International SCOSTEP Newsletter

TARGET OF OPPORTUNITY CAMPAIGN TO OBSERVE ACTIVE REGION 8307

SOLAR ALERT/STATUS REPORTS
Status Change of Solar/Alert Status Reports
July 31, 1998, Solar Status Report
August 18, 1998, Extra Solar Status Report and Alert
August 21, 1998, Solar Alert
August 22, 1998, Solar Alert

OTHER NEWS ITEMS
Space Weather Activities in SCOSTEP
Updating National Space Weather Program Implementation Plan
Prediction of the Location of Earth's Magnetopause: A Taiwan Space Weather Effort
Connect with the Space Science Institute for Education and Public Outreach
The Japanese Mars Orbiter, Planet-B, Launched Successfully
Information on the Interball Subsatellite Magion-5
Academician Geliy Zherebtsov's 60th Birthday
Final STEP Handbook Published
Job Announcement - NRL Postdoctoral Position in Solar and Terrestrial Variability
Job Announcement - Research Associate in Virtual Reality/Scientific Visualization at the University of Warwick

MEETING REPORTS
International Symposium on Dynamics and Structure of the Mesopause Region (DYSMER)
IACG Campaign #2 during the COSPAR Assembly

FORTHCOMING MEETINGS
Fifth Latin-American Conference on Space Geophysics (V-COLAGE)
Fall AGU Special Session SM-08: Magnetic Reconnection in the Sun-Earth Connected System: Recent Progress
Fall AGU Special Session SM-09: Substorm Onset Timing
Fall AGU Special Session SH-05: Origin, Initiation and Three-Dimensional Structure of CMEs
Fall AGU Special Session U-11: Climatic Effects of a Changing Sun
Radar Observations of Meteors: Issues and Results
Special Session on Ionospheric Heating
Second Announcement for the Chapman Conference on Magnetospheric Current Systems
Dynamics of the Magnetosphere and its Coupling to the Ionosphere on Multiple Scales using Interball, ISTP, and Ground-Based Observations
Long-Term Changes and Trends in the Atmosphere (LT-ACT'99)
PIERS 1999: Progress in Electromagnetic Research Symposium
4th SEC User Conference and 5th Research-to-Operations Workshop
Science for the 21st Century
Solar Variability and Climate
Solar Magnetic Field: Reversals, Polar Field, Dynamo
IAGA Symposium on Magnetic Storms
IAGA Symposium GA 4.02: CMEs, Prominence Eruptions and Flares: Onsets and Relationships
International Workshop on Radio Methods for Studying Turbulence
Magnetospheres of the Outer Planets Conference (MOP 99)

CALENDAR OF EVENTS

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.

TARGET OF OPPORTUNITY CAMPAIGN TO OBSERVE ACTIVE REGION 8307

RECENT ACTIVITY AND OBSERVATIONS (for 19 Aug. 1998):
Active region 8307 (N32E72 at 00:00 UT on 20 Aug.) produced an M3 X-ray class flare at 19/14:26 UT. There were associated type II and IV radio bursts. More significantly, the region exhibited an impulsive X3.9 X-ray burst with a flux peak at 19/21:45 UT. In radio, the flare peaked at 18,000 SFU at 245 MHz and 5,800 SFU at 15.4 Ghz. Mauna Loa (Darral Koon) reports an associated fast CME that was simultaneous with the flare. W. Marquette at Big Bear relates that the region is still in the growth phase, spot count and area have increased -- especially SW of the biggest spot. Also the spot group is predominantly negative or trailer in polarity. He states: "We expect the high level of activity to continue" (and many others agree.)

The X3.9 flare was well observed at Big Bear but only decay phases were observed by Yohkoh. Note, Yohkoh did obtain excellent observations of the X-class flare on the 18th and images are reportedly available on their web pages. Today's X3.9 flare was the first significant event observed by the High Speed H-alpha Camera/Polarimeter in Boulder (A. Kiplinger, P.I. at Sommers Bausch Obs.) The camera obtains polarization maps of active regions with a cadence of 0.5 s in H-alpha center line and at -1.3 A in the blue wing. It is looking for signatures of accelerated particle beam polarization in H-alpha in conjunction with hard X-ray and other high energy signatures. (Limb observations are predicted to optimize polarization effects.) After stop and go attempts to observe through monsoon-like clouds over Boulder, a hole in the clouds miraculously cleared about 3 m before the flare and stayed open until early decay. More than 2000 polarization maps of the flare were obtained in the brief hole.

SCIENTIFIC OBJECTIVES: This region is a prime target for numerous objectives -- many are geoeffective. It has displayed fast CMEs, long duration and impulsive soft X-ray flares. Obviously, while it is so close to a limb, studies involving vertical geometries both off limb and on disk should be considered and conducted.

FUTURE OBSERVATIONS: Magnetic coverage is extremely important (long. and vector.) Radio flux and imaging is needed. Yohkoh's modes of performing whole sun observations as well as flare mode observations appear to be performing admirably.

Reports of successful and interesting reports of observations are welcomed by sending (brief) email to: akipling@proton.sec.noaa.gov.
Alan L. Kiplinger

STATUS CHANGE OF SOLAR ALERT/STATUS REPORTS

Pat McIntosh, retired solar forecaster from NOAA's Space Environment Services group, has been operating a personal forecast service from his home observatory for several months. With encouragement from several persons, he distributed his alerts to a lengthy list of contacts. We have published a number of his interesting forecasts in issues of these Newsletters, especially one or two sets that were followed by significant activity.

As indicated below, Pat is suspending his no-charge forecasting until he can review his circumstances and determine whether there may be a way of charging for the service and gaining some income to supplement his retirement annuity.

As he notes, this 23rd solar cycle has begun as one that is difficult to forecast. Past characteristics of sunspot groups that were indicative of particular performance and that were used during prior cycles as the basis for forecasts have not led to the same results in the early part of this cycle. For a while, it seemed as if this cycle was likely to rise to a high maximum sunspot number. Now activity has decreased and the cycle no longer offers indications of future high activity. This may yet change. We can only wait and see and try to read any precursor signs offered by the active Sun.

This note is not a solicitation for business for Pat, but is an opportunity to thank him for the months of interesting and informative forecasts. I think the SCOSTEP community interested in solar activity (especially the Space Weather component) has greatly appreciated Pat's volunteer work.
Joe H. Allen

July 31, 1998 1600 UT

HELIOSYNOPTICS, Boulder, Colorado

SLOW EVOLUTION EQUALS LOW ACTIVITY REGION 8282 PROTON FLARE PREDICTION FAILED LARGE NORTH POLAR CORONAL HOLE

END OF GRATIS ALERT SERVICE

The past two months have been much less active than expected for the rising portion of a solar cycle. This epoch of solar life has included numerous but very small active regions, with remarkable longevity for their small size. Of particular difficulty to solar predictions is the appearance of several regions with preflare attributes but which failed to flare. It appears the reason is related to the stability of those regions. Rapid evolution is the hallmark of flaring regions. The trends that were successfully extrapolated in earlier portions of this solar cycle are unsuccessful predictions in this present epoch.

The monthly solar indices for July will be higher than the previous months, but barely so. The rate of rise of this solar cycle is now defined as too slow to predict a large sunspot cycle. There continue to be anomalous aspects to the cycle that warn against any long-term predictions.

NORTH POLAR CORONAL HOLE

The north polar coronal hole has enlarged significantly in the past two months, resembling coronal holes for the post-maximum phase of a solar cycle. There is a high-speed solar wind stream associated with the low-latitude extension of this coronal hole. Significant geomagnetic disturbances are correlating with this solar wind stream, including the one in progress at this hour.

END OF GRATIS ALERT SERVICE

HelioSynoptics has finished a full year of gratis, experimental solar alert and prediction service. There will be no further alerts until new funding is obtained. The alerts may resume as a subscription service.
Patrick S. McIntosh

August 18, 1998, 2000 UT

EXTRA SOLAR STATUS REPORT AND ALERT

HELIOSYNOPTICS, Boulder, Colorado

POSSIBLE SUPER-REGION AT N31 E90 - SOURCE OF TWO X-FLARES CAUTION FOR REGION 8299 (N16 W66) REDEVELOPING REGION 8307 N31 E90

Observations at 1800 UT show a chain of strong, small spots, possibly embedded in penumbra, in an arc near, and south of, the large spot in Region 8307 near N30 E90. A large-scale white-light image taken by Big Bear Solar Observatory at this time confirm this visual observation.

The BBSO magnetogram for this region strongly suggests a major delta configuration in this region, not surprising for a region that produced a pair of Class-X flares. This region may qualify as a super-region, which raises the forecast for significant proton emission. Particles might not reach Earth in a large fluence until the region nears solar central meridian. Propagation of particles will be assisted by the nearby open magnetic fields in the large coronal hole adjacent to this region, to the north and west of its location. Coronal mass ejections are common along the polarity boundary adjacent to major polar coronal hole lobes; therefore, expect all the Big Flare Syndrome properties with events from Region 8307.

Region 8307 is the return of Region 8282 which drew much attention last month for its unusual morphology and unrealized flare potential.

INCREASED FLARE POTENTIAL IN REGION 8299

Region 8299 has increased its flare potential with growth of new spots on the south side of the eastern large penumbral mass, creating a new delta configuration that is more potent than the continuing delta on the NE corner of that same penumbral mass. A dark filament embedded in the plage north of the spots adds further flare potential. If proper motions and/or additional growth occur in this new delta area there could be a strong Class-M with protons and a west-limb CME. The importance of Region 8299 is enhanced by its near-180 degree longitude separation from the strong Region 8307 coming over the east limb. Caution for activity in Region 8299 is necessary as it becomes more difficult to detect changes because of proximity to the solar limb.

Some speculation from an old observer: In periods of flaring regions, located 180 degrees apart, the other active regions tend to be small and inactive, as if the sun redistributes flux and flaring-dynamics to concentrate those features in the favored, active longitudes.

MOST-RAPID RISE OF SOLAR CYCLE IN PROGRESS

With the present east limb activity, the solar indices for August are assured to rise sharply from the July values, affirming the expectation of the most-rapid rise portion of the solar cycle. Indices will attain solar maximum levels by November, with peak indices expected in the last quarter of 1999.
Patrick S. McIntosh

August 21, 1998, 1600 UT

SOLAR ALERT

HELIOSYNOPTICS, Boulder, Colorado

SUNSPOT GROWTH REGION 8307 (N32 E47) brings size and geometry closer to classic proton-flare sunspot groups. Growth consists of strong umbrae along NW edge of large penumbral area. Polarity of these spots inferred to be same as larger umbrae near center of the penumbra, but the gradient is increased between these new spots and the strong opposite polarity spot at the north end of the penumbra.

The region is now more similar to the proton-flare sunspots of August 4, 1972. That region went through a few days of quiet before its worst series of flares. Counter-clockwise rotation is evident in the spot motions and curvature of H-alpha fibrils surrounding the region. Magnetic fields are possibly twisting, storing energy and become less stable.

A lack of important flares in the past 36 hours is not evidence of decay. Additional Class X flares, with protons and strong radio emission, are expected.

Analysis is seriously affected by a lack of observations world-wide, due to well-placed storms. SOHO is sorely missed. An update will follow when Big Bear and Mt. Wilson data are available.

This alert was delayed by an interruption in internet service, possibly due to U.S. West strike in Colorado.
Patrick S. McIntosh

August 22, 1998, 2000 UT

SOLAR ALERT

HELIOSYNOPTICS, Boulder, Colorado

ANOTHER CLASS-X EVENT IMMINENT FROM REGION 8307

Despite some evidence of sunspot decay, do not be deceived by this region. The rotation and proper motions of the spots continue to show a counterclockwise vorticity, and this is now apparent in a spectacular extension of the principal polarity boundary around to the east side of the spot group. Plage development at this new location indicates early stages of flux eruption. No spots on the east side of the main spot, yet; but, new spots have emerged north of the main spot, where the M9 X-ray flare occurred (as expected) at 0h UT today. The negative-polarity spot in the small delta to the west of the main spot continues to move northward relative to its opposite-polarity companion, proving that magnetic-field shear is continuing. The large spots within the main penumbra rotated more rapidly CCL since yesterday and the brilliant facular patch embedded among them continues. A large and active filament is developing from the region to the south. The expected flare will surely erupt this filament, giving an important CME (coronal mass ejection.) The length of polarity boundary that could be involved with the next flare suggests the optical class could reach the maximum category of 4B. Xray intensity is expected to be Class-X.

The post-flare xray loops visible at 1614 UT include an area of dark loops backlit by bright loops to the NE. The dark material appears to be directly above the area of highest magnetic-field gradient in the main delta on the north edge of the large penumbral mass. Magnetograms show a large departure from the H-alpha-inferred polarity boundary at this location, suggesting this is a localized extreme in non-potential magnetic fields. This suggests a high amount of stored energy available for the expected flare. The core of this flare is expected on the NE corner of the main spot. White-light emission may occur at this location.

If particles are accelerated with the expected flare, propagation Earthward is likely because of the large coronal hole NW of the flare site. Open field lines extend from this active region to well past central meridian, allowing particle transport at least 60 degrees to the west of the active region.
Patrick S. McIntosh

OTHER NEWS ITEMS

SPACE WEATHER ACTIVITIES IN SCOSTEP

The Space Weather (SWx) Working Group (WG) of SCOSTEP's SRAMP (STEP Results, Applications & Modeling Phase) decided to promote a month for cooperative global space weather observations and exchanges of timely information to test the technical infrastructure and determine what can be done effectively in this area. If we are fortunate and some interesting SWx phenomena happen during the selected interval this will provide material for a special analysis and modeling effort. Hannu Koskinen, Chairman of the Space Weather Working Group, announced October 1999 (repeat, 1999) is designated as 'SRAMP Space Weather Month: October 1999'. SWx WG members Phil Wilkinson (IPS, Australia) and David Boteler (Geolab, Canada) are coordinators for the special month. Phil will be the contact person for the Geophysical Calendar program of observations and David will concentrate on the interface role with the applications community. Sunanda Basu (NSF, USA) has reserved a slot on the Incoherent Scatter Radar Coordinated Observation Days list already on the WWW. There the October 1999 period is designated as the "First SRAMP Space Weather Campaign."

Further, as a result of the SWx WG meeting in Nagoya, Japan, and the SRAMP Steering Committee (SC) meeting in Taipei, Taiwan, it was decided to identify the 2-month period April-May 1998 as a "SRAMP Space Weather Analysis Interval: April-May 1998". A focus person to coordinate this effort has not been identified, but preliminary correspondence about the topic may be directed to Dan Baker (Chairman, SRAMP) and/or Joe Allen (Scientific Secretary, SCOSTEP.) Part of this active period was identified by SCOSTEP's ISCS (International Solar Cycle Study) program for special data collection and analysis efforts, during their workshop in Nagoya preceding the COSPAR Assembly. It was a period rich in solar activity, major flares, hard spectrum proton events with evidence of heavier ions, formation of a new intermediate trapping region between the inner and outer belts, and with numerous adverse operational events on satellites.

SCOSTEP encourages other groups that may be interested in either the special analysis interval of 1998 or the future observational effort in 1999 to provide information about your plans and to take account of our community of interest in these events and times.
Hannu Koskinen
Hannu.Koskinen@fmi.fi

UPDATING NATIONAL SPACE WEATHER PROGRAM IMPLEMENTATION PLAN

Kile Baker is updating the US National Space Weather Program implementation plan with regard to information about models that are now in use or under development. He has invited circulation of the following message among the Space Weather community.

I would very much appreciate your help in this task. If you are involved with the creation and/or development of a model which is either currently being used or is likely to be used in the future for studies involving space weather, please let me know the following information.

1. Name/acronym of the model.

2. Type of model (examples: Global MHD simulation, empirical model of ionospheric electron density, ionospheric convection model, etc.)

3. Status (e.g., mature, usable but still under development, not usable/under development.)

4. Funding sources (if still under development.) Also feel free to provide any additional information that you think should be included in a brief overview of space weather models.
Kile Baker, Prog. Dir. Mag. Physics
NSF, GEO/ATM, 4201 Wilson Blvd., Arlington, VA 22230
phone: 703-306-1519 FAX: 703-306-0849
email: kbaker@nsf.gov

PREDICTION OF THE LOCATION OF EARTH'S MAGNETOPAUSE:
A TAIWAN SPACE WEATHER EFFORT

The location of the magnetopause (MP) is one of the most important pieces of information in space weather. Over the past few decades, various attempts have been made to model the location of the MP under the influence of the solar wind. Chapman and Ferraro (1931) first introduced the concept of the MP assuming that a discontinuity surface separates the magnetosphere from interplanetary space. In early models the location of the MP depended on solar wind dynamic pressure, Dp. Many years later, Dungey (1961) suggested an open magnetosphere. In this model, the interplanetary magnetic field (IMF) orientation also affects the MP location.

Still later, more empirical models of the MP location were developed using large in situ data sets of MP crossings. In most of those models, the size and shape of the MP is assumed to depend mainly on IMF's north-south components, Bz and Dp. The other parameters such as the east-west components of IMF, the thermal and magnetic pressure of the solar wind, the geomagnetic activity indices, Dst and Kp and others are assumed not important in comparison with Dp and Bz for controlling the location of the MP.

In 1994, at the Institute of Space Science, National Central University, Chung-li, Taiwan, we initiated a project to compile a catalog of MP crossings. The MP crossings are obtained from ISEE 1 and 2, AMPTE/IRM, and IMP-8 data. The upstream solar wind data were obtained from ISEE-3 and IMP-8. The time delay for the solar wind flowing from ISEE-3 and/or IMP-8 to the MP have been considered for each individual MP crossing. Other parameters such as the time, location, normal directions of the boundary, magnetic fields on both sides of the boundary, upstream solar wind, and geomagnetic activity indices for each crossing are included. These crossings are documented in order to satisfy various needs in MP studies. This catalog is also useful for a variety of statistical studies.

The success of the MP prediction model depends strongly on the quality of the catalog. To ensure a good quality catalog, we have carefully identified the MP crossings using both the plasma and magnetic data, and searched for particular solar wind Dp and Bz causing the MP crossing by considering the time delay between the two satellites.

Neither the identification of the MP crossings nor the search for correct Dp and Bz is trivial. The differences in prediction models depend on how well the input data are selected. Perhaps it is due to the fact that we have paid more attention to the selection procedure than most of the other studies that our model now seems to give a better prediction for the location of the MP.

A functional form, r = r0 [2/(1+cos q)]a is assumed to fit the size and shape of the MP using those crossings selected in our catalog. This functional form has two parameters r0 and q representing the standoff distance and the level of tail flaring. We assume that r0 and q vary with Bz and Dp.

Using a multiple parameter fitting scheme with 552 crossings, we obtain a function form of r0 and q in terms of Dp and Bz as follows (Shue et al., 1997, 1998.) This explicit function is useful for operational space applications such as predicting when satellites at geosynchronous orbit will be found in the magnetosheath.

r0 = (11.4 + 0.013Bz)(Dp)-o(1,6.6), for Bz „ 0 r0 = (11.4 + 0.14Bz)(DP) -o(1,6.6), for Bz < 0 a = (0.58 - 0.010Bz)(1 + 0.010DP)

During the January 11, 1997 event, the MP was pushed inside the geosynchronous orbit as seen by several geosynchronous satellites on the dayside and Geotail in the tail region. The predicted MP location based on our model is shown in the above figure where geosynchronous and Geotail satellites are also shown. This model predicts correctly the MP crossings on the dayside and also correctly for the Geotail crossing. It will be implemented at NOAA's Space Environmental Center as a space weather monitor.

This research project is being carried out in collaboration with Prof. C. T. Russell of UCLA and Dr. P. Song of the University of Michigan. Currently we are working on the improvement of the model, particularly for extreme space weather conditions.

References:
Chapman, S. and V. C. A. Ferraro, A new theory of magnetic storm, I. The initial phase, J. Geophys. Res. 36, 77, 1931.
Dungey, J. W., Interplanetary magnetic field and the auroral zones, Phys. Rev. Lett., 6, 7, 1961.
Shue, J. H., J. K. Chao, H. C. Fu, C. T. Russell, P. Song, K. K. Khurana, and H. J. Singer, A new functional form to study the solar wind control of the magnetopause size and shape, J. Geophys. Res., 102, 9497, 1997.
Shue, J. H., P. Song, C. T. Russell, J. T. Steinberg, J. K. Chao, G. Zastenker, O. L. Vaisberg, S. Kokubun, H. J. Singer, T. R. Detman and H. Kawano, Magnetopause location under extreme solar wind conditions, J. Geophys. Res., 103, 17,691, 1998.
Jih Kwin Chao
T272362@twncu865.ncu.edu.tw
Jih Hong Shue
Jhshue@stelab.nagoya-u.ac.jp

CONNECT WITH THE SPACE SCIENCE INSTITUTE FOR EDUCATION AND PUBLIC OUTREACH
Please note the corrected web address.

The Space Science Institute (SSI) is offering to work with PIs to design, develop, and manage all phases of effective Education and Public Outreach (E/PO) programs. Education and Public Outreach has taken on new importance with one to two percent of flight project proposals required to include an Education and Public Outreach segment. The Space Science Institute is a nationally recognized center of excellence for the integration of scientific research, education and public outreach programs in the space and earth sciences. SSI's experience and capabilities include curriculum materials development, exhibit development, professional development for scientists and educators along with partnerships with science centers and museums, industry and government. SSI offers E/PO workshops for scientists in the Spring of each year and additionally offers custom-designed workshops at your site. The E/PO segment of your proposal will be strengthened by including a custom-designed workshop training for your mission team. The Space Science Institute is a national leader in space weather education and has developed the national touring exhibition "Electric Space, Bolts, Jolts and Volts from the Sun." currently displayed in Arkansas. Contact the Space Science Institute for development, design and management of the E/PO segment of your next proposal. Susan Solari, Space Science Institute, 1540 30th St., Suite 23, Boulder,CO 80303-1012, 303.492.5184, solari@colorado.edu, Web address:
http://www-ssi.colorado.edu
Susan Solari
solari@colorado.edu

THE JAPANESE MARS ORBITER, PLANET-B, LAUNCHED SUCCESSFULLY

The Japanese Mars orbiter, PLANET-B, was successfully launched from Uchinoura, Japan, at 18:12 UT on July 3 into a translunar orbit. It was named "Nozomi" in Japanese, which means "hope" in English. Nozomi will leave the Earth on December 20 by using the Earth gravity assist after swingbyes twice with the Moon in the translunar orbit, and arrive at Mars on October 11, 1999.

The main objective is to study the Martian upper atmosphere/ionosphere and its interaction with the solar wind. Nozomi carries 14 instruments with total weight of 35 kg, of which the functional test on orbit will be carried out in a month.
Koichiro Tsuruda, tsuruda@stp.isas.ac.jp

INFORMATION ON THE INTERBALL SUBSATELLITE MAGION-5

May 18, 1998.
MAGION-5, the INTERBALL-Auroral Probe Subsatellite was successfully reactivated on May 7, 1998, after 20 months in space.

It was launched on August 29, 1996, together with the INTERBALL-2 spacecraft (the AURORAL PROBE) into an elliptic orbit with apogee to 20,000 km and inclination of 65 deg (as the last one of the four INTERBALL-Project satellites.) After only one day of operation, on August 30, 1996, MAGION-5 went out of control and ceased to transmit telemetry data for a critical deficit of power. After analyzing the telemetry data and after spare subsystems laboratory tests, it was concluded that the failure was caused by a short circuit in the solar array and it was decided to continue periodically in attempts to reactivate the spacecraft.

The first telecommand response from MAGION-5 was achieved at the Panska Ves TC/TM station of the Institute of Atmospheric Physics (Czech Academy of Sci.) on May 6 and on May 7, 1998. All the principal subsystems of MAGION- 5 were successfully activated. The following 10 days were devoted mainly to tests of the power-subsystems, attitude control and housekeeping measurements. Regular data acquisition including housekeeping as well as scientific information was started at Panska Ves on 17 May, 1998. Detailed testing of the scientific payload continues. The orbit of MAGION-5 is essentially the same as the orbit of the AURORAL PROBE and the distance between the two s/c has been estimated to be about 15 minutes and 20 seconds (approximately 3000 km in apogee.)

After a reasonable interval of simultaneous measurements at this distance it is proposed to reduce the distance between MAGION-5 and AURORAL PROBE to only some hundreds of km. The joint program of operation of the INTERBALL spacecraft will be continued.
Pavel Triska
(P.I. MAGION-5, Subsatellite Project Scientist, Czech Side)
L.M.Zeleny (INTERBALL Project Coordinator)
Yu.N. Agafonov (Subsatellite Technical Manager, Russia) yagafonov@romance.iki.rssi.ru

ACADEMICIAN GELIY ZHEREBTSOV'S 60TH BIRTHDAY

In celebration of Academician Geliy Zherebtsov's 60th birthday on September 17, 1998, a colloquium will be held at the Institute of Solar-Terrestrial Physics in Irkutsk, Russia.

Geliy Zherebtsov is well known in the scientific community for his work on polar ionosphere dynamics, radio wave propagation, solar and geomagnetic activity influence on the upper atmosphere state, and substorm effects in the ionosphere. His results have found their application in solving many important practical problems. He is author or co-author of more than 170 publications. His talent as an organizer was first displayed in 1964 at the polar region of Siberia, near the city of Norilsk, where he created a new observatory with a broad spectrum of scientific tasks. In 1981 he was appointed to the post of Director of the Siberian Institute of Terrestrial Magnetism, Ionosphere and Radio Wave Propagation (now Institute of Solar-Terrestrial Physics.) In this new position he is able to pursue the development of new scientific and technological directions in the Institute. They are:
Geophysical environment impact on workability of satellite equipment,

Development of the Earth monitoring center using satellite data, and

Application of military incoherent scattering radar to solve problems of the upper atmosphere sounding.

The latter point gave occasion to the development of a joint program for upper atmosphere investigation which is executed now in cooperation with Massachusetts Technological Institute, USA.

In 1998, G. Zherebtsov was appointed to the post of Vice-Governor of the Irkutsk region in science and technology politics continuing him in office of Director of the Institute. The colloquium will take place on Thursday, September 17, 1998.
V. Mishin , V. Grigorev,
G. Smolkov, G. Kuklin ,
V. Kovalenko, A. Potapov,
A. Potekhin

FINAL STEP HANDBOOK PUBLISHED

The final STEP publication: Proceedings of the Eighth Workshop on Technical and Scientific Aspects of MST Radar is printed and in the mail. In 360 pages it contains some 68 papers given as oral presentations and 21 papers given in poster sessions. The papers are essentially 4-page extended abstracts.

The School on Atmospheric Radar (SAR) was held 10-13 December 1997 at Tirupati/Gadanki, India; and the Eighth International Workshop on Technical and Scientific Aspects of MST Radar (MST8) was held in Bangalore, India, following SAR on 15-20 December. Brief reviews of SAR and MST8 and appendices about related topics, actions, and future possibilities are included.

Publication of the Handbook was paid for by authors' fees and SCOSTEP subsidy. Some 230 copies were mailed to authors and Bureau members. About 40 copies were sent to a list of international libraries.

Mrs. Belva Edwards, former SCOSTEP Secretariat office secretary edited and assembled the publication. The books were printed in Boulder, Colorado. A few undistributed copies are available at the Secretariat.
JHA

JOB ANNOUNCEMENT - NRL POSTDOCTORAL POSITION IN SOLAR AND TERRESTRIAL VARIABILITY

Applicants are sought for a postdoctoral position in the Solar Terrestrial Relationships Branch of NRL's Space Science Division to study solar radiation variability and, in conjunction with NRL's Upper Atmosphere Physics Branch, the impact of this variability on the Earth's atmosphere. A focus of the work will be the utilization and improvement of in-house models of solar radiative output, especially in the EUV and X-ray spectrum, and of in-house upper and middle atmosphere models to characterize and interpret terrestrial impacts.

Planned research initially includes the utilization of a variety of ground- and space-based solar flux and image data to improve the time-dependent representations of the spectral irradiance models. One- and two-dimensional, theoretical and semi-empirical middle and upper atmosphere models will utilize these representations to simulate solar forcing of the stratosphere, mesosphere and lower thermosphere. Opportunities exist to extend and augment these tasks with a broader range of solar-terrestrial research within the larger on-going effort at NRL to model and understand the mechanisms of solar spectrum variability at X-ray, EUV and UV wavelengths and their terrestrial impacts in support of ongoing and upcoming spacecraft missions (Yohkoh, UARS, SOHO, TIMED, Solar B.) Experience with IDL in a UNIX environment would be an advantage.

This position is available starting immediately for 1 to 3 years, depending on funding. The stipend is $42,000, depending on experience. U.S. citizenship is required in order to be eligible for the required security clearance. For further information, please contact Judith Lean (lean@demeter.nrl.navy.mil), John Mariska (mariska@aspen.nrl.navy.mil), or David Siskind (siskind@uap.nrl.navy.mil).
Judith Lean lean@demeter.nrl.navy.mil

JOB ANNOUNCEMENT - RESEARCH ASSOCIATE IN VIRTUAL REALITY/SCIENTIFIC VISUALIZATION AT THE UNIVERSITY OF WARWICK

Applications are invited for a Research Associate in Virtual Reality Research in the Physics Department at the University of Warwick. This post is part of a recent joint HEFCE-SGI initiative to create an interdisciplinary team for Virtual Reality research at Warwick, with particular emphasis on Space Plasma applications.

The post is to facilitate the application of semi and fully immersive VR techniques as tools for analysis and interpretation of complex data that are generic in both large scale numerical simulation, and multiinstrument datasets. The post requires an ability to liaise with science teams from a variety of disciplines and also the SGI VR development team. It will provide an unparalleled opportunity for the successful candidate to gain expertise in current fully and semi immersive VR technology as it is developed and prototyped.

The successful candidate will have a strong background in mathematics, computational science, or the physical sciences and demonstrated expertise in C, C++ in a UNIX environment. Expertise in scientific visualization, including development with packages such as OpenGL, AVS is also highly desirable.

The appointment is on the RA1A scale and is initially for a fixed term of two years with a possible further year extension.

To apply, send a resume, publication list, statement of research interests, previous relevant technical experience and the names of at least three referees to:

S. C. Chapman, Physics Dept., University of Warwick, Coventry CV4 7AL, UK Email sandrac@astro.warwick.ac.uk fax +44 (0)1203 692016

emailed applications should be in plain text or Latex. Details may also be found on http://www.astro.warwick.ac.uk/vrpost.html

MEETING REPORTS INTERNATIONAL SYMPOSIUM ON DYNAMICS AND STRUCTURE OF THE MESOPAUSE REGION (DYSMER)
March 16 - 20, 1998, Kyoto, JAPAN

The International Symposium on Dynamics and Structure of the Mesopause Region (the DYSMER Symposium) was held in Kyoto at the Radio Atmospheric Science Center (RASC) of Kyoto University on March 16-21, 1998. The Symposium was devoted to the dynamics and structure of the mesosphere and lower thermosphere, with particular emphasis on wave propagation, interaction, and instability processes that shape this region.

The advisory board of the DYSMER Symposium was composed of Prof. C.-H. Liu, Prof. Hiroshi Oya, and Prof. Susumu Kato. The Symposium was organized by an international Program Committee, including Peter Dyson, David C. Fritts (Co-Chair), Shoichiro Fukao, Hiroshi Fukunishi, Maura E. Hagan, Kiyoshi Igarashi, Saburo Miyahara, Chikao Nagasawa, Akio Nomura, Shoichi Okano, Yuri Portnyagin, Gordon G. Shepherd (Co-Chair), Hisao Takahashi, and Toshitaka Tsuda (Secretary.) The local organization was under the direction of T. Tsuda and T. Nakamura of RASC, Kyoto University.

The DYSMER Symposium was primarily organized within the framework of PSMOS (Planetary Scale Mesopause Observing System) of SCOSTEP, and it had joint scientific co-sponsorship by ICMA (International Commission on the Middle Atmosphere) of IAMAS, the Society of Geomagnetism and Earth, Planetary and Space Sciences (SGEPSS), the Meteorological Society of Japan, and the Communications Research Laboratory (CRL.) A total of 126 scientists from 15 countries attended the Symposium, whereof 51 were from outside Japan. The DYSMER Symposium was opened with welcoming speeches by T. Tsuda, D. C. Fritts, and G. G. Shepherd. The Vice President of SCOSTEP, Prof. H. Oya, extended a message, noting the importance of the PSMOS project as a post-STEP activity.

The main topics of the symposium were ground-based radar/optical observations, satellite and rocket measurements, modeling and theory of atmospheric wave and turbulence processes near the mesopause, and the implications of these processes for transport and diffusion. The five full days of the Symposium were composed of eight main sessions: (1) Gravity waves and turbulence (chairs: W.K. Hocking, D.C. Fritts, and R.A. Vincent), (2) Atmospheric tides (chairs: S.K. Avery and M.E. Hagan), (3) Planetary waves (chairs: J.M. Forbes, Yu.I. Portnyagin, and A.H. Manson), (4) Layered structure (chairs: U.-P. Hoppe and C.S. Gardner), (5) Thermal structure of the mesopause (chair: C. Nagasawa and F.-J. Luebken), (6) Neutral wind in the lower thermosphere (chair: H. Fukunishi), (7) Global structure of airglow (chairs: H. Takahashi and W.E. Ward), and (8) Small scale structure of airglow (chairs: M.J. Taylor and S. Fukao.)

A diverse group of experimentalists, modelers, and theoreticians having a common middle atmosphere dynamics focus was brought together. A total of 85 papers were presented at the Symposium, where 61 presentations, including 30 solicited papers, were given orally, and 24 were displayed as posters. Many of them were accompanied by lively and productive discussions. Most of the papers presented at the Symposium will be published in a special issue of Earth, Planets and Space (EPS.)

In association with the scientific sessions, group discussions were organized in order to promote the PSMOS project. The Symposium participants were separated into five working groups: Optical winds and temperatures (WG-1: J. Sheer), Radar winds (WG-2: W. Singer), Optical emissions and imaging (WG-3: J. Stegman), Planetary-scale description (WG-4: A. Pogoreltsev), and Modeling (WG-5: M. Hagan). Separate group discussions and a general meeting took place in the evenings on March 16 and 17, and the PSMOS Steering Committee Meeting was held on March 18.

(Refer to the PSMOS website at http://www.hao.ucar.edu/psmos/home.html for details of the PSMOS working group discussions.)

At a final plenary session, presided over by Prof. G. G. Shepherd, session chairs assessed current understanding of the diverse dynamical processes defining the structure and variability of the mesopause region and its coupling to higher and lower altitudes. The DYSMER symposium coincided with the beginning of post-STEP projects, and successfully contributed to the PSMOS project by identifying unresolved issues that must be pursued in collaboration with SRAMP and EPIC -- companion projects within SCOSTEP.

Following the Symposium, participants were invited to a bus tour on March 21 to the MU radar facility in Shigaraki, and further joined an excursion to a historic castle in Hikone.
Toshitaka Tsuda
tsuda@kurasc.kyoto-u.ac.jp

IACG CAMPAIGN #2 DURING THE COSPAR ASSEMBLY

On July 14, during the COSPAR Assembly in Nagoya, we had a meeting for the Inter-Agency Consultative Group's (IACG) Campaign #2 on boundary layers. It was the first opportunity for people interested in this campaign to get together. It was held in a room with the capacity of 24 people, and about 15 people attended by the end of the meeting. We campaign coordinators are grateful for them. The coordinators first presented the overview of the campaign, with the major stress placed on the official webpage for the campaign
http://www-ssc.igpp.ucla.edu/IACG/.

Events under study were then briefly introduced by the coordinators and a participant. Events on Feb. 11, 1998 and May 4, 1998 were suggested as new campaign events. (The former event was chosen because of the closeness of EQUATOR-S and GEOTAIL and their encounters with the low-latitude boundary layer. The latter event was chosen because POLAR encountered the magnetosheath and even the bow shock during the event.) The participants, including PIs of the ISTP satellites, agreed. In regard to the former event, we had also obtained an agreement from Prof. Haerendel, the project scientist of Equator-S. As written in the official web page, each campaign event is to have its event coordinator(s), who are basically selected on a voluntary basis. Please look at the webpage for more detail. Finally, we note that the latest information on possible future campaign events, including satellite positions for them, might be found at http://www.iki.rssi.ru/vprokhor/camp2.htm to which one can go from the official homepage on Campaign #2.
S. Savin
ssavin@mx.iki.rssi.ru

FORTHCOMING MEETINGS

FIFTH LATIN-AMERICAN CONFERENCE ON SPACE GEOPHYSICS (V-COLAGE)
3-7 November 1998, San Jose, Costa Rica

The Fifth Latin American Conference on Space Geophysics (V-COLAGE) is organized by the Laboratorio de Investigaciones Atmosfericas y Planetarias (LIAP) of the Escuela de Fisica, Universidad de Costa Rica (UCR.) It is sponsored by the Asociacion Latinoamericana de Geofisica Espacial (ALAGE), with the support of COSPAR, IAGA, SCOSTEP and various other international, Latin American and local organizations.

General Program
The activities of the V-COLAGE will consist of three types of sessions: invited talks, poster sessions, and workshops on specific topics with oral presentations and group discussions. These workshops are:

1. "Space Weather". Organizer: W. Gonzalez (INPE, Brazil).
2. "Latin American Scientific Satellites". Organizers: G. Bisiacchi (UNAM, Mexico) and M. Machado (CONAE, Argentina).
3. "Planets and Minor Bodies". Organizers: A. Poveda and M.A. Herrera (UNAM, Mexico).
4. "Geomagnetic Variations". Organizer: J. Marques da Costa (INPE, Brazil).

Confirmed Invited Speakers and Corresponding Titles:
M. Acuna (NASA, USA), Mars Surveyor.
H. Campins (Univ. Florida, USA), Comets: Cosmic Fossils.
S. Cauffman (NASA/GSFC), Space Environment Monitor Instruments Used by Geostationary Operational Environmental Satellites (GOES) for Space Weather Prediction.
F. Chang-Diaz (NASA/JSC), The Interplanetary Propulsion Project.
J. Costa (USP, Brazil), Solar Radio Astronomy.
J. Fernandez (Univ. Nac. Uruguay, Uruguay), Comets: Bodies Holding Valuable Keys about the Solar System Origin.
E. Friis-Christensen (Danish Space Res. Institute), Long- Term Variations in Solar Activity and the Effects on Climate.
R. M. Haberle (NASA/Ames Research Center), Mars Atmospheric Dynamics.
V. Jones (NASA, USA), The NASA Balloon Program.
J. Joselyn (NOAA, USA), Heliospheric Climate.
B. Lazo (IGA, Cuba), Ionospheric Fluctuations.
P. Martens (ESTEC, The Netherlands), Scientific Highlights from SOHO.
A. Mendis (UCSD, USA), Dusty Plasmas.
J. Morales (UCLA, USA), Laboratory Plasma Experiments Under Cosmic Conditions.
J. Roederer (Univ. Alaska, USA), Energetic Particles in Jupiter's Magnetosphere.
G. Rostoker (Univ. of Alberta, Canada), Sun-Earth Relationships.
D. Sentman (Univ. Alaska, USA), Electric Discharges in the Upper Atmosphere.
H. Sobral (INPE, Brazil), The Brazilian Scientific Satellite.
B. Tsurutani (JPL, USA), The Solar Probe Mission.
J. Valdes-Galicia (UNAM, Mexico), Solar Neutrons.
K. Yumoto (Univ. Kyushu, Japan), Magnetic Pulsations.

Registration and Site of the Sessions
The registration fee for participants is US$ 180; the registration fee for accompanying persons is US$ 40. These fees will be collected at the beginning of the Conference. Payment must be in cash (US dollars or Colones). The registration fee will cover, in addition to the program and abstract booklet for the participants, attendance of the welcome reception and refreshments during the breaks.
Meeting Site: The sessions will be held at the Hotel Best Western Irazu (Hotel Irazu) in San Jose. Room rates, including taxes, are:

a. Single, premier.............................. US$ 71.47
b. Double, premier.............................US$ 80.09
c. Single, standard............................. US$ 59.83
d. Double, standard........................... US$ 68.45
e. Triple, standard.............................. US$ 80.00

The rates include: Superior continental breakfast, Free open bar (6-7 p.m.) during the meeting, Transport to airport at departure, Local calls.

The cost of the buffet lunch is US$ 12.30 per person, including taxes.

To make your lodging reservation you must contact the hotel directly at: Hotel Best Western Irazu, ATT: Tannia Davila Apartado 962-1000, San Jose, COSTA RICA
Fax: +506 231-6485; Tel.: +506 232-4811
Email: bestwestern@irazu.co.cr
tdavila@irazu.co.cr

Please indicate that you will participate in the V-COLAGE. A copy of your lodging reservation message must also be sent to the Local Organizing Committee.

NOTE THAT THE V-COLAGE WILL TAKE PLACE DURING HIGH TOURIST SEASON IN COSTA RICA; therefore you are urged to make all your reservations as soon as possible, and in any case, before 30 September 1998.

Visas and Currency:
It is the responsibility of the participants to obtain their visas, if needed. For information contact your international airline or the nearest Costa Rican consulate. The national currency unit is the "colon"; 1 US$ = 250 Colones, approximately. US dollar bills and travelers checks can be exchanged at banks and some money exchange bureaus. It is not recommended to bring currencies from other countries. The hotel and many stores accept the main credit cards.

For additional information contact the Local Organizing Committee: Dr. Walter Fernandez, Laboratorio de Investigaciones Atmosfericas y Planetarias, Escuela de Fisica, Universidad de Costa Rica, San Jose 2060, COSTA RICA
Email: wfer@cariari.ucr.ac.cr,
Fax: +506 207-5619; Tel.: +506 207-5394.
Juan G Roederer, jgr@geewiz.gi.alaska.edu

FALL AGU SPECIAL SESSION SM-08:
MAGNETIC RECONNECTION IN THE SUN-EARTH CONNECTED SYSTEM:
RECENT PROGRESS
6-11 December 1998, San Francisco, CA

In recent years our understanding of the magnetic reconnection process and its consequences has increased considerably. New empirical knowledge was obtained primarily through the analysis of space plasma observations in the ISTP era and through laboratory measurements. Remote and in situ space observations covered the entire Sun-Earth Connected System, ranging from the solar corona, to the Earth's magnetosphere including the magnetopause. These new results were accompanied by new laboratory efforts and progress in theoretical investigations facilitated by the availability of improved and extended numerical models. This session summarizes the state of research involving the process of magnetic reconnection and its consequences and attempts to define directions for future research. Contributions are solicited primarily from observational as well as theoretical reconnection research in the Sun-Earth Connected System but also from recent laboratory experiments addressing related issues.

Conveners:
Michael Hesse, NASA Goddard Space Flight Center Code 696, Greenbelt, MD 20771
hesse@gsfc.nasa.gov
Tsugunobu Nagai, Department of Earth and Planetary Sciences, Tokyo Institute of Technology Tokyo 152-8551, Japan,
nagai@geo.titech.ac.jp

FALL AGU SPECIAL SESSION SM-09:
SUBSTORM ONSET TIMING
6-11 December 1998, San Francisco, CA

The temporal relationship of substorm signatures is an important part of substorm research. Determining the relative timing between signatures leads to clarification of cause-and-effect that contributes to our understanding of substorm onset mechanisms. ISTP and GEM campaigns of multiple satellite and ground station studies have contributed to our understanding of substorm processes. However, much confusion still persists between studies that utilize different substorm signatures for their onset time. Recently it has been suggested to find a readily available and local time-independent relative timing ß for substorm studies. At the last GEM/Snowmass Workshop, mid-latitude pi 2 accompanied with an H component bay was suggested as such a signature. This session seeks contributions that illuminate the substorm timing problem and those that examine the feasibility of using a global, widely available, sub-one-minute-accuracy reference time for substorm onset identification.

The conveners encourage contributed submissions on related topics which are within the scope of the session. All prospective authors of the SM-09 session, including those giving invited talks as well as contributed talks or posters, must submit an abstract which explicitly refers to SPA-SM Session number (SM-09). Please send a copy of your abstract to one of the SM-09 Conveners.

Conveners: Shin Ohtani, Johns Hopkins University Applied Physics, Laboratory, Johns Hopkins Road, Laurel, MD 20723-6099, Phone:+1-240-228-3641, Fax: +1-240-228-6670; Email: ohtani@fluxgate.jhuapl.edu;
Mark Moldwin, Florida Institute of Technology, 150 West University Boulevard, Melbourne, FL 32901, Phone: +1-407-674-7208, Fax: +1-407-674-7482, Email: moldwin@pss.fit.edu
Mark Moldwin

FALL AGU SPECIAL SESSION SH-05:
ORIGIN, INITIATION AND THREE-
DIMENSIONAL STRUCTURE OF CMEs
6-11 December 1998, San Francisco, CA

Observations from the LASCO/SOHO, EIT/SOHO, and SXT/Yohkoh experiments have provided a wealth of observations of CMEs from their earliest stages. These observations and many recent models have demonstrated the importance of the 3-dimensional structure of CMEs. We are organizing a session at the Fall AGU meeting to bring together discussions of the observations and theories related to these topics. We would like to understand what the 3- dimensional structure of a CME appears to be, both at its initiation and as it develops, what this has to do with its acceleration, and whether these structures are evident before the CME eruption. We believe that this should be an exciting topic and welcome the presentation of both observational and theoretical results.

Conveners: K. P. Dere, Space Science Division, Code 7663, Naval Research Laboratory, Washington, DC 20375-5320, phone: 202-767-2161, fax: 202-767-5636, email: dere@halcyon.nrl.navy.mil
R. A. Howard, Code 7666, Naval Research Laboratory, Washington, DC 20375-5320, phone: 202-767-3137, fax: 202-767-5636, email: howard@cronus.nrl.navy.mil
Ken Dere

FALL AGU SPECIAL SESSION U-11:
CLIMATIC EFFECTS OF A CHANGING SUN
6-11 December 1998, San Francisco, CA

A half-day Union Session (U-11) "Climatic Effects of a Changing Sun", with additional time for poster papers, will be held during the AGU 1998 Fall Meeting.

Two decades of measurements of both electromagnetic and particle fluxes from the Sun has established conclusively that it exhibits changes on timescales from minutes to decades. Since solar energy is one of the major natural driving forces of the terrestrial atmospheric and climate system, the effect of solar variability on climate change is critical for a wider understanding of the climate response to other influences, including increasing greenhouse gas concentrations.

The major goal of this U-11 session is to summarize the most recent measurements of solar total and spectral irradiance as well as those of particle fluxes, modeling and interpreting the observed irradiance and particle flux variations, and the climate effect of solar variability. The following major topics will be covered:
(1) Variations in Total Solar Irradiance and their Physical Basis
(2) Variations in Spectral Irradiance and their Physical Basis
(3) Long-term Solar Indices and Solar Scenarios
(4) Climate and Irradiance, Atmospheric Chemistry and Dynamics--Direct and Indirect Solar Influences
(5) Effect of Solar and Cosmic Particles on Earth
(6) Observational Climate Records

The conveners encourage contributed submissions on other related topics which are within the scope of the session. All prospective authors of the U-11 session, including those giving invited talks as well as contributed talks or posters, must submit an abstract which explicitly refers to UNION Session number (U-11.) Please send a copy of your abstract to the U-11 Lead-Convener, Dr. Linton Floyd. The conveners are:
Dr. Linton Floyd (floyd@susim.nrl.navy.mil),
Dr. Judit M. Pap (pap@astro.ucla.edu)
Dr. Claus Frohlich (claus@obsun.pmodwrc.ch),
Dr. Gerard North (northead@ariel.met.tamu.edu).

Dr. Linton Floyd
Code 7660, Naval Research Laboratory
Washington, DC 20375
Phone: 202-767-2258, Fax: 202-767-5636
Linton Floyd, Judit Pap
Claus Frohlich, Gerard North.

RADAR OBSERVATIONS OF METEORS:
ISSUES AND RESULTS
1999 URSI National Meeting
January 4-8, 1999, Boulder, CO

The recent advent of narrow-beam V/UHF radar observations of meteors plus reports of interstellar meteors and interest in the effects of meteor showers on space systems has led to a resurgence of interest in meteor science. As a measure of this interest, last year's meteor session resulted in 14 papers.

Again this year papers are sought on the current state of radar meteor science from both observational and technological viewpoints. Emphasis should be given on outstanding problems such as meteor head/tail-echo scattering mechanisms and velocity determination and the technology needed to solve these problems.

Contributed papers are 20-minutes, while invited papers may be 40-minutes depending on available time.

General information, including abstract submission instructions and guidelines, may be found by consulting the URL: http://cires.colorado.edu/ursi

Email submittal of abstracts is suggested. A copy of the abstract should also be sent directly to the session organizer: Joint G/H Session Organizers: John D. Mathews (JDMathews@psu.edu) and Qihou Zhou (zhou@naic.edu)
John D. Mathews

SPECIAL SESSION ON IONOSPHERIC HEATING
1999 URSI National Meeting
January 4-8, 1999, Boulder, CO

Papers are sought, in particular, concerning the new results from recent Arecibo and HAARP campaigns, but papers on all topics are encouraged. Recent up-grades to facilities have provided increased power densities and afforded new opportunities to generate nonlinear effects in the ionospheric plasma.

General information, including abstract submission instructions and guidelines, may be found by consulting the URL: http://cires.colorado.edu/ursi

Email submittal of abstracts is suggested. A copy of the abstract should also be sent directly to the session organizer:

Commissions G and H Session Organizer:
Michael P. Sulzer (msulzer@naic.edu)
Michael P. Sulzer

SECOND ANNOUNCEMENT FOR THE
CHAPMAN CONFERENCE ON
MAGNETOSPHERIC CURRENT SYSTEMS
11-15 January 1999, Kona, Hawaii
(A student session may start on January 10 -- see below.)
Editor's Note: See International SCOSTEP Newsletter, Vol. 1, No. 2, June 1998, page 12, for the first announcement.

This Chapman Conference will target outstanding issues related to magnetospheric current systems placing its emphasis on inter-regional processes and driving mechanisms of current systems. The Conference will provide an ideal opportunity to discuss recent observational and theoretical achievements and will foster communication among people working with different approaches.

1) IMPORTANT DEADLINES
Abstract deadline:............... September 30, 1998
Preregistration deadline:...... December 11, 1998

2) AGU WEBSITE
AGU has set up a web site for this conference at http://www.agu.org/meetings/chapman.html which provides general information about the conference.

3) LIST OF TUTORIAL/INVITED SPEAKERS
The following is the present list of invited speakers (all confirmed):
Tutorial speakers: Cowley, Iijima, Kivelson, Parker, Richmond
Invited speakers: Carlson, Connerney, Elphic, Glassmeier, Gombosi, Greenwald, Hesse, Hughes, Iyemori, Jacquey, Janhunen, Kaufmann, Khurana, Lockwood, Lu, Lyon, Lysak, Marklund, Opgenoorth, Pontius, Pulkkinen, Samson, Siscoe, Slavin, Sonnerup, Tanaka, Temerin, Thayer, Toffoletto, Tsyganenko, Wolf, Yamauchi

4) SESSION OF INNOVATIVE STUDIES
We are planning to have a session about innovative studies. The session will emphasize future possibilities rather than present achievements. We encourage contributed submissions on new theoretical concepts, new experimental plans, or new methods of data analysis and simulation which are expected to have an impact on future studies of magnetospheric current systems.

A limited number of oral presentation spots are available for this session. Contributors are asked to inform either convener about their intention when submitting an abstract.

5) STUDENT OPPORTUNITY
We are looking for volunteer students to organize a student session during the Conference. The session can be used, for instance, for presenting papers to each other (the number of oral presentations is extremely limited at regular sessions) or inviting lecturers. We simply provide the place and time for the session, and all details will be decided by the student program committee. Anyone who is interested may contact either convener at the email address found at the end of this message.

Limited funding will be available for students to attend the Conference. More information can be found at http://www.agu.org/meetings/chapman.html. The travel application must be received by AGU by September 30, 1998.

6) AGU Monograph
We seek to publish an AGU monograph to report the achievements of this Conference. Details will be announced later.
Ryo-ichi Fujii and Shin-ichi Ohtani (Conveners)
Email: rfujii@stelab.nagoya-u.ac.jp or ohtani@jhuapl.edu

DYNAMICS OF THE MAGNETOSPHERE AND
ITS COUPLING TO THE IONOSPHERE ON
MULTIPLE SCALES USING INTERBALL,
ISTP, AND GROUND-BASED OBSERVATIONS
8-13 February 1999, Zvenigorod (near Moscow), Russia

New achievements in satellite instrumentation, the availability of simultaneous multipoint observations, and rapid advances in numerical simulations allow us to study various fundamental problems not only in magnetospheric and ionospheric physics but also in basic plasma physics. We propose to hold a meeting designed to integrate these efforts and identify future opportunities for cooperative studies.

The INTERBALL space mission (INTERBALL-1 with its subsatellite MAGION-4 in orbits with an apogee of 30 Re, and INTERBALL-2 with its recently reactivated MAGION-5 subsatellite in orbits with an apogee of 3 Re) continue to provide a vast quantity of solar wind, magnetosheath, and magnetospheric observations as part of an unprecedented "fleet" of spacecraft now in orbit which includes GEOTAIL, AKEBONO, WIND, SOHO, POLAR, and FAST, together with several low-altitude and geosynchronous satellites, and an extensive network of well-organized supporting ground-based geophysical observatories.

The INTERNET and direct contacts have enabled numerous effective cooperation projects between the various satellites teams. SCOSTEP guidance played a significant role in international efforts to ground-based and satellite observations. IACG (Inter Agency Consulting Group) campaigns 1 and 2 on "Nonlinear dynamics in magnetotail" and "Boundaries in Collisionless Plasma" gave an added impetus to joint studies. This makes coordinated efforts especially fruitful.

It should be noted that some of the INTERBALL Project results were already published in special issues of Ann. Geophys., v.15, N 5, 1997; Cosmic Research, v.36, N 1 and N 3, 1998, and some are in preparation (Ann. Geophys., 1998; Cosmic Research, v.36, N 6, 1998; N 3, 1999.) Besides, many papers are already published in other journals.

Now is the time to further stimulate the fruitful analysis of these multipoint measurements, modeling and theoretical efforts to deepen the understanding of space plasmas, substorm and storm processes, nonlinear and/or stochastic behavior of the real near-Earth's plasma, properties of magnetopause, cusp, mantle and boundary layers.

As a part of these efforts, the Space Research Institute (IKI, Moscow) will organize a topical symposium entitled "Dynamics of the Magnetosphere and its Coupling to the Ionosphere at Multiple Scales from INTERBALL, ISTP Satellites and Ground-Based Observations" during February 1999 at Zvenigorod (a resort 50 km from Moscow.) The meeting will focus on INTERBALL results, but certainly will include results from other space projects on these topics and related modeling and theoretical research. The total number of participants is expected to be about 100-150 (based on our experience at the preceding Workshop in Finland, during February 1998.) At the Workshop homepage (http://www.iki.rssi.ru/interball/Zvenigorod_Symposium/) we have placed a detailed list of the main topics which the members of the INTERBALL community are currently studying. We will try to give some preference to presentations directly related to these topics. Our aim is to concentrate efforts on studies of important new problems which can be addressed by the multiple scientific payloads of the ISTP program.

PRELIMINARY SUGGESTIONS FOR THE MAIN
SCIENTIFIC TOPICS OF THE ZVENIGOROD MEETING
February 8-13, 1999

1. Acceleration - Spontaneous Reconnection in the Tail, BBF, Bursty Convection
2. Thermal and Superthermal Plasma
3. Plasma Boundaries in Near-Earth Space
4. Auroral Acceleration Region - Particles and Fields
5. Solar Wind and IMF Features and Their Interaction with Outer Magnetosphere

We also plan to discuss briefly some new Russian space projects in the magnetospheric physics and possible international cooperation in their accomplishment.

The detailed list of these topics with the names of the panel discussion organizers can be found on the workshop homepage.

We would be grateful for your comments, additions and corrections to the preliminary proposals for the Program of Zvenigorod Symposium.

At the workshop homepage you will also find social information about Zvenigorod, sightseeing possibilities in this area, and the approximate cost of accommodation. Please, come and try a real Russian Winter!

Please visit the workshop homepage and complete the online registration form for the Zvenigorod meeting.
Lev Zelenyi
Scientific Coordinator of the INTERBALL Programme
Space Research Institute of RAS
84/32 Profsoyuznaya Str. Moscow 117810, Russia
Phone: +7 095 333 11 22; Fax: +7 095 310 70 23
Email: lzelenyi@iki.rssi.ru

LONG-TERM CHANGES AND TRENDS IN THE
ATMOSPHERE (LT-ACT'99)
16-19 February 1999, IITM, Pune, INDIA

Information on this meeting can be found at the following Website of our homepage: http://www.iucaa.ernet.in/iitm.html

I invite you to participate in this exciting scientific event and make it a success. I request you to kindly view this site and return the attached Pre-registration form at your earliest. If you are unable to view the above Website then kindly let me know in the following email address so that we can send you the text by email. LTACT@tropmet.ernet.in
Gufran BEIG
Scientific Secretary, LT-ACT'99
IITM, PUNE, INDIA

PIERS 1999:
PROGRESS IN ELECTROMAGNETIC
RESEARCH SYMPOSIUM
22-26 March 1999, Taipei, Taiwan

Main Session on
RADAR APPLICATIONS FOR ATMOSPHERE AND IONO-SPHERE RESEARCH

PIERS provides an international forum for reporting progress and recent advances in the modern development of electromagnetic theory and its applications. Among 28 session topics are, for instance (only those listed here, which have some relevance to radar): antenna theory, RF and microwave circuits, EMC, computational and numerical techniques, waves in composite and complex media, guided waves and propagation, tropospheric and ionospheric propagation, propagation and radio communications, wavelets in electromagnetics, remote sensing of earth, ocean and atmosphere, surface and volume scattering, random media, nonlinear and turbulent media, near- and far-field measurements, SAR and SAR interferometry, inverse scattering, and there is also the topic on RADAR APPLICATIONS FOR ATMOSPHERE AND IONOSPHERE RESEARCH (main convener:Jurgen Röttger), which is subdivided into:

(1) Precipitation studies with weather surveillance and wind profiling radars.
(2) MST radars and wind profilers.
(3) MF and meteor radars.
(4) HF radars: SuperDARN, digital ionosondes, OTH.
(5) Incoherent and coherent scatter radars.

Each of these session should have about 7-10 papers, and several of these should be solicited or invited. The papers should have relevance to the main direction of the symposium, namely "progress in electromagnetic research." That means the subjects should not so much be dominated by geophysical results although such results should not be excluded, particularly when they justify the design philosophy of systems, projects or programs and yield innovative geophysical or meteorological findings.

Sessions: (1) Precipitation studies with weather surveillance and wind profiling radars (convened by: D. Zrnic, K.S. Gage.) Both weather surveillance and wind profiling radars detect signals from precipitation. In this session we focus attention on this common attribute of meteorological radar, i.e., observation of hydrometeors. Scanning radars have a long history of providing a real coverage for tracking severe storms and estimating precipitation. The addition of polarimetric capability to these radars has provided possibilities to map hydrometeor fields in unprecedented detail. With the advent of wind profiling, there has been a resurgence of interest in the use of vertically directed Doppler radars for observing the vertical distribution of hydrometeors. Radars on space platforms can provide a truly global perspective of precipitation. In November 1997, the TRMM Precipitation Radar was placed in orbit in a cooperative effort by NASA (USA) and NASDA (Japan.) The TRMM Precipitation Radar provides a major advance in the capability of estimating global precipitation from space. Global estimates of precipitation are needed to better quantify the hydrological cycle, to specify diabatic heating and to validate numerical model simulations.

(2) MST radars and wind profilers (convened by: P. Currier, S. Chakravarty, T. Tsuda.) Clear air turbulent scattering echoes of VHF/UHF radio waves have been studied using MST radar and wind profilers with wide ranging applications in understanding meteorological, atmospheric and ionospheric interactive processes. The main advantage of these studies has been the capability of these systems to acquire data continuously at very high spatial and temporal resolutions, presently not possible with other techniques. Recent developments have shown the efficiency of these radars for providing vital information on winds, clouds, temperature and humidity profiles, rainfall features, cyclogenesis etc. Further innovations will be necessary to cover the main gap area of radar observations between 30-60 km, which is crucial for better understanding of various atmospheric coupling processes.

(3) MF and meteor radars (convened by: D. Thorsen, I. Reid.) Our understanding of the middle atmosphere circulation has increased significantly through the extensive observations of neutral winds obtained from MF and meteor radars. These radars have also been instrumental in the calibration and validation of recent satellite missions such as UARS. Recent developments have shown that these radars can also provide information on temperature (meteor radars) and momentum flux divergence (MF radars) in the mesopause region. As with all instruments, each technique has its strengths and weaknesses which need to be considered when the results are interpreted.

(4) HF radars (SuperDARN, digital ionosondes, OTH) (convened by: T.B. Jones, B. Reinisch, S.J. Anderson.)
(4a) SuperDARN: The coherent backscatter HF radars are powerful tools for studying convection flows in the high latitude ionosphere, providing vector velocities over a very wide observing region with high temporal and spatial resolution. They play a key role in the study of the coupling between the solar wind, magnetosphere and the ionosphere. Recent highlights have included the electrodynamics of the cusp region, magnetospheric substorms, flux transfer events, and the effect of the IMF on ionospheric convection flows. The availability of radars in both northern and southern hemispheres enable conjugate studies to be undertaken.

(4b) Digital Ionosondes: Modern digital ionosondes operate as vertical HF radars that measure range, electron density, Doppler spectrum, and angle of arrival. Since these low cost instruments operate more or less continuously they are an excellent monitor of geophysical events. Vertical profiles, horizontal density structures and velocity distributions can be deduced from these data. Interpretation of these new data requires new concepts that have only just begun to be developed. The session will emphasize new technical developments and observational modes and interpretation techniques, as well as geophysical observations.

(4c) Developments in HF skywave (over-the-horizon (OTH)) radar: The past two years have seen some significant changes in the focus of OTH radar research and applications. Three areas are of particular interest to ionospheric research :
(I) The introduction of sophisticated ameliorative signal processing techniques aimed at mitigating the effects of ionospheric distortion and contamination of radar signals,
(II) The design of HF antennas optimized for specific radar measurements, and (III) The exploitation of HF transmissions of opportunity as channel probes for determining ionospheric structure and dynamics.

The new signal processing techniques incorporate the estimation of ionospheric spatial and temporal fluctuations as a precursor to their removal from the radar returns, while sparse arrays and novel antenna designs optimize resource allocation for ionospheric measurements.

This session will attempt to delineate the state-of-the-art in these areas and to identify priorities for future research.

(5) Incoherent and coherent scatter radars (convened by: J. Kelly, K. Hanuise.)
At VHF or UHF frequencies, ionospheric radars operate as either incoherent scatter radars (Thomson scattering from electrons) or coherent scatter radars (Bragg scattering from field-aligned density fluctuations.) The session will emphasize recent developments in hardware and signal processing techniques for both radar types, in relation to existing, recently developed or future facilities. Among them are incoherent scatter radars and interferometry imaging techniques for coherent scatter radars.

A one page abstract is to be submitted to:
Prof. Kun Shan Chen, PIERS 1999
Center for Space and Remote Sensing Research
National Central University, Chung-Li, Taiwan.

Deadline for abstract submission is 30 September 1998. Guidelines for abstract format can be obtained from: <dkchen@csrsr.ncu.edu.tw> and <maylai@csrsr.ncu.edu.tw>

For more details on PIERS see:
http://piers1999.csrsr.ncu.edu.tw/

4th SEC USER CONFERENCE
19-21 April 1999, Boulder, CO
and
5th RESEARCH-TO-OPERATIONS WORKSHOP
21-23 April 1999, Boulder, CO

In an effort to accelerate and maximize effective transitioning of space environment research results into operations, the Space Environment Center will host a conjoined conference of users, researchers, and vendors the week of April 19, 1999. The 4th SEC User Conference will be held April 19, 20, and 21. The 5th annual Research-to-Operations Workshop, co-organized by Air Force Research Laboratory and NSF Division of Atmospheric Science, will be April 21, 22 and 23. The proximity of the two meetings, one emphasizing research findings and new models and one emphasizing the operational concerns of users, will allow those interested to attend both meetings if they choose. The researchers are invited to attend the wrap-up of the User Conference the morning of April 21. Both groups should plan to attend a joint social evening, April 20.

Additionally, there will be a Space Weather Services Vendor Meeting on April 21. This meeting will allow private sector enterprises access to both researchers (who might generate new products) and users (who might purchase new products.) Vendors may want to attend one or both of the meetings on either side of the vendor meeting.

Details about the conference will be posted by September 30 on Space Environment Center's Website http://www.sec.noaa.gov/AboutSEC. Questions can be directed to Barbara Poppe (bpoppe@sec.noaa.gov).

SCIENCE FOR THE 21st CENTURY
26 June - 1 July 1999, Budapest, Hungary

UNESCO and ICSU are jointly sponsoring a meeting "Science for the 21st Century, A New Commitment." A First Announcement has been mailed and recipients are asked to publicize this meeting. Attendance is limited to 2,000 invited participants to be selected from applications of interested persons. This is billed as "The World Conference on Science." The objectives are to "analyze where the natural sciences stand today and where they are heading, what their social impact has been and what society expects from them. Finally, it will establish what efforts need to be made to make science advance in response to these expectations and to the challenges posed by human and social development."

Participants will come from national governments and institutions, educational and research establishments, members of the scientific community, the industrial sector, intergovernmental organizations (IGOs) and non-governmental organizations (NGOs), as well as the media and the general public. All are welcome, however participation in the Conference itself depends on the space and facilities available. Balance in participants will be sought and a special role is envisioned for financial institutions and specialized agencies of the United Nations.

The World Conference on Science will comprise Forum I - Science: Achievements, Shortcomings and Challenge; Forum II - Science in Society; and Forum III - Towards a New Commitment. Outcomes of the meeting will involve two documents:

· Declaration on Science, to underscore political commitment to scientific endeavor and to solution of problems at the interface between science and society; and

· Science Agenda - Framework for Action, an innovative and pragmatic framework for fostering partnerships in science and the use of science for development and the environment.

Information about the Conference and, presumably, copies of the first announcement are available from Secretariat, World Conference on Science, UNESCO, 7, place de Fontenoy, 75352 Paris, France. Fax: (33) 1 45 68 58 23; and email: confsci@unesco.org. A preliminary attendance form was circulated with the First Announcement, but the cover letter from ICSU requests that only one form per organization be returned. However, the form has a space for those who wish to "attend as an individual."

Maurizio Iaccarino, Asst. Director-General for Natural Sciences, Secretary-General of the World Conference on Science has written encouraging circulation of information about this conference within ICSU body organizations and inviting consideration of sending a delegation to this event.
JHA

SOLAR VARIABILITY AND CLIMATE
18-30 July 1999, Birmingham, U.K.

The 1-day Symposium is to be held during the IUGG99 Assembly and is sponsored by IAGA, IAMAS, and SCOSTEP.

This symposium will discuss the most recent results obtained on solar variability and its effects on the Earth's atmosphere and climate system. Measurements of the solar energy flux (electromagnetic radiation and the emission of charged particles) and understanding its variability are extremely important issues for both solar and atmospheric physics. Measurements of the solar energy flux over the last decades have demonstrated that it varies with the 11-year solar activity cycle, and it has been established that the Earth's climate, radiative environment and upper atmospheric chemistry are influenced by the varying solar energy flux. In addition to the terrestrial implications of solar variability, the observations and interpretation of the variations in the solar energy flux also led to new ways of understanding the structure and dynamics of the Sun on a global scale. The ultimate goal is to understand why, how, and what mechanisms govern solar variability which controls many of the terrestrial processes. This symposium provides an excellent opportunity to bring together the international research community to summarize and discuss the results gained on solar variability and its terrestrial effects.
Convener: Judit M. Pap,
Department of Physics and Astronomy,
University of California, Los Angeles
Box 951562, 405 Hilgard Ave.,
Los Angeles, CA 90095-1562
Phone: 310-825-1289; Fax: 310-206-2096
Email: pap@astro.ucla.edu or jpap@solar.stanford.edu

Co-Convener: Claus Frohlich,
Physikalisch-Meteorologisches Observatorium Davos,
World Radiation Center,
PMOD/WRC, Dorfstrasse 33,
CH-7260 Davos-Dorf, Switzerland
Phone: 41 81 417 51 36; Fax: 41 81 417 51 00
Email: cfrohlich@obsun.pmodwrc.ch or cfrohlich@solar.stanford.edu

The topic of the symposium will cover the following areas: Measurements, results and interpretation of solar total, spectral (near-UV to IR), and UV irradiances; Variations of solar-type of stars; Climate effect of irradiance and particle flux variations; Long-term solar and climate records. The symposium is also related to the "International Solar Cycle Studies (ISCS): Working Group 1, Solar Energy Flux Variations: from the Interior to the Outer Layers." ISCS is an international research program operated under the auspices of SCOSTEP.

The deadline for receiving abstracts is January 15, 1999. Further details can be found in the IUGG99 Birmingham Second Circular - Call for Abstracts. If you wish to receive Circulars for the IUGG99 meeting please contact:

IUGG99 Secretariat School of Earth Sciences
University of Birmingham, Edgbaston
Birmingham B15 2TT, United Kingdom
Phone: +44 121 414 6165, Fax: +44 121 414 4942
Email: IUGG99@bham.ac.uk,
or visit its Website: http://www.bham.ac.uk/IUGG99/
If you have further questions on the Solar Variability and Climate Symposium, please do not hesitate to contact us.
Judit Pap and Claus Frohlich

SOLAR MAGNETIC FIELD:
REVERSALS, POLAR FIELD, DYNAMO
18-30 July 1999, Birmingham, U.K.

The 1-day Symposium GA 4.03 will be held during the IUGG99 Assembly and is sponsored by IAGA, IAMAS, and SCOSTEP.

The Symposium is aimed at reviewing all aspects of cyclic evolution of large-scale fields. One of the main problems today is how to correlate recent observations, showing that the photospheric magnetic field consists of relatively small elements, and the direct and indirect evidence of the existence of global fields. We do not know why the polar field reversal is so rapid and why it does not occur simultaneously at both poles. On the other hand, the open magnetic fields are known to change their sign simultaneously all over the solar disk. The nature of high correlation between variations of the polar field at a cycle minimum and the local fields at the subsequent maximum is not clear. It is also proposed to discuss the generation mechanisms of magnetic fields of large spatial scale.
Convener: Vladimir N. Obridko, IZMIRAN, 142092
Troitsk, Moscow Region, Russia
Phone: (095) 334-02-82; Fax: (095) 334-01-24
Email: solter@izmiran.troitsk.ru or solter@izmiran.rssi.ru

The topics of the Symposium will cover the following areas: Evolution of large-scale fields; Evolution of polar fields; Polarity reversal; Main reference points of the cycle; Present-day state of the solar magnetic field generation theory; Up-to-date methods of long-term forecasting; and Prediction of the current cycle.

This Symposium is also related to the "International Solar Cycle Studies (ISCS): Working Group 1, Solar Energy Flux Variations: from the Interior to the Outer Layers." ISCS is an international research program operated under the auspices of SCOSTEP.

The deadline for receiving abstracts is January 15, 1999. Further details can be found in the IUGG 99 Birmingham Second Circular - Call for Abstracts. If you wish to receive Circulars for the IUGG99 meeting please contact:

IUGG99 Secretariat School of Earth Sciences
University of Birmingham, Edgbaston
Birmingham B15 2TT, United Kingdom
Phone: +44 121 414 6165; Fax: +44 121 414 4942
Email: IUGG99@bham.ac.uk or visit its Website: http://www.bham.ac.uk/IUGG99/
If you have further questions on this Symposium, please do not hesitate to contact me.
Vladimir Obridko

IAGA SYMPOSIUM ON MAGNETIC STORMS
18-30 July 1999, Birmingham, U.K.

A two-day Symposium on "Interplanetary Medium and Geophysical Phenomena During Geomagnetic Storms" is planned for the IAGA Scientific Symposia which will be held during the 22nd General Assembly of the IUGG (University of Birmingham, UK, July 19-30, 1999. The Convener is B. Tsurutani (btsurutani@jplsp.jpl.nasa.gov) of IAGA Division IV, and Co-Conveners are J. Lastovicka (jla@ufa.cas.cz) of Division II, Ya. Feldstein (lgromova@izmiran.troitsk.ru) of Division III, and V. Papitashvili (papita@umich.edu) of Division V.

The Symposium will be composed of invited talks, contributed oral talks, and contributed poster talks. An arrangement has been made with T. Killeen, North-American Editor-in-Chief, to publish the papers in special issues of the Journal of Atmospheric and Solar-Terrestrial Physics. The papers will be refereed and only those that pass the normal standards will appear in the special issues. The topics to be covered are:

1. What (and where) are the events that occur at the Sun that cause magnetic storms at the Earth and can they be predicted with remote observations?
2. What are the interplanetary causes of superintense magnetic storms, substorms and geomagnetic quiet?
3. What are the energetics and topology of the magnetosphere during magnetic storms?
4. What are the developments, possible interactions and decay of the magnetospheric ring current and tail currents?
5. Interplanetary and magnetospheric electric fields during storms: What is most important: steady state fields, fluctuating fields, or both?
6. Magnetosphere-ionosphere coupling: How do oxygen ions get into the storm-time ring current and why is there a delay?
7. Ionospheric and lower thermospheric responses during magnetic storms: Is there a predictable pattern given interplanetary input parameters?
8. Geomagnetic field modeling for magnetic storms and its comparison with observations.

IAGA SYMPOSIUM GA 4.02: CMEs, PROMINENCE ERUPTIONS AND FLARES: ONSETS AND RELATIONSHIPS
18-30 July 1999, Birmingham, UK

This 1-day Symposium is aimed on new insights of CMEs, prominence eruptions and flares and is sponsored by IAGA and SCOSTEP. Instruments on the Yohkoh (SXT), SOHO (CDS, SUMER, EIT, LASCO) and TRACE spacecraft allow us to detect the onsets of CMEs, prominence eruptions and flares and to follow them out to 30 solar radii. In addition, full disk magnetograms from the MDI instrument on SOHO are obtained at a regular cadence that permits studies of the evolution of photospheric fields, which should play a crucial role in the conditions that lead to plasma and magnetic field ejection. These observations are changing our understanding of CMEs in a fundamental way and new theories and models are being developed to explain the new observations. This session will involve the results from both observations and theory/modeling.
Convener: Brigitte Schmieder, schmieder@obspm.fr
Observatoire de Paris, Section Meudon
92195 Meudon Cedex Principal, France
Phone: (33)1 45 07 78 17 Fax: (33)1 45 07 79 17
Co-conveners: K.Shibata (Mitaka, Japan), K. Dere (NRL, Washington USA); S. Plunkett (NRL, Washington, USA), D. Webb (Phillips Lab, USA), T. Hoeksema (Stanford Univ., USA)

The deadline for receiving abstracts is January 15, 1999. Further details can be found in the IUGG99 Birmingham Second Circular - Call for Abstracts. If you wish to receive Circulars for the IUGG99 meeting please contact:
IUGG99 Secretariat School of Earth Sciences
University of Birmingham Edgbaston, Birmingham B15 2TT, United Kingdom
Phone: +44 121 414 6165, Fax: +44 121 414 4942
Email: IUGG99@bham.ac.uk or visit its Website: http://www.bham.ac.uk/IUGG99/
B. Schmieder
(schmieder%mesoph@mesiob.obspm.fr)

INTERNATIONAL WORKSHOP ON RADIO METHODS FOR STUDYING TURBULENCE
9-12 August 1999, Urbana, IL

Preliminary Announcement
Turbulence is a phenomenon common in nature, observed in geophysical and astrophysical, neutral and ionized, media. Specialists working on turbulence, whether in the atmosphere, ionosphere, or solar wind, encounter similar problems with data analysis and interpretation in terms of theoretical models.

The Workshop is intended to meet the general need for an exchange of information and ideas between scientists working on turbulence in various environments. It will bring together experts from all over the world who work on turbulence using radio methods. Emphasis will be put on data analysis, characterization and interpretation, but theoretical results are also welcomed. Participation by Young Scientists (less than 35 years of age at the time of the meeting) is encouraged.

All papers will be presented at plenary sessions. Poster sessions can be arranged if needed. An abstract book will be distributed at the Workshop.

Sponsors:
The Workshop is a joint effort of URSI Commissions: E - Electromagnetic Noise and Interference, F - Wave Propagation and Remote Sensing, G - Ionospheric Radio and Propagation, H - Waves in Plasmas, and J - Radio Astronomy. The Workshop is sponsored by URSI and SCOSTEP but sponsorship by various other scientific organizations is being sought.

Venue:
The workshop will be held at the University of Illinois, Urbana, IL, from Monday August 9th to Thursday August 12th 1999. The first session will start at 9:00 am and the last will end at 12:00 noon.

Registration fee:
Regular - $120US, Young Scientists - $70US

Program and Scientific Committee:
H. Kikuchi (Japan) and S. Moiseev (Russia) (Comm. E), A. W. Wernik (Poland) and K. C. Yeh (USA) (Comm. G), V. Krasnosselskikh (France) and F. Lefeuvre (France) (Comm. H), B. J. Rickett (USA) (Comm. J), + representatives of other sponsors.

Organizing Committee:
Belva Edwards, Steven J. Franke, Erhan Kudeki, Joyce Mast, K. C. Yeh, George Swenson, Jr. (all from University of Illinois at Urbana-Champaign, USA), and Andrzej W. Wernik (Space Research Center, Poland.)

For more information, please contact:
A.W. Wernik, Space Research Center
Polish Academy of Sciences
ul. Bartycka 18a, 00-716 Warsaw, Poland
Tel: +48-22-403766 ext. 379; Fax: +48-22-403131
Email: aww@cbk.waw.pl

MAGNETOSPHERES OF THE OUTER PLANETS CONFERENCE (MOP 99)
9-14 August 1999, Paris France

Preliminary Announcement
According to the ballot organized during the MOP 97 meeting, the MOP 99 will be held in Paris, during the week of the last total solar eclipse of the millennium. Preliminary information is given below. The most important points concern transportation and updating of the mailing list.

Purpose and Format
The conference will follow a series of meetings on the topic of the magnetospheres of the outer planets. The main purpose is to compare and better understand physical processes at work in the magnetospheres of the four giant planets, often with reference to the terrestrial magnetosphere (and with possible application to the magnetospheres of distant astrophysical objects.) Lively discussions are expected to be fed by new data from the Galileo extended mission at Jupiter, UV observations using the Hubble Space Telescope, and ground-based IR and radio observations, as well as continuing (re-)analyses of Ulysses, Voyager or Wind data.

As usual for these meetings, there will be no parallel sessions, ample time for discussion, and posters will be on display all week.

Topics
Topics to be discussed include, but are not limited to:
* Large-scale magnetospheric structure and dynamics.
* Coupling with the satellites and rings.
* Dust distribution and dynamics.
* Io, its plasma torus, and its electrodynamic interaction with Jupiter.
* Auroral phenomena and ionosphere/magnetosphere coupling.
* Small-scale, microscopic processes (particle acceleration and heating, wave-particle interactions...).

Local Organizing Committee
Philippe Zarka Obs. Paris, DESPA, Meudon Philippe.Zarka@obspm.fr
Renee Prange Inst. Astrophys. Spat., Orsay prange@ias.fr
Michel Moncuquet Obs. Paris, DESPA, Meudon Michel.Moncuquet@obspm.fr
Sylvestre Maurice Obs. Midi-Pyrenees, Toulouse smaurice@obs-mip.fr
Alain Lecacheux Obs. Paris, ARPEGES, Meudon alx@obspm.fr
Yolande Leblanc Obs. Paris, DESPA, Meudon Yolande.Leblanc@obspm.fr
Patrick Canu CETP/IPSL, Velizy Patrick.Canu@cetp.ipsl.fr

General Information
Location, still to be finalized, will be downtown Paris.

Dates are Monday 9th to Saturday 14th August 1999. As Wednesday will be off for eclipse viewing (see below), there will probably be sessions on Saturday 14th (morning or whole day, depending on the number of abstracts submitted).

Accommodation: Downtown Paris offers many hotels and restaurants of all categories, as well as a very large selection of social/cultural events. Detailed information will be provided.

Eclipse: The last total solar eclipse of the millennium will take place on Wednesday 11 August, about 1020 AM. The totality band will pass 20-100 km north of Paris. We will organize a one-day trip in the countryside, some 50-100 km north of Paris for eclipse viewing (50% probability of clear weather) and some social/cultural event.

Transportation: Because of the eclipse, plane flights are booking up fast, so we advise you to make reservations as soon as possible.

Mailing List
This announcement was sent to a mailing list updated from previous MOP meetings. Please distribute it around to interested colleagues. For being added on the mailing list, or for eliminating duplicate email addresses, please send a message to: MOP@megasx.obspm.fr

CALENDAR OF EVENTS

1998

October 19-23: Chapman Conference on Space Based Radio Astronomy at Long Wavelengths, Paris, France. Contact: R. G. Stone (stone@urap.gsfc.nasa.gov)
November 3-7: Fifth Latin American Conference on Space Geophysics (COLAGE-V), San Jose, Costa Rica. Contact: W. Fernandez (wfer@cariari.ucr.ac.cr)
December 6-11: AGU 1998 Fall Meeting, San Francisco, CA
Special Session SM-08: Magnetic Reconnection in the Sun-Earth Connected System: Recent Progress. Contact: M. Hesse (hesse@gsfc.nasa.gov)
Special Session SM-09: Substorm Onset Timing. Contact: M. Moldwin (moldwin@pss.fit.edu)
Special Session SH-05: Origin, Initiation and Three- Dimensional Structure of CMEs. Contact: K. Dere (dere@halcyon.nrl.navy.mil)
Special Session U-11: Climatic Effects of a Changing Sun. Contact: L. Floyd (floyd@susim.nrl.navy.mil)

1999

January 4-8: Radar Observations of Meteors: Issues and Results, Boulder, CO. Contact: J. D. Mathews (jdmathews@psu.edu)
January 4-8: Special Session on Ionospheric Heating, Boulder, CO. Contact: M. P. Sulzer (msulzer@naic.edu)
January 11-15: Chapman Conference on Magnetospheric Current Systems, Kona, Hawaii. Contact: R. Fujii (rfujii@stelab.nagoya-u.ac.jp)
February 8-13: Dynamics of the Magnetosphere and its Coupling to the Ionosphere on Multiple Scales using Interball, ISTP, and Ground-Based Observations, Zvenigorod, Russia. Contact: L. Zelenyi (lzelenyi@iki.rssi.ru)
February 16-19: Long-Term Changes and Trends in the Atmosphere (LT-ACT '99), Pune, India. Contact: G. Beig (ltact@tropmet.ernet.in)
March 22-26: Progress in Electromagnetic Research Symposium (PIERS 1999), Taipei, Taiwan. Contact: K.S. Chen (dkchen@csrsr.ncu.edu.tw)
April 19-21: 4th SEC User Conference, Boulder, CO. Contact: B. Poppe (bpoppe@sec.noaa.gov)
April 21-23: 5th Research-to-Operations Workshop, Boulder, CO. Contact: B. Poppe (bpoppe@sec.noaa.gov)
June 24-26: Open Meeting of the Human Dimensions of Global Environmental Change Research Community, Kanagawa, Japan. Contact: Caroline Nunes, (carolinen@icc.es)
June 26-July 1: Science for the 21st Century, Budapest, Hungary. Contact: UNESCO (confsci@unesco.org)
July 16: SCOSTEP Bureau Meeting, UK July 18-30: IUGG99 Assembly, Birmingham, UK
Long- and Short-Term Variability in the Sun's History and Global Change. Contact: W. Schröder, Hechelstrasse 8, D-28777 Bremen-Roennebeck, Germany
Solar Variability and Climate. Contact: J. Pap (pap@astro.ucla.edu) or (jpap@solar.stanford.edu)
Solar Magnetic Field: Reversals, Polar Field, Dynamo. Contact: V. Obridko (solter@izmiran.troitsk.ru) or (solter@izmiran.rssi.ru)
IAGA Symposium on Magnetic Storms. Contact: B. Tsurutani (btsurutani@jplsp.jpl.nasa.gov)
IAGA Symposium GA 4.02: CMEs, Prominence Eruptions and Flares: Onsets and Relationships. Contact: B. Schmieder (schmieder%mesoph@mesiob.obspm.fr)
August 9-12: International Workshop on Radio Methods for Studying Turbulence, Urbana, IL. Contact: A. W. Wernik (aww@cbk.waw.pl)
August 9-14: Magnetospheres of the Outer Planets Conference (MOP99), Paris, France. Contact: (mop@megasx.obspm.fr).