous basis at its radar research station in southern Australia. In the near future real-time results from this system will also be available on our web site.

Please see the following pages on our web site for information on the SKiYMET radar system and for news items: http://www.gsoft.com.au/skiymet.html

Please don't hesitate to contact us for further information on any of the above at genesis@gosft.com.au. If you are visiting Australia, we would be very pleased to receive your visit and for you to view our SKiYMET meteor radar system at our radar research station.

The Solar Light Company produces a line of "affordable, accurate" measuring radiometer/photometers in the PMA**** series. They also market solar simulators in the 1,000 watt class. Their Microtops units are calibrated annually against NOAA's ozone measurements from the Mauna Loa, Hawaii, observatory. They also conduct materials testing for durability, UV transmission, and other factors. Their e-mail address is: info@solar.com; website is: www.solar.com; or write to 721 Oak Lane, Philadelphia, PA 19126-3342, USA; or telephone (215)927-4206 or FAX (215)927-6347.

ICSU's Standing Committee on Freedom in the Conduct of Science has published a new edition of the "Blue Book" on the Universality of Science and requests widespread distribution of information about the availability of this important international document. The "Preamble" states: "The International Council for Science (ICSU), on behalf of the scientific communities of the world, affirms the universal nature of science and the fundamental right of scientists to associate freely with international scientific activity." They cite ICSU Statute 5: "5. In pursuing its objectives in respect of the rights and responsibilities of scientists, ICSU, as an international non-governmental body, shall observe and actively uphold the principle of the universality of science. This principle entails freedom of association and expression, access to data and information, and freedom of communication and movement in connection with international scientific activities, without any discrimination on the basis of such factors as citizenship, religion, creed, political stance, ethnic origin, race, color, language, age or sex. ICSU shall recognize and respect the independence of the internal science policies of its National Scientific Members. ICSU shall not permit any of its activities to be disturbed by statements of actions of a political nature."

prerequisite to the pursuit of scientific activity and that the unrestricted flow of scientific ideas and information exchange among scientists is critical to the advancement of science."

"ICSU observes the fundamental policy of universality of science based on the rights of scientists throughout the world to participate in international scientific activity without any discrimination on the basis of citizenship, religion, creed, political stance, ethnic origin, race, colour, age or sex. ICSU also has a well established non-political tradition which is central to its character and operations. ICSU exists to promote active cooperation in scientific matters among scientists from all parts of the world, regardless of the political structure of governments and, therefore, does not permit any of its activities to be disturbed by words or actions of a political nature. In accepting and implementing the principle of the universality of science, and in assuring the non-political character of its affairs, ICSU is able to pursue the rights of scientists to associate on a non-discriminatory basis with international scientific activities."

After an introduction that describes the historical position of ICSU on this topic, the Blue Book contains sections on the Free Circulation of Scientists, on Advice to Organizers of International Scientific Meetings, on Movement of Scientific Materials, on Freedom in the Pursuit of Science, and on International Human Rights Law.

Appendices are included on ICSU, the ICSU Statement on Freedom in the Conduct of Science, ICSU Resolutions from 1958-1993 on this topic, a Summary of International Human Rights Law, and a list of ICSU Members and Committees associated with this subject.

Additional copies of the "Blue Book" are available from the ICSU Secretariat in Paris and the SCFCS Secretariat in Berne, Switzerland. Write to either: Swiss Academy of Sciences, Baerenplatz 2, 3011, Berne, Switzerland, or International Council for Science, 51 Boulevard de Montmorency, 75016 Paris, France. Also, requests can be submitted to: schindler@sanw.unibe.ch; or secretariat@icsu.org.

Dr. Roni Avissar, Editor of JGR Atmospheres, has agreed to support a special section of the JGR-Atmospheres devoted to the topic of the mesosphere inversion layer phenomenon (see the 1998 Fall Meeting AGU abstracts for SA-02) with a submission deadline of 1 June 1999. This Special Section will be published at the same time that the TIMED satellite will be launched into orbit and offers an opportunity to summarize our understanding before these new expected measurements. Satellite limb scanners and ground-based lidar observations have shown that the mesosphere inversion layers can extend over areas as large as several million square km and persist for weeks to months. Turbulent gravity wave heating associated with breaking gravity waves, atmospheric tides, chemical heating, and gravity wave tidal interactions have all been suggested as the source of the inversion layers. This Special Section of JGR-Atmospheres is being organized to feature the most recent research on the phenomenon. Original papers are solicited featuring new observational data, theoretical studies, and model calculations which provide increased understanding of the mechanism(s) which lead to the formation of the persistent temperature inversions in the middle atmosphere and which improve the characterization of the phenomenon.

The expected publication date is May 27, 2000. Original manuscripts for this issue, prepared according to the standard JGR-Atmosphere guidelines, should be submitted to:

Professor Roni Avissar, Editor, JGR-Atmospheres
Department of Environmental Sciences
Cook College, Rutgers University
14 College Farm Road, New Brunswick, NJ 08901-8551
e-mail jgr@gaia.rutgers.edu phone 732-932-3482

The Laboratory of Inertial Geodetic Systems (LIGS) issued a new book by Dr. Oleg Salychev, Professor at the University of Calgary (Dept. of Geomatics Eng.) and Bauman Moscow State Technical University, Inertial Systems in Navigation and Geophysics. ISBN 5-7038-1346-8. Hard cover. 360 pages, 50 figures, English.

The advances made during the past decade in the use of inertial technology for navigation and the geosciences are described. The reader will get a first-hand account of new application areas and current research developments, as well as a solid introduction into the principles of inertial navigation, the integration of inertial systems with the Global Positioning System (GPS), and the use of selected filtering methods for the processing of such data.

The applied aspects of inertial technology and estimation theory for the navigation, guidance and geosciences:

Price is $58.00 (Postage and Shipping included) Delivery by air mail. Discounts are available. For ordering information visit our site http://www.glasnet.ru/~ligs/ and http: //www.glasnet.ru/~ligs/newbook.htm. Or request an order form from Dr. Vladimir Voronov at ligs@glasnet.ru

The report with reference, Analysis of Freja Charging Events: Modelling of Freja Observations by Spacecraft Charging Codes, by A. I. Eriksson, L. Wedin, J.-E. Wahlund and B. Holback, ESA contract No. 11974/96/NL/JG(SC), SPEE-WP120-TN, December 1998, is now available on the www at the address: http://www.estec.esa.nl/wmwww/wma/ esa_contract.html (cf also http://www.geo.fmi. fi/spee/ .)

As an accompanying measure of the development of the Space Environment Database and Analysis Tools (SEDAT), a meeting of experts was held at BIRA-IASB, Brussels, Belgium, on 14 January to discuss a number of critical issues, in particular: data correction, data formats, inter-operability and data interchange that can determine the ultimate capabilities and range of application of SEDAT in the context of several on going space database projects in Europe.

The SEDAT project is intended to develop a new approach to the engineering analysis of charged-particle environments and their effects (cf also http://www.wdc.rl.ac.uk/sedat/.)

The homepage is automatically updated with plots and data for the previous day's activity as well as pointers to earlier, archived predictions (at the end of the page.) There are two GIF files per day. The first displays the PC index and the predictions from it, and the second compares them with ACE-based predictions.

The "Online Transmission Facility" (OTF) of JASTP is now accepting papers in flexible electronic formats. Files may be compressed or uncompressed and transmitted via ftp, the worldwide web, or e-mail. JASTP is an international journal that publishes peer-reviewed papers in the areas of solar, magnetospheric, ITM, and atmospheric physics. JASTP has no page or color figure charges (with acceptable color separations) and provides authors with 25 free reprints. Publications in the Journal can incorporate peer-reviewed short movies, animations, and ancillary data sets. More information on recent changes to JASTP can be found at http://www.sprl.umich.edu/JASTP.

Attendees: Eric Priest (chair), Marcello Coradini (secretary), Claudio Chiuderi, Luc Dame, Richard Harrison, Olav Kjeldseth-Moe, Oskar von der Luhe, Eckart Marsch, Jean-Claude Vial. Apologies from Pino Tondello.

He reminded them of the Tenerife consensus whereby the community agreed to recommend a Solar Orbiter concept as the next major European solar and heliospheric mission and to encourage European involvement in the American Stereo and Probe missions and development of interferometric techniques. The meeting congratulated Bob Harris on a speedy and well-constructed proceeding of the Tenerife workshop (ESA SP 417 A Crosssroads for European Solar and Heliospheric Physics, ed. ER Priest, F. Moreno-Insertis and RA Harris (1998)). The details of the presentations, the discussion and the consensus can be found in that publication.

Since then many events have occurred. The consensus resolution of the Workshop has been presented to ESA's SSWG and SSAC where it was received very favourably. The SSWG agreed that the SPPG should continue in existence in order to help evaluate the solar and heliospheric response to the expected call for ideas next year and to monitor and encourage the follow-up.

In early June, Eric Priest met George Withbroe in Washington and described the Tenerife ideas. George Withbroe was enthusiastic about the idea of European involvement in stereo and probe and American involvement in an orbiter. He was particularly keen on the idea of an orbiter that could view the solar poles and could link up with whatever stereo spacecraft were in the ecliptic at the time.

A meeting took place in Paris on July 24 between R. Bonnet and W. Huntress and their advisors at which the possible ESA and NASA programmes for solar and heliospheric physics were discussed.

A workshop was held in Lindau 26-29 October specifically to discuss solar and heliospheric physics with a Near-Sun Orbiter.

The Tenerife consensus was then taken as a starting point and the aim of the present meeting was to see how the Orbiter concept was developing and how to encourage European involvement in future stereo, probe and interferometric opportunities.

M. Coradini described this meeting which was also attended by M. Huber. There was a constructive reaction from NASA. In addition at the Inter-Agency Consultative Group meeting in Berne, there was a presentation of the Tenerife ideas and general acceptance of them.

The whole ESA Science programme is evolving. Mars Express had stimulated new methods of working in a cost-effective way with a realistic costing of missions. Flexible slots of about 170 MAU (F-missions) and technology-testing

(Smart) missions are complementing the cornerstones. The Executive agrees on the need for a solar physics mission in the programme and so a future F-mission is highly likely to be such a mission before 2010 since there is international coherence in this idea and the natural next solar system mission is a solar and heliospheric one.

If the level of resources remains constant, we should aim for a mission in the 2006-2008 time-frame. It was therefore important to express the scientific goals of an orbiter in a more sparkling way so as to appeal more generally. The four Solar Physics representatives in the SSWG will have responsibility to advocate the identified mission and to convince the SSWG to endorse the idea of a Solar Physics mission in the 2006-2008 time-frame.

E. Marsch described the talks and discussions that took place at this meeting, including the various mission scenarios and scientific goals.

It was agreed that Mercury should not be part of the science goals since the payload will be extremely limited, and it would dilute the solar mission and the planned Mercury cornerstone.

The main scientific rationales should be the unexplored region around 30 solar radii and a polar vantage point of at least 40 degrees. In addition, there was the correlation of in situ and remote observations, high resolution and proximity to the Sun. Long-term co-rotating observation of the same region would be attractive with a disentangling of spatial and temporal effects. The origin of the slow solar wind with correlated optical and particle observations would be of high value. Others would be the first polar magnetograms and high-resolution optical observations. In addition, stereo observations with a near-Earth satellite may be possible.

For possible payloads, the in situ instruments are well-defined and feasible, but the remote instruments would need compact innovative designs. Surviving 50 solar constants and a strategy for data storage and telemetry would need careful consideration.

One option was to have three stages - (i) going to a solar orbit with a 30 solar radius perihelion, (ii) inclining the orbit to 30 or 40 degrees and (iii) lowering the orbit to say 10 solar radii. Phases (ii) and (iii) would be very important for the science (being complementary to the solar probe and stereo and providing a "sparkling" aspect.) Another option may be to tilt the orbit first and then to approach to 30 solar radii.

Some of the Orbiter conceptual discussion was based on the Russian Interhelios concept, but the Committee agreed to proceed on the basis of a purely European mission (with Russian scientific involvement and input) rather than a joint European-Russian mission in view of the financial uncertainties in Russia.

There are a variety of scientific goals and several different orbit possibilities, which have not all yet been studied in detail. The Committee agreed therefore to ask R. Harrison (together with E. Marsch, P. Cargill, O. Moe and C. Chiuderi) to produce a report of the different possible mission scenarios with their sets of science goals and their orbits. This would be used to initiate a small ESA study of the orbits in order to determine the feasibility of such mission scenarios.

J.C. Vial reported on the status of the mission and of European involvement. He described the science issues and compared the US and Ramses proposals. The US Probe is aiming for a launch in Feb 2007, two passes (the first in 2010 and the second in 2015), a payload of 20 kg, power of 16 W and TM of 100 kbps. The AO will be issued early in 1999 and it would be open for foreign competition. Proposals may be for individual or groups of instruments. There is likely to be a PI for the in situ instruments and another for the remote instruments. There would be a probe session at the AGU in December (this indeed took place.)

There is strong European interest in the US Probe and strong technological interest at CNES. It was suggested that the best way for European scientists to be involved was to become parts of mainly-US consortia.

R. Harrison gave an account of the current status and of European involvement. A pre-phase-A study is in progress at the Johns Hopkins University and the AO is expected early in 1999. The JHU study is considering launch opportunities in 2002 or 2004 but the former appears to be unrealistic. One problem in the current study is in the design of a high-gain antenna configuration which would work for all points in the orbit of the spacecraft. One option would be to have both spacecraft lagging Earth, but this was undesirable since we would like good observation of the western limb region. Because of the ESA-NASA reciprocity agreement, Europeans can respond to the AO. Several European scientists have been closely involved in the mission concept study phase (e.g., Volker Bothmer, Len Culhane and Richard Harrison) and have become active members of US-led instrument consortia.

L. Dame described the laboratory research and development progress. Soon there will be a solar test of the whole SOLARNET three-telescope co-phased set-up at Meudon. His PICARD project is an approved CNES micro-satellite mission to be launched in 2002 to measure the solar diameter, differential rotation and the solar constant and to seek for g-modes (through diameter variations in the UV.) PICARD will develop and use the highly stable carbon-carbon structures and SiC mirror technologies that SOLARNET aims to use. He would like to see SOLARNET accepted on a CNES Proteus platform (2006-2008 framework) with an ESA launch for the Smart-3 technology mission, noting that interferometric technologies and stable structures approaches are of interest for IRSI/DARWIN.

O. von der Luhe agreed to write a report on the progress of Dame's interferometry project and to make recommendations about its future development.

The VII Symposium on Solar-Terrestrial Physics for the scientists of Russia and former USSR countries was held during December 15-18, 1998, at IZMIRAN (Troitsk, Moscow Region.) The Symposium was organized by the Scientific Council on Solar-Terrestrial Physics of the Russian Academy of Sciences ("Sun-Earth" Council), Astronomical Society, and IZMIRAN under the sponsorship of the Russian Foundation for Basic Research (RFBR), Russian Ministry of Science, and INTAS. The scientific program of the Symposium covered the main fields of solar-terrestrial physics. By decision of the ISCS Steering Committee the Symposium was assigned the status the Regional Symposium on ISCS (International Solar Cycle Studies.). The first half of each day was devoted to plenary sessions where 12 invited review lectures on the main STP topics were delivered. In the afternoon, 5 parallel topical sessions were held at IZMIRAN:

A number of associated meetings were also held during the Symposium. These were:

The total scientific program comprised 12 invited review lectures, 123 oral presentations and about 120 poster papers. Thanks to the financial support from RFBR, INTAS, and the Ministry of Sciences, the Symposium was held at a high level of organization. The Organizing Committee rented the City Youth Hall of Troitsk for the plenary sessions, hired buses to bring participants from Moscow to Troitsk and back, acquired the necessary projection and other facilities and waste materials, prepared for publication and issued the booklets of Program and Abstracts of the submitted papers. More than 140 participants got financial support in one or another form. As a result, more than 200 scientists representing 45 scientific institutions from all parts of Russia (including Siberia and the Far East), from a number of the former USSR countries (Ukraine, Georgia, Kazakhstan, and Tadzhikistan), as well as from Bulgaria and Poland, could attend the Symposium in spite of a hard economic situation. Some of the submitted reports were prepared in co-authorship with the colleagues from the USA, France, Poland, Slovakia, Hungary, and other countries.)

The Solar Section held 4 afternoon sessions with 38 oral and over 50 poster presentations. Besides, 3 invited review lectures on solar topics were delivered at the plenary sessions: Large-Scale Solar Activity by V.N.Obridko, InterHelios space mission - a Solar and Heliospheric Observatory by V.N.Oraevsky and V.D.Kuznetsov, and Precise Time Scales of 10,000 Years to Study the History of Cosmic Ray Variations by V.A.Dergachev. The scientific program of the Section was comprised of the following topics:

The results of optical and radio observations of the Sun both at ground-based observatories, and on Russian and foreign satellites were widely discussed within the listed topics. Along with traditional studies of isolated phenomena of solar activity active regions, flares, filaments, and coronal mass ejections, a large number of papers were devoted to global events due to cyclic variations of the large-scale solar fields. Lately, it became obvious that practically all active solar events are in some or other way associated with global large-scale processes. Variations with a period of ~5-6 and 2-3 years have been revealed in addition to the 11- and 22-year variations. The origin of quasi-annual and shorter-period variations (~150, ~ 80-100, ~ 40 days) was discussed. Some authors reported an asymmetry in rotation characteristics and various active manifestations (both in the photosphere, and in the corona) between the Northern and the Southern hemispheres. The asymmetry was shown to change its sign from cycle to cycle. The ambiguity in understanding the global processes in the Sun is one of the main causes of low reliability of the activity cycle forecast. Even now, at the growth of the cycle, we still cannot predict the level of activity at the maximum or the date of the latter with an accuracy better than 0.5-1 year. The forecasts of the Wolf numbers issued by various authors differ by more than 50. The most interesting results reported at the topical sessions were as follows:

An up-to-date concept of solar activity, based on the entire complex of phenomena and structures in the local and global magnetic fields in the Sun, was developed using ground-based data from Russian observatories, Stanford (USA), Kodaikanal (India), Nobeyama (Japan), as well as satellite observations on KORONAS (Russia), Yohkoh (Japan), SOHO (ESA), and TRACE (USA). According to this concept:

These results make it possible in prospect to conceive a physically consistent model of solar activity, including its forecast. For the first time, the scenario of intensive solar flares has been described in detail, including the analysis of variation of physical conditions from the onset up to the explosive phase and later. The scenario is based on the unique SSRT, NRN, Yohkoh, and Ha data on distribution and evolution of microwave, X-ray and optical radiations. The energy release is shown to occur in a confined region of closed magnetic configuration, whose location is determined by interaction of the coronal magnetic flux tubes. (The results were obtained at ISZF SO RAN and Nobeyama Observatory.) A cyclotron line was discovered in the spectrum of microwave radiation from the solar active region. Spectral polarization observations were performed on RATAN-600 using a 2-30 cm panoramic spectrum analyzer with a 5% frequency resolution. The source of the 8.5 cm narrow-band radiation was identified with the point source of radio emission at 1.7 cm, recorded at Nobeyama. It was shown that the observed line could be accounted for in terms of the thermal cyclotron radiation mechanism (at a frequency corresponding to the 3rd harmonic of electron gyrofrequency) from a compact source of dense hot plasmas in the coronal loop, whereas the enhanced radiation at 1.7 cm was due to the bremsstrahlung mechanism. The performed measurements and interpretations were used to determine physical conditions in the source. (The results were obtained at IPF RAN and SAO RAN.)

A number of multi-aerial VLBI experiments on stimulation of interplanetary plasmas by radio signals from space revealed the medium-scale "stringy" structure of the solar-wind plasmas existing in the form of narrow jets of irregularities mainly aligned with the solar wind direction. The jets were estimated to be 1.5-2 thousand meters across and more than 300 thousand km along. Within a particular "filament", the irregularities were approximately isotropic in direction and did not exceed 1000 km in size. (The result was obtained at NIRF.)

The Section had 3 afternoon sessions (on Dec. 15, 16, and 17, chaired by L.Kh.Shatashvili, K.G.Ivanov, and G.A.Bazilevskaya, respectively), where 22 oral and 25 poster papers were presented. Two invited reviews on this topic were delivered at plenary sessions: Review of the Present-Day State of Solar Wind Studies by I.S.Veselovsky and Heliosphere and Cosmic Rays by A.V.Belov.

Observational and theoretical aspects of long-term variations of the solar wind and interplanetary magnetic field were discussed in the papers by N.A.Lotova et al., T.V.Kuznetsova et al., V.I.Vlasov, I.S.Veselovsky et al., and Yu.R.Rivin.) Experimental data were used to analyze the structure of the solar wind sources and their manifestations in the heliosphere (K.G.Ivanov, T.E.Valchuk et al., V.G.Fainshtein.) Modeling topic was represented by a theoretical acceleration model of the solar wind from a polar coronal hole by Yu.V.Pisanko, numerical models of interaction of the trapped stellar ions with the solar wind by A.S.Lipatov et al., models of some discontinuity MHD structures by S.A. Grib. A number of papers were devoted to radio astronomic observations of interplanetary shock waves (V.I.Vlasov and V.I.Shishov) and small-scale turbulence in the solar wind (V.A.Alekseev et al.) and near the bow shock in the vicinity of the Earth (Yu.V.Tokarev et al.), carried out at Pushchino, Nizhny Novgorod, and Kharkov.

Some papers were submitted dealing with modulation effects in cosmic rays and their relevance to the structure of the heliosphere and the solar wind dynamics. The results of investigation of SCR were considered, including their spectra and anisotropy during some solar flares, spectrum variations associated with the Forbush effect, the role of SCR in atmospheric processes and in correlation between the solar activity and lethal pathologies. Since there is a correlation between the interplanetary magnetic field and galactic cosmic ray fluctuations, some authors suggested that the latter could be used to estimate conditions in the heliosphere (S.A.Starodubtsev, V.I.Kozlov, M.A.Bakhareva and A.V.Dmitriev, A.V.Belov et al., V.M.Dvornikov and V.E.Sdobnov.) The SCR and GCR variations were discussed in the papers by L.Kh.Shatashvili et al., M.A.Despotashvili et al., G.A.Bazilevskaya et al., G.Grigoryeva et al., M.A.Zeldovich et al., K.Kechkemeti et al., M.V.Alania et al., M.S.Kalinin and M.B.Krainev, V.P.Okhlopkov, Z.Kobilynski, E.V.Vashenyuk, V.M.Aushev and O.N. Kryakunova, A.K.Svirzhevskaya and N.S.Svirzhevsky, V.L.Yanchukovsky and G.Ya.Filimonov, V.G.Stolpovsky et al., V.E.Timofeev et al. The influence of the heliospheric current sheet on detachment of comet tails was discussed by N.Ya.Vanyarkha.

The probable relevance of the IMF sector structure to initiation of earthquakes was considered by L.Kh.Shatashvili. The paper by Yu.I.Stozhkov et al. was devoted to the role of cosmic rays in atmospheric processes, and the paper by N.N.Volodichev et al. to the relationship between seismic activity, lunar-solar tides, and the bursts of neutrino. V.V.Borog aroused great interest of the audience by describing a muon hodoscope-tomograph designed at the Moscow Institute of Physical Engineering and suitable for the study of dynamic processes in the Earth atmosphere and near-Earth space environment.

The solar and heliospheric space projects were considered by V.N.Oraevsky et al., I.I.Sobelman et al. (KORONAS-F mission ) and G.A.Efremov et al. ("Patrul-Strela" mission.)

Twenty-two oral and 14 poster papers were submitted at the topical sessions and 3 invited reviews were delivered at the plenary sessions Some aspects of the heliosphere-magnetosphere coupling by G.N.Zastenker, Nonlinear particle dynamics in the magnetotail by L.M.Zeleny, and On the sub-storm burst mechanist by Yu.I.Galperin.)

Most papers were based on earlier and recent experiments on Soviet and Russian spacecraft. The problems of particular interest were:

Twenty-eight oral and 31 poster papers were submitted at the topical sessions and 3 invited reviews were delivered at the plenary sessions: Atmospheric electric field as a source of variability of the ionosphere by S.A.Pulinets (IZMIRAN); Relationship of the ionosphere and thermosphere with solar activity by M.G.Deminov (IZMIRAN); Response of the Earth ozone layer to variations of the space factors by A.A.Krivolutsky (Central Aerological Observatory.) The main topics under discussion were:

Solar activity is known to affect all characteristics of the ionosphere. The channels of this influence are multiple and poorly understood. Therefore it is interesting to study relationships between the solar activity and ionospheric parameters. The data on solar X-rays and radio emission, Wolf numbers, occurrence rates of the F-scatter events and traveling ionospheric disturbances were analyzed to reveal pronounced periodicities of 2-4 and 4-6 years in all these characteristics. This implies a solar origin of quasi-biennial variations in the ionosphere (Vybornov F.I., Zyryanova M.S., Mityakov E.E. et al. - NIRFI.)

An important problem is to establish the cause of long-term variations in the ionosphere. It was shown that these variations could be due both to the human factors, and to cyclic variations in the level of solar activity (with a period of 100 years and more), in the occurrence of geomagnetic storms, and to the geomagnetic field secular variations. For example, the theoretically expected effects of human activity at certain longitudes in the F2 layer of the ionosphere are compatible with secular variations of the magnetic fields (Deminov M.G., IZMIRAN.)

Direct measurements of solar UV radiation are rare enough, because they can only be made on satellites. A new activity index was developed in terms of ionization in the ionospheric E-layer. The index determines the solar UV and X-ray fluxes, that form the ionosphere at those altitudes, from the measured E-layer critical frequencies. This will allow us to use the E layer as a detector of ultraviolet radiation (A.A.Nusinov, L.A.Antonova, V.V.Katyushina, IPG.)

The ionospheric disturbances associated with flare processes in the Sun and high-speed solar wind fluxes are of special interest, because they are the main source of radio blackouts. The joint analysis of flare-generated X-rays, E-layer critical frequencies, and high-energy proton fluxes shows that, at the same value of X-ray flux, the variations of critical frequencies are greater during "proton" flares (A.A.Nusinov, O.I.Prokopenko, IPG.) This allows the use of ionospheric data for diagnostics of hazardous radiation events. A new ingenuous mechanism was suggested and experimentally substantiated by V.A.Kuzmin, V.D.Sokolov, and I.P.Bezrodnykh (IKFIA SO RAN) to explain the influence of solar X-ray flares on the daytime high-latitude ionosphere. According to this mechanism, the X-ray flare results in the enhancement of the Eastern electrojet. This triggers the auroral particle precipitation, which, in turn, leads to modification of the ionosphere. A proton flare can cause noticeable changes in the ozonosphere (A.A.Krivolutsky, A.A.Kuminov, A.I.Repnev, Central Aerological Observatory.)

The data on variations of the ionospheric D region during geomagnetic storms are scarce, especially as far as the lower part of the D region is concerned. Midlatitude measurements by the method of partial reflections show that the electron density at altitudes below 75 km remains increased by several fold during 5-10 days after the storm (A.M.Gokov, Kharkov, Ukraine).

The analysis of the ionosphere in search for indicators and precursors of earthquakes has lately become the task of particular interest. The data on various ionospheric parameters (electron density, ion composition, temperature) combined with the earthquake preparation characteristics (e.g., increased content of radon) allow us to rightfully regard the electric field as one of the main causes of ionospheric variations before an earthquake (S.A.Pulinets, K.A.Boyarchuk, V.V.Khegai - IZMIRAN.) A joint analysis of time variations of the ionospheric parameters and the level of subsoil waters shows that the seismic precursors appear in the ionosphere at the final stage of preparation of earthquakes, i.e. as the cracking starts (N.D.Kvavadze, G.I.Melikadze, Z.S.Sharadze - Tbilisi State University.) The electric field excited in the ionosphere prior to major earthquakes may result in generation of acoustic-gravity waves (AGW) through the mechanism of Joule heating. While propagating in the ionosphere, these waves may cause noticeable changes far enough from the source. It is shown that the AGW effects in the ionosphere display a strong azimuthal anisotropy (V.V.Khegai, V.P.Kim - IZMIRAN.)

Lately, impressive results have been obtained concerning the dynamics of the atmosphere and its effect on the ionosphere. The middle atmosphere temperature, Tn, measured by optical and radiophysical rocket techniques during four cycles of solar activity, was analyzed to plot the annual mean profiles of Tn at the altitudes of 25-110 km. It was shown that (a) the character of height distribution of Tn changed significantly from the maximum to the minimum of a solar cycle; and (b) for the past 4 decades, Tn values at mesopause altitudes decreased by about 20 K, i.e., the trend in the long-term variations of Tn was high enough (A.I.Semenov - IFA RAN.) The energy balance in the lower atmosphere does not only depend on the supply, but also on the escape of energy. As the solar activity grows, the escape of energy from the lower atmosphere decreases due to the enhancement of a broad range of waves. Thus, at low solar activity, the global cooling of the lower atmosphere by 1 K may take about 100 years, which was the case during the Mounder Minimum in 1645-1715 (E.V.Kononovich - GAISH, N.N.Shefov -IFA RAN.)

Because of the complicated relationship between the dynamics of the ionosphere and the thermospheric circulation, the complex 3D models can be efficient for providing a self-consistent description of the upper atmosphere (Yu.N.Korenkov, V.V.Klimenko, V.V.Bessarab -ZO IZMIRAN.)

The method of incoherent scatter of radio waves is one of the powerful tools of ionospheric studies. It provides detailed information on the vertical component of ion drift velocity, on the electron (Te) and ion (Ti) temperatures, as well as on the Ne, Ni, Te, and Ti variations under naturally and artificially disturbed conditions (V.N.Lysenko, V.I.Taran - Institute of Ionosphere, Kharkov.) The results of observation of solar activity and tidal manifestations in the upper atmosphere by radio astronomical methods were reported by M.I.Ryabov (URAN-4, Odessa.) The basic characteristics of inner gravity waves in the atmosphere at 80-100 km were isolated by long-term observations with an automatic angle meter of the meteor radar of MARS (B.P.Kashcheev, A.N.Oleinikov - Institute of Radio Electronics, Kharkov.) Differential measurements of delayed signals from the navigation satellites of the GSP system provide data on the space-time variations of total electron content in the ionosphere without temporal and spatial limitations. As shown by I.I.Shagimuratov, L.V.Baran, I.I.Efishov, and Yu.N.Tepenitsym (ZO IZMIRAN), this method can be efficiently used to study the dynamics of the ionosphere.

The scientific program of the Section comprised 13 oral communications. An invited review lecture by B.M.Vladimirsky and A.V.Bruns on the Impact of solar activity on the technosphere - problems and results was delivered at a plenary session. The submitted papers dealt with a broad spectrum of solar and cosmophysical effects on various global events on the Earth, such as climate variations, biological effects of magnetic storms, earthquakes, geographic distribution of air accidents, parameters of long midlatitude radio lines, cosmophysical variations in the elements of measuring facilities, etc. Though the reliability of these relationships is still not too high, their consideration is important because the development of high technologies makes our civilization more and more sensitive to various regular and random influences.

The progress and the main results of some INTAS projects (including RFBR-INTAS and Georgia-INTAS) were discussed at a special INTAS Session.

Vladimir M. Bogod and Alexander S. Grebinskij (Special Astrophysical Observatory, RAS, 357147, Nizhnij Arkhyz, Karachaevo,-Cherkessia, Russia.) Large scale structure of the quiet Sun, coronal holes and plages as deduced by tomography study of RATAN 600 Observations.

In the paper the emission tomography methods was described. These methods are used in radio astronomy to investigate the solar atmosphere parameters of the quiet Sun, coronal hole and plages. The first method is based on the classical deconvolution in the wide range (1 mm - 300 cm) of wavelengths for reconstruction of atmospheric temperature profiles from the corona to deep chromosphere. Another one is the spectral index method which give us an additional possibility to extract information about parameters of solar corona using spectral data at decimetric wavelengths (such as the temperatures Tc, opacity (tau) and column emission measure EM.) The results achieved are based on the RATAN-600 observations in the (2.0-32 cm) range and supplemented by data of other observatories. The EUV measurements of differential emission made with high spatial resolution are used for the evaluation of the filling factor in the chromosphere, corona and CCTR ranges. It was shown that the bulk of the matter in the transition temperatures range gives only a negligible part of the solar atmosphere observed radio emission. Clear refraction effects detected in decimetric band radio emission also point to the presence of dense and compact structures in the coronal temperature region.

Alissandrakiss, C. (University of Ioannina, Section of Astrogeophysics, GR-45110 Ioannina, Greece), Bogod, V., Garaimov, V. (Special Astrophysical Observatory, 357147, Karachaevo-Cherkessia, Russia), Gelfreikh, G. (Pulkovo Astronomical Observatory, 196140, Pulkovo, Russia), Zheleznyakov, V., Zlotnik, E. (Institute of Applied Physics, 603600 Nizhny Novgorod, Russia.) Unusual inversion of polarization in microwave sources associated with sunspot group: RATAN-600 Observations and their interpretation. The data of multi-wavelength observations in the range from 1.7 cm to 32 cm on the reflector type radio telescope RATAN-600 were obtained with high polarization accuracy up to 0.5 %. They detected a new polarization phenomenon in radio emission of active region AR 7962 during May 13-16, 1996, on the Sun. The interesting phenomenon is connected with the change of polarization sign for both polarized components of the active region at wavelength 15 cm simultaneously, which is conserved during all days of observations. As the interpretation versions of the phenomenon was proposed to account for the linear coupling for consideration of magnetic field perpendicular to the plane connecting the spots of the group of the opposite magnetic polarity. That implies the effect of the field, parallel to a solar meridian. Such a field can provide independence of polarization patterns on solar rotation and reversal at the same frequency for both parts of the group. This field may be a manifestation of the large scale (say, "general = global") magnetic field of the Sun.

2. INTAS - RFBR grant 95-316, Physics of the solar corona as given by CM- and MM-observations. Urpo, S. (Coordinator, Metsahovi Radio Observatory, Kylmaa, Finland), Stepanov, A.V. (PI, Pulkovo Astronomical Observatory, S.Petersburg, Russia), Grebinskij, A., Bogod, V. (Special Astrophysical Observatory, S. Petersburg Branch, Russia), Gelfreikh, G., (Pulkovo Astronomical Observatory, S. Petersburg, Russia), Pohjolainen, S. (Metsahovi Radio Observatory, Kylmaa, Finland), Shibasaki K., (Nobeyama radio observatory, Japan.) Microwave tomography of the solar magnetic fields.

Analysis of polarization and spectra of the thermal bremsstrahlung emission of plasma structures of the solar atmosphere has opened an important tool to magnetic field measurements both in the chromosphere and corona. At the moment these structures include: faculae, prominences and even coronal holes. However, the method based on the solution of the equation of emission transfer meets serious problems which were under discussion in the paper. First, to analyze rather weak magnetic fields under investigation on the Sun, it is needed to measure the very low degree of polarization (of the order of 1% or less.) That implies usage of the largest radio telescopes accessible for solar observations, the absence of the proper spectral analysis and limited sensitivity to low polarization signals often are an essential obstacle to use of the method. Secondly, the usage of traditional approximation with the assumption of the homogeneous magnetic field is not a satisfactory solution for some wavelengths used. To overcome this problem the authors found a new form of the solution of equations of radiation transfer for thermal bremsstrahlung in anisotropic plasma with magnetic field. In the approximation of two values of magnetic field (coronal and chromospheric) it is possible to use the spectral data available. A simplified model of the chromosphere was also used in analyzing the problem. The result shows that there are three spectral regions of microwave radio emission with different interpretation of the results of the magnetic field measurements: (i) at shortest wavelengths the found magnetic field strength refers to the chromospheric level, (ii) in the middle wavelength range there are comparable inputs in polarized flux both from chromospheric and coronal layers while intensity dominates the chromosphere, (iii) at longer wavelengths polarized signals are mostly due to the corona, so some mean value of the coronal field is found from observations. For active regions the problems of input from different mechanisms of the generation of the radio emission are essential.

The development of the method was shown on examples of observations made with the radio telescopes RATAN-600, WSRT, Nobeyama radio heliograph.

It found the unexpectedly large values of the magnetic fields in the corona (0.6-0.7 of the photospheric strength.) This result can be interpreted as a consequence of the very inhomogeneous structure of the solar corona, correlated both in density and the magnetic field.

3. INTAS-RFBR grant 96-0659, Neutrino processes in strong magnetic fields and hot dense matter, Coordinator V.B. Semikoz

1. Significant progress was made in approaching the problem of solar neutrino. According to a new scenario, developed by the research groups at the Moscow State University and IZMIRAN, the spin-flavor conversion of neutrino occurs in random magnetic fields in the solar convection zone. Unlike the resonance spin-flavor oscillations in the regular magnetic field (the mechanism by Akhmedov-Lima-Marciano with the same transition magnetic moment of the Mayoran neutrino), the effective conversion of neutrino in the new model occurs aperiodically due to the influence of the random field, with the right-handed active anti-neutrino being generated more effectively. The latter contributes significantly to the deficit of neutrino fluxes measured in the neutrino experiments.

2. The analysis of scattering of the solar neutrino for future experiments (BOREXINO, HELLAZ) was continued. A new method was proposed to measure the transition magnetic moment of the Mayoran neutrino from the asymmetry of neutrino scattering on electrons when measuring the energy and direction of the recoil electron pulse (HELLAZ experiment.)

3. A search for restrictions on the expanded calibration models was carried out in collaboration with the experimental groups of the Gran-Sasso Laboratory (R.Bernabei) and the Institute for Nuclear Research (I.R.Barabanov.)

4. Electromagnetic interaction between electrons was shown to result in collective effects that significantly (about 3 times) enhanced the contribution of the weak vector current of electrons to the synchrotron emission of neutrino pairs.

5. The specific luminosity of the direct URCA process was calculated for strongly magnetized degenerated matter of neutrino stars under beta-equilibrium conditions. It was shown that a sufficiently strong magnetic field trapping all electrons and protons to the basic Landau level violated the threshold condition on proton density, necessary for the URCA reactions in isotropic medium. In a strong magnetic field, a direct URCA process is allowed at an arbitrary low proton density, which must lead to an abnormally fast cooling of neutron stars. This allows us to impose an upper limit on the value of magnetic fields inside the observed neutron stars.

4. INTAS grant 96-183, Low frequency VLBI research for solar studies and as a precursor to space VLBI with radio astron: Benz, A. (Zurich), Martivani, F. (Bolongna), Lichachev, S.F. (Lebedev Institute of Physics, Moscow), Bazelyan, L.L. (Kharkov), Poperechenko, B.A. (Moscow), Snegirev, S.D. (Nizhny Novgorod.)

1. A radio interferometer for the wavelength of 91 cm with a base of 70 km was put into operation at Staraya Pustyn-Zimenki (NIRFI), and the device for 52 cm was designed.

3. Three observation campaigns were conducted within the international VLBI network: Green Bank, Arecibo (USA), Hart RAO (South Africa), Hobart (Australia), Torun (Poland), Shanghai (China), and Russian telescopes.

4. Four observation campaigns were carried out at the network, comprising telescopes at Pushchino, Medvezhyi Ozera, Evpatoria, Staraya Pustyn, and Zimenki.

5. INTAS grant 95-932, Modeling of the electromagnetic weather and of the energy balance in the near-earth space environment by ground-based and satellite observations. Coordinator Feldshtein Ya. I.

The studies in 1998 focused mainly on developing a dynamic paraboloid model magnetic field in the magnetosphere and its application for calculating the magnetic field of large-scale three-dimensional magnetospheric current sheets, for determining the relationship between the low-altitude geophysical events and the magnetospheric plasma structure, and for updating the quantitative model of electromagnetic space weather.

6. INTAS grant 96-2346, Multi-satellite study of the magnetospheric dynamics driven by solar wind plasma flow: electromagnetic energy dissipation processes (substorms and particle acceleration.) Coordinators Sauvaud, J.-A. (France) and Zeleny, L (Russia.)

During 1998, regular measurements from the INTERBALL-2 satellites were performed, and since May 1998 also from its MAGION-5 subsatellite. Also scientific analysis of the received data was performed together with numerical modeling and theoretical analysis. Publication of new results took place, in particular, in special issues of European journal Annales Geophysicae, v.16, N9, 1998 and in the Russian journal Cosmic Research (Kosmicheskie Issledovania, English version), v.36, N1, N3 and N6, 1998, as well as in other scientific journals. The main scientific results obtained in 1998, are:

Some anomalous cases of solar-diurnal anisotropy in the intensity of neutron and hard components of cosmic rays were analyzed to isolate those associated with the meteorological effect of the meson component, as well as with geomagnetic field variations.

A number of abnormal increases of the mu-meson cosmic ray component, the new and full moon epochs, the perigee and apogee of the Moon, and singular proton solar flares were compared with major earthquakes. The obtained complex diagrams lead us to the conclusion that major disastrous earthquakes are more frequent when several factors listed above coincide.

8. INTAS-RFBR grant 97-1088, Support for the SOHO solar maximum science mission. Makarov (GAO RAN, Kislovodsk Station) team-leader, Grigoriev (Sibizmir, Irkutsk) and several members of his team, Obridko (IZMIRAN, Moscow Region) and several members of his team, Kim (Moscow, SAI) and several members of her team, Stepanyan (CrAO, Ukraine) and several members of his team, Kulidjanishvili (Abastumani Obs, Georgia) team leader.

The project is a follow-up project of INTAS 94-2521 (Ground-based Support for SOHO: The Solar and Heliospheric Observatory) which was successfully completed on 30 November 1997. Both the INTAS and NIS teams are the same, with one exception: CR 9 of INTAS 94-2521 (Fesenkov Astrophysical Institute, Kazhakstan) will not participate anymore in this project because the communications with them were very difficult, mainly for technical reasons.

INTAS 94-2521 can be considered a full success. The FSU participants not only acquired synoptic data which are now being used during the scientific exploration of the SOHO data, but also participated in numerous SOHO campaigns, several of which were organized by the INTAS member state participants. Among the campaigns in which FSU contractors participated were the large international efforts to study the onset of coronal mass ejections, several X-ray bright point campaigns, filament and prominence campaigns, and the "Whole Sun Month" campaign. Some of the FSU participants also became active in analyzing SOHO data (mainly from EIT and LASCO), and we hope that, now that the first steps have been made, this level of involvement will continuously increase.

Considerable progress has been achieved in spite of the fact that the funding of the project has not yet begun because of the bank crisis in Russia.

9. INTAS grant 96-367, Characteristics of Maidanak Observatory among the major international ground-based astronomical facilities of the future. Eghamberdiev, S. (Institute for Astronomy, Uzbekistan) team leader Ilyasov, S. (Institute for Astronomy, Uzbekistan) team member.

The project was discussed at a special meeting of the Board of Officers of Euro-Asian Astronomic Society (EAAS.) Because of disintegration of the USSR, many links between the former republics were broken. At present, certain measures have been taken to create a joint international observatory with EAAS as one of the constituting bodies.

10. INTAS grant 97-1162, Baltic electromagnetic array research-processing, modeling and interpretation. Coordinators: Kopytenko, Yu.A. (St.-Petersburg Branch of IZMIRAN), Toivo Korja (Geological Service, Finland.) In 1998 magnetotelluric sounding was carried out in Russia at 3 stations within the BEAR network. The data in a single format were forwarded to the Coordinator.

On behalf of Jeff Thayer, Rod Heelis, and myself, who are your representatives on the NASA SEC Roadmap Committee, we would like to bring you up to date on ITM future planning opportunities.

The first meeting of the present day SEC Roadmap Committee occurred January 25-26, 1999. SEC is one of four themes of the Office of Space Sciences, see http://umbra.nascom.nasa.gov/spd/. It stands for Sun Earth Connections and encompasses Solar, Heliospheric, Magnetospheric, and us (ITM.) It is responsible for satellite programs, explorers SMEX, MIDEX, suborbital, SRT and in particular has a line of missions called Solar-Terrestrial Probes (which are basically at a funding level of twice a MIDEX.)

The S-T probes are the major missions for the future, see http://stprobes.gsfc.nasa.gov. At the present time, we have TIMED, Solar-B, STEREO, Magnetospheric Multi-Scales (MMS), Global Electrodynamics (GED), and Magnetospheric Constellation. However, this only goes until 2007!!! One of the major objectives of this Roadmap Committee is to extend this queue beyond 2007.

An open-to-all workshop is being held on March 2 and 3, 1999, in Greenbelt, Maryland (Editor's Note: see first item under Forthcoming Meetings.) This is where the ITM, as well as the other disciplines, can present suggested missions for the Future of SEC physics. In fact, these missions do not need to be entirely technically feasible today. If you have a great science concept, but the mission needs technology effort, it is still quite acceptable. The Solar-Terrestrial Probes line has technology funds as well.

This is a very unique position within NASA in that the S-T probe line out to 2007 is preapproved and on track to carry out the 6 missions proposed. It is a great opportunity for ITM to ensure continuous satellite missions for ITM science beyond 2010.

What is the meeting format? The Roadmap consists of solar, heliospheric, magnetospheric, and us (ITM). However, to prevent discipline splinter groups debating their own mission sciences, the Workshop will use a different format that follows the SEC Quests. Hence, splinter groups will form based on the following three Quests:

In addition to providing equal opportunities for all participants to present their science and mission, each participant is invited to prepare a Poster describing (selling) their concept. These posters will be displayed for the entire Workshop time and the Workshop participants will be given ample time to interact with the poster presenters as well as through the interaction in splinter groups.

The three of us (Heelis, Thayer, Sojka) will work in any way possible with ITM scientists who are unable to attend the meeting to have their ideas, concepts, and missions represented at the Roadmap Workshop.

At the first Roadmap meeting (January 25-26), both Dr. George Withbroe, our SEC Theme Director, and Dr. Ed Weiler, the Associate Administrator, provided the following encouragement:

As an aside, the technology associated with tethers was discussed, however, compelling science was not identified. Similarly, a space station is to exist, as are commercial satellite constellations. Basically, NASA into the new millennium is extremely open to compelling science being done with conventional (NASA satellites) and unconventional methods as listed. Planetary ITM was also discussed and indeed could become a major thrust in the revised Roadmap.

Please read and think about it, and pass it on to our ITM colleagues that we have not been able to reach. Please consider the three of us as your mouthpieces if you are unable to attend the Roadmap meeting. However, your presence would be preferred in order to show other disciplines that ITM is alive and wants to do NASA science.

A two day Sun-Earth Connection (SEC) Workshop will be hosted by the NASA Office of Space Science (OSS) and Goddard Space Flight Center Solar Terrestrial Probes (STP) Program Office. The primary purpose of the Workshop is to elicit from the SEC community new, exciting and innovative science mission and technology concepts which will become input for the 2000 - 2025 SEC strategic plan. Tri-annual strategic plans are now required of most federal agencies and their enterprises and provide much of the basis for the development of policy and decision making. All of the OSS themes have appointed "Roadmap Teams" which are charged with creating a "vision" for the future of their science for the next 25 years and charting the scientific, technologic and programmatic goals which must be achieved to bring the vision to fruition.

At the SEC Strategic Planning Workshop reports on the state of the SEC theme, near-term mission development activities, and the on-going technology development programs will be given. However, most of the time will be given over to contributed poster sessions and to splinter group meetings framed around the 3 "science quests" identified in the 1997 SEC Strategic Plan (see http://stprobes.gsfc.nasa.gov) and their enabling technologies.

These quests serve to communicate simply and directly to the public, industry and government the nature of the scientific and technologic vision we are pursuing and the compelling reasons why we must be provided the support necessary to succeed. The SEC quests are:

Splinter groups will review these quests, the visions of the future they convey, and their scientific and technological foundations. The splinter groups will then develop recommendations for the present SEC Roadmap Team (Chair: K. Strong/Lockheed-Martin) regarding how they should best be implemented through individual Solar Terrestrial Probe and Frontier Probe missions or "campaigns" involving a series of linked missions. The instrument and spacecraft technology developments which are necessary for the successful implementation of these missions will be addressed both within the individual quest splinters groups and in a dedicated technology splinter group. These splinter sessions will be chaired by members of the SEC Roadmap Team. The final Workshop agenda is now available on the Solar Terrestrial Probes website listed above. The Workshop will end late on March 3rd and be followed by a meeting of the full SEC Roadmap Team the next day.

Scientists and technologists are encouraged to participate in the Workshop. It will be held at the Marriott Hotel (6400 Ivy Lane, Greenbelt, MD 20770; 301-441-3700.) There is no registration fee, but all participants are requested to register at their earliest convenience. If you wish to contribute a poster presentation, then a title and a 1 - 2 sentence description should be included in the space provided on the registration form. (Note: Poster board areas will be ~ 4 ft x 8 ft and straight pins will be provided.) The registration form is available at the STP website.

The local workshop organizer is Dr. James A. Slavin. He can be reached at 301-286-5839 or jim.slavin@gsfc.nasa.gov. The conference coordinator is Ms. Kelly Whetzel. She can be reached at 301-345-3211 or kelly.whetzel@gsfc.nasa.gov.

Spend four days in beautiful Boulder, Colorado learning about science education!

The Workshop will be held at the Space Science Institute which is a national leader in providing science education training for scientists, engineers, and science outreach professionals affiliated with:

Paul B. Dusenbery, Space Science Institute; Ramon E. Lopez, University of Maryland; Cherilynn Morrow, Space Science Institute

"The SSI Workshop was a turning point for me as a science educator. I'd given many presentations in classrooms and teachers' workshops, but knew very little about cognitive science and its implications for education, or about the way school systems really work. The Workshop gave me a foundation for the next stage of Outreach work - Outreach as a form of scholarship. The professional contacts that I made were invaluable, and I received useful tools that I have used many times (e.g., ways to evaluate curricula.) I'd recommend this Workshop for scientists at all stages of Outreach work, from novice to expert." Dr. Alex Weaver, Director of Education and Outreach, CIRES, University of Colorado at Boulder.

The registration fee is $250. Included in the registration fee are the reception during the poster session on the first evening of the Workshop (Sunday, April 11), and the evening banquet (Tuesday, April 13), conference materials (including a source book), continental breakfasts, coffee or tea and snacks and luncheons. Register on-line at:
http://www/ssi/colorado.edu/Education/ResourcesForScientists/Workshops/General Web Site: http://www. spacescience.org (Hot Stuff) For more information, contact: Susan Solari, Space Science Institute, 1540 30th St., Suite 23, Boulder, CO 80303-1012 Phone: (303)492-5184, Fax: (303)492-3789.

After the success of the first meeting of this kind in Nice, we will have the next special session (ST11) on "Theory and Simulation of Solar System Plasmas" during the forthcoming General Assembly of EGS. The scope of the next year meeting can be found below.

Theoretical investigations are necessary to understand the plasma dynamics in the solar system and numerical simulations provide additional tools when analytical treatments fail. On the other hand, many space plasma phenomena appear to be common to different regions of space like magnetospheric tails, solar corona, or planetary and cometary boundaries. After the success of the first meeting of this kind during the 1998 EGS meeting in Nice the goal of this symposium is, again, to bring together all the scientists interested in the understanding of similar physical processes taking place in different parts of the solar system and to continue the exchange and discussions, started in Nice. During the 1999 EGS General Assembly, a particular emphasis will be put on the macroscopic consequences of the kinetic phenomena and on the limits of the MHD description for phenomena such as reconnection or parallel electric fields in collisionless plasmas. Contributions concerning particle heating and acceleration involved in these phenomena are especially encouraged. Analytical theoretical treatments are welcomed as well as numerical simulations, since many of the problems mentioned above are unreachable to analytical solutions.

All information and forms concerning Registration and Hotel Reservation can be found on the Web at: http://www/copernicus.org/EGS/EGS.html or the EGS office: Max-Planck-Str. 13, 37191 Katlenburg-Lindau, Germany, Tel: +49-5556-1440 Fax: +49-5556-4709 e-mail: EGS@COPERNICUS.ORG.

Note: Registration will be limited to approximately 200 participants, and facilities are available for approximately 50 poster presentations. Meeting information, including registration and abstract submission forms, is available at the following Web location http://sec.noaa.gov/~ swc/sww99/index.html

The third annual Research-to-Operations meeting will be held in Boulder, CO on April 21-23, 1999, in conjunction with the NOAA Space Environment Center Users Conference on April 19-21. Research and operations topics will be addressed that span the full solar-terrestrial environment, from the sun to the upper atmosphere. Among the topics that will be addressed are: recent research advances, data assimilation, community modeling activities, future data sources, rapid prototyping centers, and the status of space weather operations centers. For the first time, the Research to Operations meeting will be combined with the SEC Space Weather Users Conference, allowing space environment researchers to interact with users of space weather services.

As solar maximum approaches we are faced with increasingly frequent solar events such as Coronal Mass Ejections (CMEs) and the geomagnetic storms they cause. A substantial fraction of the energy incident from the solar wind during storms is converted to the high-energy portion of the particle distribution and manifested in the inner magnetosphere as enhanced ring current injections and relativistic electrons. Energetic particle acceleration and transport thus represent a key component of understanding magnetospheric dynamics. Recent modeling, theory and observations all indicate that the ring current and radiation belts are highly dynamic and are coupled in ways that are not easily predicted from standard diffusion. Relativistic electrons appear to require some preconditioning before their final energization to populate the radiation belts. In at least some circumstances, strong interplanetary shocks can stimulate prompt generation of new radiation belts. Ultimately, the temporal and spatial configuration of the electric and magnetic fields govern the motion of charged particles so a complete understanding of high energy particle source mechanisms necessarily requires a global view of the inner magnetospheric electrodynamics. With the availability of multiple satellites and new, more advanced detectors and advances in modeling and simulation capabilities we are in the best position ever to tackle outstanding issues in the inner magnetosphere including: global electric and magnetic field changes, enhanced wave activity during storm times, and energization and transport of charged particles. This session invites papers on dynamic modeling, multi-point observations, solar wind correlations particularly on the differences and commonalities among storms that are driven by different solar wind conditions, and new theoretical developments on the dynamics of the inner magnetosphere, ring current and radiation belts.

Brian J. Anderson, The Johns Hopkins Applied Physics Laboratory, 11100 Johns Hopkins Road, Laurel, MD, 20723-6099, USA, Phone: 240-228-6347, E-mail: brian.anderson@jhuapl.edu

Anthony A. Chan, Department of Space Physics and Astronomy, Rice University, 6100 Main Street, Houston, TX 77005, USA, Phone: 713-527-8101, E-mail: