International SCOSTEP Newsletter

KUDOS

SOLAR STATUS REPORTS AND SOLAR ALERTS

PUBLICATIONS
Publications Received at the Secretariat
New Book
Sessions on History of Space and Geophysics

JOB OPPORTUNITIES
Postdoctoral Fellows at the Bartol Research Institute
Studentship at the University of Sussex

MEETING REPORTS
Dayside Transients Workshop
CSSP/CSTR Meeting
School on Atmospheric Radar and Eighth International Workshop and Scientific Aspects of MST Radar

FORTHCOMING MEETINGS
Chapman Conference on Space Based Radio Astronomy at Long Wavelengths
Chapman Conference on Magnetospheric Current Systems
Open Meeing of the Human Dimensions of Global Environmental Change Research Community
Long- and Short-Term Variability in the Sun's History and Global Change

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.

KUDOS

SCOSTEP congratulates the winners of the Hannes Alfvén Medal. Prof. Carl-Gunne Fälthammar, SCOSTEP's Adherent Representative from Sweden, is the recipient of the 1998 Hannes Alfvén Medal for outstanding contributions towards the understanding of plasma processes in the solar system and other cosmical plasma environments. In 1997 the European Geophysical Society (EGS) established the Medal in honor of the late Hannes Alfvén, 1970 Nobel Laureate for Physics. The 1997 Medal was awarded to Prof. Charles Kennel: both Medals were awarded at the 1998 EGS General Assembly in Nice, France.

SOLAR STATUS REPORTS
AND SOLAR ALERTS

Editor's Note: The following timely Solar Status Reports and Solar Alerts are given for your information regarding their availability from Heliosynoptics and Big Bear.

April 23, 1998 1800 UT

CLASS X FLARE S18 EAST LIMB INCREASE IN RADIO FLUX TO BEGIN IN TWO DAYS POST MORTEM ON SW LDE EVENT 20/1021

An X1 long-duration xray flare occurred early today, at approximately 0515 UT. The optical aspect is a long-lived system of bright loops at S18 East Limb. There was no significant region at this location two weeks ago when this area was crossing west limb. The corona has not been particularly bright or complex at this location in the past two days. The inference is that this is a young but rapidly developing region that may show large sunspots in the next day or two.

The trend in solar radio flux is due for a reverse to increasing flux in 2 days. Flux should by that time fall to the projected background for this point in the new solar cycle. That background is estimated by extrapolating the locus of minima in the daily radio flux values that was determined from fitting a straight line to the graph that extends from the middle of 1996. The large xray flare early today guarantees a region of significance will rotate into view a day or two from now, contributing the radio flux that will reverse the trend in 10.7 cm flux.

PROTON EVENT POST-MORTEM The relatively-large proton event generated by the long duration M1 xray flare of 20 April was a surprise to all forecasters. The absence of observable, large sunspots prevented application of forecasting by analogy with the classic proton-flare regions. The large CME was correctly forecast, albeit without an exact date, in the HelioSynoptics report of April 11/1700 UT.

This large nest of bipolar regions created convolutions along the principal polarity boundary that inter-connected six bipolar areas, including a spotless remnant of a high-latitude region near the south polar crown. Three bipolar regions to the east and west of this boundary expanded the complex to an impressive 60 heliographic degrees. Filaments formed over most of the polarity boundaries and these became increasingly active as the complex began its 5-day transit of the west limb. These filaments were the sure sign of impending CME activity; but, filament activity, so far, does not predict proton events. The coronal activity above those filaments, now visible to us with the SOHO and Yohkoh spacecraft, has not been observed for enough events to utilize it for proton prediction. The only long-term coronal datum that should have been heeded was the NSO report of very intense CaXV emission the day before the event. HelioSynoptics was not operational at that time.

Nearly all of the large activity complex had rotated out of view before the proton flare occurred. It is possible there was new magnetic flux emergence that further complicated and energized this region. The intense and complex coronal activity at the limb increased for three days prior to the event, giving credence to this possibility. Confident forecasts of events such as this await the advent of deep-space observing platforms that allow a view of the Sun orthogonal to our Earth-based line of sight. The east-limb event today suggests that two deep-space observing platforms are necessary, one looking at east limb, the other at the west limb.
Patrick S. McIntosh
pmcintosh@solar.stanford.edu

April 27, 1998 1730 UT

REGION 8210 DELTA CONFIGURATION, REVERSED POLARITY UNUSUAL POLARITY BOUNDARY PATTERN FILAMENT ACTIVITY PRIOR TO SECOND X1 EVENT INADEQUATE SOLAR IMAGES PRIOR TO FLARE

SOLAR CYCLE RISE PREDICTS NON-RECORD SOLAR MAXIMUM
The second X1 long-duration xray event early today. from Region 8210 (S18 E45), was not forecast effectively (imprecise time, low confidence) because of the limb proximity of the region, a declining xray background prior to the event, and the lack of high-resolution H-alpha images prior to the event. Only the H-alpha structure allowed detection of the delta-configuration (opposite-polarity spots within a common penumbra) on the NW corner of the large spot in this region. Line-of-sight magnetograms failed to clearly show the nature of the complex magnetic fields here. Data on April 26, when space weather operations were not fully manned, began to reveal this situation. HelioSynoptics normally does not operate on weekends. The H-alpha images on April 26 allowed a detailed map of the large-scale polarity boundaries in this region. This analysis shows a highly convoluted boundary looping around the large sunspot, with an active filament near the high magnetic-field gradient in the delta configuration. Had there been frequent, high-resolution H-alpha images available to forecasters, this event might have been predicted in the short-term. Images with 512x512 pixels for the full disk are unable to record the detail needed for these forecasts.

This region has follower polarity in a large area of plage leading the large leader-polarity spot, making this a reversed-polarity region. All the characteristics of this region place it in a highly-active category despite the small sunspot area and the relatively simple McIntosh sunspot-group type (Cko). The k-type principal sunspot is common to proton-flare, Class-X flare regions.

The lack of any other active regions of substance has held the solar radio and sunspot indices at a low level. The regions expected to rotate into view at east limb in the next four days are not expected to be large or active. The monthly mean indices for April, therefore, will remain close to the March values. The lack of a continued rapid increase in the monthly means at this time begins to clarify the long-range prediction for the peak of this solar cycle. It is now unlikely that the amplitude of this cycle will exceed that of the previous three cycles, consistent with the opinion of the NOAA ad hoc committee on prediction of the solar cycle.
Patrick S. McIntosh
pmcintosh@solar.stanford.edu
April 29, 1998 2100 UT

SOLAR ALERT HELIOSYNOPTICS, Boulder, CO

SECOND MAJOR FLARE FROM REGION 8210 ASSOCIATED ERUPTING FILAMENT FROM WITHIN REGION LOCATION FAVORABLE FOR CME DIRECT To EARTH GEOMAGNETIC DISTURBANCE EXPECTED LATE MAY 01

An expected major flare (xray class M7; optical class 2B) occurred at about 1630 UT today from Region 8210 (S15 E20), the second major event from this region in 3 days. The xray flare was of long-duration, but not as long as from the X1 event on the 27th. A CME is expected, but not confirmed at this hour.

The event position is favorable for the CME to travel directly to Earth, possibly at faster than usual speed due to the association with a major flare. THIS DISTURBANCE COULD ARRIVE AS EARLY AS LATE ON MAY 01, near the expected time of arrival of the disturbance from the previous flare; that is, this second CME may catch up with the previous CME, producing a complex interplanetary cloud upon arrival at Earth. This combined event could be either stronger than from a single event, or a weaker, dampened event due to canceling effects of the two events. Interplanetary monitoring is insufficient to discern between these two possibilities. The first event is likely to be a "glancing blow" of the edge of the interplanetary "bubble" encountering Earth. The second event will be a direct hit.

An alert prior to this event was not issued due to a communication breakdown late yesterday. Observations on 28 April of active, dark, embedded filaments in Region 8210 and the rapid formation and proper motions of numerous new spots late in the day gave a high probability of a major flare within 24 hours of those observations. Most interesting was the rapid formation of a single dark spot west of the primary sunspot, and its subsequent rapid movement westward toward a spot of opposite polarity. The M7/2B flare was centered on the location of the high magnetic-field gradient between these two spots.

The usual synoptic data of sunspot area and classification were insufficient predictors of this event. This situation again emphasizes the importance of high-resolution images in white-light and H-alpha for detection of active filaments and their positions relative to evolving sunspots. The spots in this case were not easily observed in 512x512 pixel images. Direct visual observation in white light was an important factor in making a correct solar forecast.
Patrick S. McIntosh
pmcintosh@solar.stanford.edu
April 29, 1998 2130 UT

CORRECTION TO PREVIOUS ALERT

GEOMAG STORM FROM TODAY'S FLARE/CME NOT EXPECTED UNTIL LATE ON MAY 02.
Patrick S. McIntosh
pmcintosh@solar.stanford.edu
May 01, 1998 0030 UT

SOLAR ALERT
HELIOSYNOPTICS, Boulder, CO

SPOT GROWTH MAY FORM NEW DELTA CONFIGURATION IN 12 HOURS INCREASING COMPLEXITY, ACTIVE ABSORPTION FEATURES ANOTHER MAJOR FLARE EXPECTED WITHIN NEXT 72 HOURS MODERATE SPOT GROUP DEVELOPING NE QUADRANT
New sunspots near the SE and NW edge of the principal sunspot in Region 8210 (S16 W02) are opposite in polarity to the principal spot, and growth during the day established a trend toward merging of these three areas. A number of active absorption features emanate from this developing area, suggesting there will be surges from this area. The prospect for at least one area of delta-configuration (opposite-polarity spots within a common area of penumbra) renews the potential for another major flare. This new configuration could generate an event more energetic than the previous event. A major flare might occur as early as midday on May 01, or wait as long as late on May 03. Growth of sunspot at N25 E45 has built an Eai group that may become a large group in the next 24 hours. Its flare potential is low, but its presence will contribute to an increase in radio flux.
Patrick S. McIntosh
pmcintosh@solar.stanford.edu
May 2, 1998 1530 UT

SOLAR ALERT
HELIOSYNOPTICS, Boulder, CO

MAJOR PROTON EVENT IN PROGRESS CLASS-X FLARE REGION 8210 1340 UT HIGH-ENERGY PROTONS ARRIVED IN LESS THAN 30 MIN MAJOR MAGNETIC STORM IN PROGRESS
Region 8210 (S17 W17) produced a Class-X1 flare at approximately. 1340 UT today and high energy protons arrived in less than 40 minutes. The event occurred near the rapidly developing delta configuration reported in yesterday's alert. The sunspots are now very complex and showing clockwise rotation, including the delta-configuration. These are classic properties of proton-flare sunspots.

The magnetic storm expected from the X1 event of 29 April arrived late on 01 May and is now of major proportions.

Advance notice of the impending proton-flare was impaired, again, by the absence of high-resolution white-light observations from the Pacific region. Observatories in California, Hawaii, Australia and Japan are urged to establish patrols of important sunspot groups with image resolutions of at least 2-arc-seconds and to operate them in the interval 2000-0400 UT.
Patrick S. McIntosh
pmcintosh@solar.stanford.edu
May 5, 1998 1500 UT

SOLAR ALERT AND STATUS REPORT
HELIOSYNOPTICS, Boulder, CO

PROTON FLARE (LARGE CLASS-M) EXPECTED CME FROM LARGE FILAMENT ERUPTION EXPECTED SOLAR INDICES DECLINING DURING NEXT WEEK
Region 8210 (S16 W57) is again experiencing flare buildup. A dark negative-polarity spot has moved from beside the large principal spot to the delta-configuration at the north end of the penumbral area. The penumbra involved with the delta has darkened. A proton flare is expected in the next two days, possibly in just a few hours. The xray background has continued a slow rise during the past three days.

Region 8214 (N27 W19) has stretched to 16-degree length, boosting its classification to Fki. Most of the spots have weakened and there are fewer of them, but still the spot count is very high (over 50). Flares here will not exceed Class C unless there is new growth and more complicated topology.

No new spots have appeared at SE limb. The returning activity complex which produced the M1 proton event of 20 April has no spots except for the old leader, now labeled as Region 8217. A large filament meanders through the large remnant plage. This filament will erupt in the next few days, with a large CME.

Solar indices are expected to decline rapidly during the next week unless there occurs a global increase in flux eruption.
Patrick S. McIntosh
pmcintosh@solar.stanford.edu
May 7, 1998 0400 UT

SOLAR ALERT
HELIOSYNOPTICS, Boulder, CO

MAJOR FLARES IMMINENT

REGION 8214 IN NW DEVELOPING COMPLEX FIELDS\REGION 8210 ON SW LIMB REMAINS BRILLIANT, COMPLEX NE LIMB SHOWING LARGE ACTIVITY COMPLEX LARGE FILAMENT SE BECOMING UNSTABLE
The growth of new, brilliant coronal loops on the north edge of Region 8214 (N27 W38) and chromospheric plage enveloping most of the leader spot indicate a more active phase for this region. Class M and Class X flares are expected for the remainder of its disk and limb transit. The first of a series of large flares may occur within the next 12 hours.

The xray background has been steady at a C2 level for over 3 hours, indicating intense preflare heating.

Region 8210 (S16 W80) has not returned to its normal brightness since the X2 proton flare of 06/0809. Loops continue above the region. An additional large event appears imminent.

A broad span of loop activity is now rising above the NE limb, spanning 15 degrees of latitude. Prominence activity nearby suggests important sunspots are present in a region that may not appear on the disk for at least another day. This location was not important when last viewed 2 weeks ago.

The large filament embedded in the large remnant complex in the SE has darkened, broadened and lifted. It is ripe for eruption. Its size is such that the eruptive prominence will be spectacular and the CME large. The surrounding chromosphere is bright and contains significant magnetic flux such that a large 2-ribbon flare is expected when the eruption occurs.

Welcome to the active part of the solar cycle!
Patrick S. McIntosh
pmcintosh@solar.stanford.edu
May 12, 1998 1930 UT

SOLAR ALERT
HELIOSYNOPTICS, Boulder, CO

CORONAL MASS EJECTION NEXT 12 HOURS FLARE BUILDUP IN REGION 8218 S20 W03
Region 8218 has become more complex in the past 24 hours due to the emergence of two new bipolar areas within the existing spot group. The leading portion of the region contains a mix of polarities. Spots are growing rapidly and moving within this area. Further growth and motion is likely to generate one or more delta configurations (penumbral areas containing spots of both polarities) and certainly there will be an eventual coalescence of leader polarity spots to form a large and more complex leader spot.

These developments are likely to lead to small Class M flares within the next 24 hours.

A more important consequence of these developments is the destabilization of the large filament channel to the south and west of Region 8218. The large filament in the channel had already been noted as having potential to erupt with an accompanying very large coronal mass ejection (CME). The filaments in the channel are changing and darkening, perhaps lifting higher into the corona.

A very large CME is imminent, most likely in the next 12 hours.

The location of this event and the large-scale polarity environment are favorable for the event heading directly at Earth and with southward-directed magnetic fields that should generate a strong geomagnetic disturbance as early as late on 16 May.
Patrick S. McIntosh
pmcintosh@solar.stanford.edu

April 27, 1998
BEARALERT

NOAA 8210 (Big Bear 3973) produced another X-class event today. We expect continued isolated M- and even a chance for another isolated X-class event.

NOAA 8210 is a reversed polarity region with a delta configuration (see images on http://www.bbso.njit.edu and click on "Latest Images"). New positive polarity flux is emerging at the northern edge of the large negative polarity trailing sunspot. It is also possible that the large, dark filament aligned along the region's neutral will erupt if another flare occurs.
WM, JV, HZ

May 1, 1998
UPDATE: NOAA Region 8210 (BBSO 3973) S16W04 at 15:00 UT/May 01, 1998.

New positive polarity flux that emerged yesterday just east of the large negative sunspot has continued to grow and has merged with the main negative sunspot creating a Delta Configuration (opposite polarity umbrae within a common penumbra). We continue to expect isolated M-class flares. In addition, an X-class flare is also possible.
WM, JV

BIG BEAR SOLAR OBSERVATORY
ALERTS AND IMAGES AVAILABLE

For some years Big Bear Solar Observatory has sent out BEARALERTS to tell the community about unexpected solar activity. The philosophy and success rate was described in "BEARALERTS: A Successful Flare Prediction System," Solar Physics 131, 149, 1991, H. Zirin and W. Marquette. We expect that the new management will continue this practice.

In addition, the BBSO home page (http://www.bbso. njit.edu/) now contains the finest full-disk solar images ever made, including a completely new Halpha image showing limb prominences. The image is 2000x2000 pixels, but a reduced image is also available.
Hal Zirin/JHA

BearAlert Mailing List Requests for subscription to the BearAlert mailing list should be sent to bearalert_admin@bbso.njit.edu. Please give your email address, affiliation, and full name. You may also reference their page on WWW (http://www.bbso.njit.edu/cgi-bin/BearAlert)

Dennis D. Dingley
BearAlert Mailing List Maintainer
Big Bear Solar Observatory
New Jersey Institute of Technology
40386 North Shore Lane
Big Bear City, CA 92314-9672 USA
voice: +1 (909) 866 5791 (ext. 11)
FAX: +1 (909) 866 4240
email: bearalert_admin@bbso.njit.edu

PUBLICATIONS

The following publications received recently at the SCOSTEP Secretariat may be of interest to different parts of our community. Information is given about each and the name and address of a contact if you should want to request addition to their mailing list.

1. AFRICAN SKIES, a publication of the Working Group on Space Sciences in Africa. Editor F. R. Querci, Observatoire Midi-Pyrenees, 14, Av. E. Belin, Toulouse, France.

The Working Group on Space Sciences in Africa is an international, non-governmental organization founded by African delegates at the 6th United Nations/European Space Agency Workshop on Basic Space Science, held in Bonn, Germany, on 9-13 September 1996. The scientific scope of the Working Group's activities is defined to encompass (a) astronomy and astrophysics, (b) solar-terrestrial interaction and its influence on terrestrial climate, (c) planetary and atmospheric studies, and (d) the origin of life and exobiology.

The Working Group seeks to promote the development of the space sciences in Africa by initiating and coordinating various capacity-building programmes throughout the region. These programmes fall into a broad spectrum ranging from the promotion of basic scientific literacy in the space sciences to the support of international research projects. The Working Group also promotes international cooperation among African space scientists and acts as a forum for the exchange of ideas and information through its publications, outreach programmes, workshops and scientific meetings.

The publication is in both French and English.

Key contacts about the publication AFRICAN SKIES are:
Editor: Dr. F.R. Querci, (see address above),
e-mail: querci@astro.obs-mip.fr

Other questions may be addressed to:
WGSSA, South African Astronomical Observatory, P.O. Box 9, Observatory
7935, SOUTH AFRICA.
e-mail: wgssa@saao.ac.za http://www.saao.ac.za/~wgssa/

In addition to the new publication AFRICAN SKIES, the WGSSA has distributed a questionnaire which will be used to create an inventory and/or membership list for persons in Africa who are interested in Space Sciences. They seek to identify individuals, but also to identify resources already in-hand and needs of persons and organizations. We suggest you correspond with the key contacts named above if you are interested in this survey and the WGSSA.
JHA

2. SOLAR SYSTEM NEWS, the Newsletter of the Solar System Division of ESA, issue No. 21, March 1998, was received at the Secretariat. It has several interesting articles, including among many: ULYSSES update; news about SOHO (the SOHO WWW website for the recent solar eclipse registered 150 "hits" per second just prior to totality of the eclipse (the highest ever for a SOHO page); information about the re-flight of the CLUSTER mission (to launch in June and July 2000); early particle measurements by EQUATOR-S; and the First Announcement of the ESLAB-98 Symposium. SOLAR SYSTEM NEWS is available twice yearly from: ESTEC, Postbus 299, 2200 AG Noordwijk, The Netherlands, e-mail: kwenzel@estec.esa.nl and see: http://helio.estec.esa.nl/.

3. A STUDY OF GLOBAL CHANGE is a lovely brochure just received from the IGBP Secretariat, The Royal Swedish Academy of Sciences, Box 50005, S-10405 Stockholm, Sweden (E-mail to: sec@igbp.kva.se). It discusses the Agenda 21, which was established as a result of the Rio Earth Summit of 1992, as an international community response and IGBP as a comprehensive programme of action to develop plans to reduce effects of environmental degradation and promote sustainable and sound environmentally considerate economic development in all countries. Each page of the brochure addresses some aspect of IGBP. Only in the complex "wiring diagram" to illustrate "Putting it Together" does there appear an element "SUN" providing external forcing to atmospheric physics and dynamics and to stratospheric chemistry and dynamics. I regret that still this is the only place in which any STP input appears.

4. THE GLOBAL CHANGE NEWSLETTER, No. 33, March 1998, was received from: IGBP Secretariat, The Royal Swedish Academy of Sciences, Box 50005, S-104 Stockholm, Sweden. The Editor is Sheila M. Lunter (sheila@igbp.kva.se).

5. SPARC NEWSLETTER NO. 10, January 1998. This beautifully produced newsletter is edited and composed by the SPARC Office, Directed by M.-L. Chanin (someone well-known to SCOSTEP participants). Marie-Lise Chanin and Marvin Geller are Co-chairs of SPARC's Scientific Steering Group. This issue includes some of the best graphics I have seen in a mass-produced publication that is not financed by subscription charges and paid advertising. It includes a report by Jan Lastovicka (jla@ufa.cas.cz) on the "Second IAGA/IAMAS Workshop: Solar Activity Forcing of the Middle Atmosphere" (Prague, 18-21 August 1997). Address of the SPARC Office is: Service d'Aeronomie, CNRS, BP 3 91371 Verrieres-le-Buisson cedex, FRANCE. E-mail to: sparc.office@aerov.jussieu.fr; see also: http://www.aero.jussieu.fr/~sparc/.

Geomagnetism and Aeronomy (with special historical case studies), Proceedings of the Session during the IAGA General Assembly in Uppsala, Sweden, August 1997. Edited by Wilfried Schröder, 450 pages, illustrations. ISSN: 0179-5658, 1998. Price 40 DM, 25 USD

In 1997, three international conferences were organized on the topic of History of Space and Geophysics and its different disciplines. These sessions have shown that there is considerable interest in the history of geophysics. Convener of all three conferences was Wilfried Schröder, Hechelstrasse 8, D-28777 Bremen-Roennebeck, Germany, from whom more details can be obtained on the conference papers and other subjects.

1. The first session was during the Assembly of the German Geophysical Society in March in Potsdam, Germany. Topics are: Theory of Relativity and Gravitation in Geophysics (H.-J. Treder); Michelson, Foucault and Mach (K. Strobach), The Work by Helmholtz (H. Hörz), and the physical application and geophysical evidence of Werner Heisenberg's research; topics from various parts of the history of geophysics, aeronomy, meteor astronomy, and geodetical research, including instrumentation during the last decades.

2. In April 1997, the session "Solar and Terrestrial Physics during the 19th/20th Centuries" was organized during the meeting of the European Geophysical Society in Vienna. Invited papers from eminent participants (Sir Ian Axford, Gerhard Haerendel, Alf Egeland, Joszef Verö, Suzanne Debarbat et al.) Topics of the lectures are the development of theories and observation in Czechoslovakia, Slovakia, Croatia, Russia, France, Scandinavia, Hungary and other places of the world.

3. During the General Assembly of IAGA in Uppsala, the Interdivisional Commission on History organized the Session "History of Geophysics and Aeronomy and Global Change." Invited papers were presented by Alf Egeland, Gerhard Haerendel, Bengt Hultqvist, E. Oni, et al. Contributed papers focused on some personalities, i.e., Helmholtz, Leo Gama, J. Bjerknes, and the development of theoretical meteorology (including Hans Ertel's work), Tanakadate, Marconi, J. Gallo and the development of geophysical sciences in Turkey, Japan, Slovakia, Nigeria, France, etc. Wilfried Schröder

JOB OPPORTUNITIES

The Bartol Research Institute of The University of Delaware has existing openings for two Post-Doctoral Fellows in Space Plasma Physics research. The positions are supported by funds from the ACE, Voyager and Ulysses projects as well as NASA's Space Grant College program in Delaware for which BRI is the lead institution.

BRI magnetic field studies on these projects include ongoing observational and related theoretical studies of the helio-spheric magnetic field with correlated studies of energetic particle transport and solar originating disturbances. BRI is the lead institution for magnetic field studies on Voyager and ACE. A recent HMGI Ulysses grant will be used to support related, high-latitude studies using the Ulysses dataset.

A range of single- and multi-spacecraft studies involving the above spacecraft along with ISTP missions are envisioned that will shed new light on interplanetary turbulence, provide new information on the structure and dimension of transients, and develop refined observations that lead to new or enhanced studies of energetic particle propagation in the heliosphere. The positions are under the direction of Drs. Norman F. Ness and Charles W. Smith with collaborative involvement of other BRI researchers anticipated. Candidates with a strong background in space plasma physics and/or fluid dynamics with an interest in the analysis of spacecraft data are especially encouraged to apply.

Initial appointments are for one year with extensions possible up to an anticipated three years, depending on satisfactory progress. For additional information, please contact N.F. Ness nfness@bartol.udel.edu or
C.W. Smith chuck@bartol.udel.edu.
To apply, send a curriculum vita and arrange to have three letters of reference sent to Dr. C.W. Smith, Bartol Research Institute. BRI's home page is http://www.bartol.udel.edu.

The University of Delaware, Newark, DE 19716, USA. Applications will be accepted until the positions are filled. The Bartol Research Institute is an equal opportunity/ affirmative action employer.
Charles W. Smith
chuck@brivs2.bartol.udel.edu

The Space Physics group at the University of Sussex, which forms part of the Space Science Centre, invites applications for a PPARC studentship in postgraduate research leading to the award of a DPhil.

The studentship is for 3 years, and is available for candidates with a relevant UK connection. Academic qualifications should consist of a 1st or upper 2nd class honours degree in a science-related subject (this restriction may be lowered if another postgraduate qualification has been acquired). Usually additional income is provided through assistance at tutorials, laboratory workshops, etc.

The Space Physics group currently has interests in the following areas, any or a combination of which could form the basis of the proposed research for the studentship:

1) Ground-based observations of the aurora, and analysis of the resulting optical video recordings in conjunction with ionospheric plasma measurements obtained from the EISCAT radars in Scandinavia.

2) Theoretical (magnetohydrodynamic) modeling of reconnection, as applied to solar wind-magnetosphere coupling at the magnetopause, substorm phenomena associated with reconnection in the magnetotail current sheet, and solar flares.

3) Analysis of spacecraft data, mostly in the form of magnetic field measurements and plasma bulk parameters, to study coupling processes at the magnetopause, and substorm phenomena in the magnetotail.

For further details and expressions of interest contact:
Richard P. Rijnbeek, Space Science Centre
School of Chemistry, Physics and Environmental Science (CPES), University of Sussex, Brighton BN1 9QH
E-mail: R.P.Rijnbeek@sussex.ac.uk
http://ww.susx.ac.uk/Units/physics/research/space/spghmp.htm
Tel: +44-(0)1273-678699 Fax: +44-(0)1273-678097
Richard Rijnbeek
richardr@susx.ac.uk

MEETING REPORTS

The one-day workshop titled "Dayside transient events in the high-latitude ionosphere and magnetosphere", took place on December 13, 1997, in San Francisco after the Fall AGU meeting.

Transient signatures (less than 30 minutes duration) at the dayside magnetopause and its boundary layers and, in particular, their ionospheric response can provide crucial information about the mechanisms of the coupling between the solar wind and the magnetosphere. The main purpose of this Workshop was to bring experimentalists, theorists and modelers together in a very informal setting and give them the opportunity to define the crucial issues and start collaborations. The Workshop viewed dayside transients from a global perspective and tried to identify the causal links between transients in the solar wind, the bow shock and the magnetosheath, and the signatures of transients in the magnetosphere and the ionosphere. The Workshop was very successful in being attended by about 30 scientists and by stimulating much discussion and many informal contributions.

A full report on the results of the Workshop is available at our web site http://www.dmi.dk/fsweb/miniworkshop/ or by emailing to the organizers.

Eftyhia Zesta, ezesta@sec.noaa.gov
Therese Moretto, moretto@dmi.min.dk

The Committee on Solar and Space Physics (CSSP) was held in Washington, DC, on January 26 - 28, 1998. Although the Committee on Solar-Terrestrial Research (CSTR) did not meet at this time, Michael Kelley, Chair of CSTR, and Norman Ness, CSTR member, represented CSTR at the meeting. The agenda topics fell under three main headings: agency reviews (NASA and NSF), radiation hazard, and parametric analysis of Sun-Earth Connection Science.

Agency Report-NASA: In his report from NASA, George Withbroe, Science Director for the Sun-Earth Connection Program, emphasized the success that space physics has had this last year as measured by the metric of public visibility. Space physics is "getting the message out." News stories, such as probing the solar interior with SOHO, appeared often in the science press (e.g., Science News), in the national press (e.g., the Washington Post), and on national TV (eight times.) These stories help the program because they respond in an objective way to a congressional order mandating all government agencies to provide metrics by which to measure their activities. In NASA's case, documenting public consumption of scientific results might serve as a metric.

Withbroe discussed a new program his office has started on the subject of solar influences on global change. An AO for this program was issued, in response to which there were 65 letters of intent. He intends to use his discretionary budget ($700 K) to fund it and to fund a workshop on the subject. The workshop will be held sometime in the Fall of this year. Part of his discussion reviewed relatively recent evidence that suggests a connection between the level of solar activity and global climate.

The Solar Probe Mission has been packaged as one of a trio of planetary missions along with the Europa Orbiter and Pluto/Kuiper Express missions. Because the possibility of discovering life on Europa in a water ocean under a thin crust of ice excites broad interest, Europa Orbiter is likely to be the first of the three missions to go. The line comprising the three missions has been approved.

Regarding Explorer selections, Withbroe noted that Space Physics came out of the last MIDEX (Mid-Class Explorer) selection with the Magnetopause-to-Aurora Global Exploration (IMAGE) mission. Now it has come out of the October SMEX (Small Explorer) selection with the High Energy Solar Spectroscopic Imager (HESSI) mission and the Two Wide-Angle Neutral-Atom Spectrometers (TWINS) mission of opportunity.

Withbroe said that there is $28 M in the FY 98 budget for FY 99, and there is $12 M/yr for 00 and for each year beyond, which he regards as a down payment for the future years.

Agency Report-NSF: Richard Behnke, Head of the Upper Atmospheric Research Section, began his report by noting that the NSF budget for FY 99 looks very encouraging. He emphasized the substantial progress that the National Space Weather Program (NSWP) has made. For example, there have been a number of space weather workshops. Besides the annual January space weather workshop held at SEC, there was a workshop on ionospheric disturbances held in November of last year. There was the first space weather session at an annual meeting of the American Meteorological Society, held in January. Seventeen NSWP awards were made during the last proposal opportunity. The NSWP implementation plan has been completed. Since the implementation plan is meant to be a "living" document, Behnke would like the CSTR to help with the task of periodically updating it. The weak link in the science-to-operations chain that binds the NSWP program together is the one just prior to operations. In Behnke's view, responsibility for funding the transition to operation belongs neither to NSF nor to NASA, but to NOAA on the civilian side. A process for carrying out the transition is specified in the NSWP Strategic Plan. It is called a "rapid prototyping center," a conceptual plan for which has been developed at NOAA's Space Environment Center (SEC). (Behnke would rather have it called a "rapid transitioning center," since its crucial function is to enable the transition of an operational procedure.) All that is missing is the needed agency funding. Scientific products engineered for applications are nonetheless moving across the terminal science-to-operations link, leading to an increased operational capability at SEC. On the military side, the Air Force is conducting a review of the DOD's space weather requirements. A report of the review will be given to the DOD Space Architect, General Robert Dickman, at the end of March. If the report recommends putting increased effort into space weather, and if the recommendation is accepted, the changes will be incorporated into a Master Space Architecture Plan covering the period out to 2025. The Plan will be developed over the next 4 to 6 months.

Behnke described a currently active NSWP project to define metrics by which to measure improvement of space weather science. A metrics task group headed by Ed Szuszczewicz has been formed to consider what parameters should be measured to monitor improvement. The group is emphasizing metrics by which to measure scientific improvements. It held a special session at the Fall AGU Meeting followed in January by a workshop at SEC in Boulder. It is now drafting a report, which will propose a set of metrics. Behnke would like CSTR to critique the report.

Behnke noted that we are entering an era of unprecedented access to tools for advancing our profession: global MHD models, the ISTP fleet, ground-based instruments, collaboratories, and eventually, the Polar Cap Observatory, though authorization to begin constructing it is still delayed in Congress. Nonetheless, he is optimistic that the facility will be ready in time to participate in Solar Max 23 campaigns.

Radiation Hazard: At its last meeting, CSSP/CSTR decided to consider for investigation an aspect of the concern over the hazard that ionizing radiation poses to astronauts and space hardware. The aspect of interest to the Committee is how information and advice on this subject is solicited by and given to the various units within NASA and other (non-DOD) government agencies to which it might be a concern. The decision to look into this question was motivated by the following perception. Different units within NASA and other agencies are independently pursuing their interests in this subject either as a supplier or a receiver of information and advice. Therefore, by reviewing these separate efforts, there might be an opportunity for the Committee to recommend ways to improve the coordination of the flow of information and advice between them. The main purpose of the radiation-hazard session conducted at this meeting of the Committee was to assess the correctness of the perception before deciding whether to recommend to the agency sponsor that the Committee undertake a formal study.

For this meeting, the Committee invited presentations primarily from people concerned with the radiation problem as it relates to NASA's Life and Microgravity Science and Applications Office (Code U.) A good way to convey the non-overlap between the space physics community interested in space radiation, viewed as a science, and the biological community interested in space radiation, viewed as a problem, is to introduce the presenters and discussants. Walter Schimmerling is the Senior Scientist of NASA's Space Radiation Health Program. Mary Jane Osborn in the Department of Microbiology at the University of Connecticut chairs the NRC Committee on Space Biology and Medicine. Lawrence W. Townsend in the Department of Nuclear Engineering at the University of Tennessee conducts studies for NASA on the physics of space radiation transport through bulk matter and its effects on astronaut exposure and risk predictions. Richard B. Setlow is Associate Director for Life Sciences in the Biology Department at Brookhaven National Laboratory. He chaired the task group that wrote the 1996 NRC report "Radiation Hazards to Crews of Interplanetary Missions." Gautam Badhwar is with the Johnson Space Center. He is correlating space radiation measurements made by NASA on Shuttle flights with those made by the Institute of Biomedical Problems (Russia) on MIR. He is also comparing NASA's and the Institute's space flight dosimeter calibration techniques. Ronald Turner of ANSER conducts studies for Code U to assess the radiation hazard to astronauts during space station construction. Turner interacts with both communities.

The Committee learned that the biologists think that by far the greatest uncertainties in assessing the radiation hazard to astronauts lie on the biology side of the question. Specifically, the biggest uncertainties lie in specifying the short-term and long-term biological consequences of subjecting different biological tissues to various dose levels of different types of radiation. They think that the space physics community's ability to specify the radiation environment is in much better shape. As a field of research in the biologists' "Components of Uncertainty" pie chart, "Further Definition of the Radiation Environment" constitutes a very small wedge. Members of CSSP felt that the biologists might be overestimating the current ability of the space physics community to forecast and specify the radiation environment. This instance suggests that there is room for improved sharing of information between different disciplinary groups concerned with the radiation-hazard question.

There is general agreement on the biological side that the ability to forecast and specify the radiation environment is a crucial component of any procedure aimed at minimizing the radiation hazard to astronauts. Schimmerling gave a long list of requirements for space radiation physics, which included predictions of galactic cosmic radiation, predictions, forecasting, and warning of solar particle events, and models of trapped radiation in free space and inside Shuttle and International Space Station (ISS.) He noted that there is a radiation coordinating team at Headquarters led by Life Sciences and including Space Physics, but it has no program.

Townsend gave a balanced though limited assessment of the relative uncertainties that reside in the two disciplines. He said that on the one hand "true uncertainties in estimates of absorbed doses and risks from exposures to large SPEs [solar particle events] are unknown," while on the other hand "there is no consensus within the space radiation community as to what constitutes a realistic 'worse case' SPE scenario."

Badhwar focused on the radiation question as it affects ISS construction. As far as he could tell, there is no central coordination within NASA to address the crucial questions: "Is there a problem?" and "Does it need to be fixed?" He suggested a way to assess the importance of the problem or to bring it to light: Determine whether any likely radiation scenario would cause the EVA manager to act differently than planned during ISS assembly.

In its subsequent discussion, the Committee decided to adopt Badhwar's suggestion and to propose to its agency sponsor the following pilot project. Shift the radiation events of the last solar cycle ahead one cycle, and superimpose them on the Shuttle flight and EVA schedule for ISS assembly. Then according to the existing rules for safeguarding astronauts against the risks of radiation, assess to what extent the EVA manager would alter EVA activity. Repeat the exercise several times with different start times for the assembly flights to get statistics with which to express the assessment. George Withbroe has approved this project, and Ron Taylor has agreed to perform the simulations. Depending on the outcome, the Committee will determine whether to carry its involvement with the radiation-hazard question further and if so, in what way.

Parametric Description of the Sun-Earth Connections Science: Space physics in 1998 finds itself in a strong position. It can claim a 40-year history of scientific progress; it addresses a diverse and rich set of scientific challenges; and it possesses a hard-won armamentarium of powerful research tools. These include its data archives, its theory programs with state-of-the-art computational codes, its ongoing missions including the multi-satellite ISTP mission, its access to space through the Explorer line, through its Solar-Terrestrial Probe line, through missions of opportunity, and through occasional larger missions. The opportunities now to advance space physics on all fronts are unprecedented. To aid this advance, CSSP/CSTR propose to construct a parametric description of Sun-Earth Connections science. A parametric description allows the field to see how good or poor the data coverage (or mission attention) is that it has to address the crucial science questions and issues in its different areas of interest. Such a view shows where emphasis is desirable in future missions.

A parametric description means a representation in which crucial SEC science questions and issues -- that is, "target science" -- apply to distinct domains within parameter spaces whose axes define natural delimiting variables. For example, spatial scales and time scales delimit many of the structures and phenomena that are the subjects of SEC target science. Magnetospherists speak of microscale, mesoscale, macroscale, and global structures and processes. They classify magnetic pulsations by divisions along a time-scale axis. Thus, many magnetospheric structures and processes of target-science interest fall into distinct domains in a two-dimensional, size-duration space. It is possible to further separate overlapping target-science domains by distributing them along third, fourth, etc. axes, for example, energy and species (for particles), frequency (for waves), and resolution (for images.) A parametric description of SEC science can separate in a standard way the different domains of target-science interest within the field. The method is applicable to all target science, including that that pertains to planetary magnetospheres and the Sun-Earth connection itself.

The goal of CSSP/CSTR in this project is twofold. First, construct a comprehensive set of parameter-space domains of crucial SEC science questions and issues. Second, overlay on these domain-marked spaces the data coverage available to address the questions and issues through data archives, ongoing missions, and planned missions. The resulting information should have an important application in demonstrating the need for future missions. In this connection, CSSP invited presentations from scientists representing planned SEC missions called out in the 1997 NASA document: "The Space Science Enterprise Strategic Plan." The presenters were asked to identify the crucial SEC science questions and issues that their missions will help answer and resolve by supplying data in appropriate parameter domains.

The following presentations were made: Vassilis Angelopouslos (SSL-UC Berkeley), Geospace Multiprobes; Spiro Antiochos (NRL), Solar B; Dave Rust (JHAPL), STEREO; Richard McEntire (JHAPL), Magnetospheric Multiscale Mission; Peter Panetta (GSFC), Magnetospheric Constellation; Rob Pfaff (GSFC), Global Electric Dynamic Mission; and George Gloeckler (Univ. of Maryland), Solar Probe. The exercise revealed that the ability to specify precisely the mission's target science varies between missions. In some cases, the science questions and issues are specific and well defined. In other cases, they are less specific and well defined, though they could become more so. In any case, these presentations will be helpful to CSSP/CSTR as they carryout out the project of constructing a parametric description of crucial SEC science questions and issues and of assessing what future missions might optimally move the field toward answering and resolving them.

George Withbroe has indicated his approval of the project. It will be a major agenda item at the next CSSP/CSTR meeting, which is scheduled for June 29, 30 and July 1 at Woods Hole.

Since the beginning of the MST radar era in the middle 1970s several workshops have been held, and these have become standardized in the International Workshops on Technical and Scientific Aspects of MST Radar. After such Workshops had been held in USA, Europe and the Far East, it was decided to hold the 8th Workshop in India. This Eighth International Workshop on Technical and Scientific Aspects of MST Radar was preceded by the School on Atmospheric Radar, which was held in Tirupati at the Sri Venkateswara University (SVU) and the Indian National MST Radar Facility (NMRF) in Gadanki. The School on Atmospheric Radar (SAR) took place 10-13 December 1997, and the Eighth International Workshop on Technical and Scientific Aspects of MST Radar (MST8) took place on 15-20 December 1997, in the Hotel Ashok in Bangalore. Both activities were sponsored by the Scientific Committee on Solar-Terrestrial Physics (SCOSTEP), the International Union of Radio Science (URSI), the Department of Space (DOS) and the Department of Science and Technology (DST) of the Government of India, the Council of Scientific and Industrial Research (CSIR) of India, the Sri Venkateswara University (SVU) in Tirupati, and the Indian Space Research Organization (ISRO).

The SAR was prepared by a steering committee, constituted by Dr. A. P. Mitra, Prof. P. B. Rao and Dr. J. Röttger, with the latter as international coordinator. The local organization was under Prof. D. N. Rao and Dr. A. R. Jain. The international coordinator arranged the lecture contributions by experts from the international MST radar community. These lectures dealt with radar scattering from refractive index irregularities in a turbulent flow (lecturer: Dr. R. J. Doviak), radar scattering from meteors, hydrometeors, lightning and dusty/icy plasma (Dr. J. Y. N. Cho), principal radar system requirements and hardware (Dr. I. M. Reid), data analysis and validation (Dr. M. Yamamoto), MST radar interferometry (Dr. J. Röttger), gravity waves and turbulence (Dr. W. K. Hocking), wind profiling and combination with other instruments, rockets and balloons (Dr. M. Petitdidier), and the operational use of atmospheric radars in tropical meteorology (Dr. M. Yamanaka.) Further lectures were given by the NMRF and SVU staff on the science, operation and experiment performance at the NMRF. Intensive group discussions and hands-on training was performed after the lectures. Some 70 participants joined these lectures and training sessions, whereof 15 were from outside India. Each participant received a set of lecture notes, which had been compiled in two volumes. The SAR opened with a formal ceremony at the Sri Venkateswara University, where Prof. R. R. Daniel presented the inaugural address. A dinner was hosted by the NMRF and the School finished with a panel discussion with the lecturers, which was chaired by the international coordinator Dr. J. Röttger. Generally, the scope and performance of the school was regarded very successful and it was considered that such Schools should be repeated in future.

Following this School the lecturers and participants traveled to Bangalore to participate in the Eighth International Workshop on Technical and Scientific Aspects of MST Radar (MST8), where they were joined by Workshop participants from all over the world. A total of 130 scientists and engineers took part in MST8, where 52 were from outside India, and from 17 countries. The program and organization of MST8 had been prepared by an international steering group consisting of Prof. S. Fukao, Prof. M. F. Larsen, Prof. C. H. Liu, Dr. A. P. Mitra and Dr. J. Röttger, with the latter as chairman. The local organization was under the direction of Prof. P. B. Rao of NMRF and Drs. S. C. Chakravarty and S. Chandrasekharan of ISRO. These were supported by a national Organizing Committee (chair Dr. A. P. Mitra), a Local Organizing Committee (chair Prof. P. B. Rao) and technical, administrative and financial sub-committees. The MST8 was opened in a formal inauguration with speeches by Prof. P. B. Rao, Dr. J. Röttger, Dr. A. P. Mitra and Prof. R. Narasimba of the National Institute of Advanced Studies in Bangalore, who gave the inaugural address. A message from the president of SCOSTEP, Prof. C. H. Liu, was read at the Workshop inauguration.

The Workshop contributions had been grouped into four main topics, which were overseen and prepared by main session organizers under the coordination of the chairman of the international steering group. These main sessions dealt with the topics: (1) Scattering processes (main session organizer: Dr. K. S. Gage), (2) Atmospheric dynamics (Dr. W. K. Hocking), (3) Meteorology (Dr. J. van Baelen, Dr. G. Nastrom) and (4) New developments and facilities (Prof. S. Fukao, Prof. S. Avery). These topics were subdivided into the sessions (1) MST scattering and reflection, ionospheric scattering and techniques for measuring scattering and reflection; (2) Lower atmospheric turbulence, lower atmospheric winds and waves, and mesosphere and lower thermosphere phenomena; (3) Meteorological applications with the Indian MST radar, operational use of wind profiler networks, diverse aspects of meteorological studies with ST radars, and middle atmosphere meteorology; (4) Highlights of coordinated observations, new technical developments, and new achievements at facilities and observations. A total of 162 papers were presented, whereof 124 were given orally, and 38 displayed as posters. Lively discussions highlighted the Workshop presentations. Working group meetings took place in the evenings. The chairman of ISRO, Dr. K. Kasturirangan, had invited the Workshop participants for a pool-side dinner during which young representatives from each continent gave short speeches. Another evening was governed by an stirring cultural event at Rudhraksha Farm House in the rural outskirts of Bangalore, during which a variety of exquisite Indian dances, performed by professional actors, gave an outstanding impression to the participants.

A final plenary session, presided by the chairman of the international steering group of MST8, took place during which sessions were summarized, recommendations on scientific, operational and educational activities were adopted, the Workshop format was discussed and activities between workshops considered. Five standing working groups were reconfirmed or created. These are: (1) System calibrations and definitions (chaired by: Dr. J. Röttger), (2) Analysis and data validation (Dr. M. Yamamoto and Dr. D. Holdsworth), (3) Accuracy and requirements for meteorological applications (Dr. G. Nastrom), (4) International collaborations (Prof. P. B. Rao), (5) Studies of transient phenomena such as meteors, lightning, etc. (Prof. B. Lokanadhan.)

The plenum accepted an invitation by the French delegation to hold the next workshop MST9 in March 2000 in Toulouse. The Workshop was closed by warm words of thanks by Dr. T. VanZandt, who expressed on behalf of the participants deep appreciation to the organizers for the excellent accomplishments and completion of the Workshop.

Abstracts of the presented oral and poster papers were included in a book of abstracts published by the Indian Space Research Organization, ISRO. The final publication of extended abstracts in the workshop proceedings will be in a Handbook for STEP, published by SCOSTEP.

The contributions to and the performance of this Workshop MST8, as well as the School SAR, proved again the profound development of the technical, scientific, operational and educational directions of the MST radar community.
Jürgen Röttger

FORTHCOMING MEETINGS

This Chapman Conference will bring together astronomers, astrophysicists, plasma physicists, solar physicists and planetary magnetosphere physicists currently conducting research involving the interpretation of long wavelength electromagnetic radiowave observations in terms of the physical properties of the source region and the medium between source and observer. One basic objective is to foster better communication amongst these diverse groups of scientists so as to advance the understanding of this topic and to generate more frequent collaborations amongst these diverse groups. The history of radio astronomy has amply demonstrated that it can be characterized as the "science of new phenomena." Over the past 5 years, there has been a plethora of new observations of solar system sources including the Sun, the magnetospheres of the outer planets, the Earth and the Heliosphere boundary. Many highly significant discoveries have been made in the past several years. This Conference will be a unique opportunity for researchers across the field to exchange ideas, learn of the latest scientific and observational techniques and to motivate younger scientists to become involved in this field. Despite the undeniable fact that the opening of each new frequency band has seen discoveries of entirely new phenomena, a sine qua non has been adequate antenna gain. With the development of new observational techniques, including space-borne interferometry and aperture synthesis, to be covered as part of the conference, observations of the cosmic background distribution and spectra of a large number of discrete sources will be possible for the first time at long wavelengths. This capability will open a virtually unexplored part of the electromagnetic spectrum. It will also greatly improve our observations of solar system sources by at least an order of magnitude. We anticipate that this Conference will lead to new mission concepts and collaborations concerning such future missions, their data, and their interpretations.

The Conference will consider new methods of exploring sources within the heliosphere. These include such missions as SIRA (Solar Imaging Radio Aperture), and STEREO. The essential connection with ground-based long wavelength observatories will be an integral part of the program. It will also discuss proposed missions such as ALFA, lunar orbiting observations, etc. for viewing with sufficient angular resolution to observe discrete sources and for mapping the cosmic background. A further objective is to demonstrate how an instrument developed for observing cosmic sources can also be used to advantage for the exploration of solar system sources.

In addition to invited tutorials and reviews, ample time has been set aside for contributed oral and poster papers.

The Organizing & Program Committee consists of the following individuals J. L. Bougeret, G. Dulk, W. Farrell, Sang Hoang, Dayton Jones, T. Kuiper, M. Kaiser, N. Kassim, R. MacDowall, H. Rucker, R. Stone, K. Weiler, P. Zarka

List of Invited Presentations
Day 1: Solar Radio Emissions
Type III Radio Bursts
Type III Radio Bursts
Type II Radio Bursts
Type II Radio Bursts
CMEs, Shocks & Radio Emission
Radar of the Sun
Radio Wave Propagation in Corona & Solar Wind
Theory of Type II & III Radio Emission

Day 2: The Terrestrial Magnetosphere
Radio Emissions from the Earth's Environment
Radio Wave Propagation: Earth's Magnetosphere
Quasi Thermal Noise: The Long Wavelength Limit
Polar/Geotail Observations of Auroral Kilometric Radio Emissions
WIND S/C Observations of Long Wavelength Bursts
Terrestrial Radio Continuum
Role of Electrostatic Waves in Radio Wave Generation
Theory of Planetary Radio Emission
Radio Emission from Lightning

Day 3: Planetary Radio Emissions & Outer Heliosphere
Radio Emissions from the Outer Planets & Moons
Radio Observations of the Outer Planets & Galileo Results
Theory of Planetary Radio Emissions
SL-9 Impact of Shoemaker-Levy at Jupiter
Radio Observations of the Heliosphere Boundary
The Synchrotron Maser- A New Emission Process

Day 4: Long Wavelength Astrophysics
Potential of Long Wavelength Radio Astronomy
Cosmic Rays, Gamma Rays, & Long Wavelength Radio Emissions
Effects of Ionized Gas at Long Wavelength
Interplanetary Medium; Scattering Processes at Long Wavelengths
Interstellar Medium: Scattering Processes at Long Wavelengths
What does the Sky Look Like at Long Wavelengths?
Supernova Remnants at Long Wavelengths

Evening Banquet: Jean-Louis Steinberg honored Guest and Speaker

Day 5: Radio Telescopes at Long Wavelengths
Ground-Based
Long Wavelength Astrophysics
Giant Meter Wavelength Telescope (GMRT) & Mauritius Telescope
VLA at 74 MHz and NRL Plans for a Long Wavelength Array
Ukrainian UTR-2/URAN System
Space-Based
Capabilities/Limitations of Long Wavelength Observations from Space
Lunar Orbiting Radio Telescope (LOREX)
Lunar Surface Arrays (LNSA, VLFA)
The Astronomical Low Frequency Array and SIRA
Instrumentation for Space Based Radio Observations

Abstract Deadline: July 12, 1998
Preregistration Deadline: September 1, 1998

Additional information about this Conference may be found on the AGU Home Page:
http://www.agu.org/meetings/chapman_past.html
or by contacting either of the conveners Jean-Louis Bougeret: DESPA, Observatoire de Paris-Meudon Place Jules Jannson 92195 Meudon, Principal Cedex, France. Telephone (33)-1-4507-7704.
E-mail: Bougeret @megasy.obspm.fr

Robert G. Stone: Laboratory for Extraterrestrial Physics, Code 690, Goddard Space Flight Center, Greenbelt, Maryland 20071. Telephone (301) 286-9631 E-mail: Stone @URAP. GSFC. NASA .GOV
R. G. Stone

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 electric current is a unique parameter among many describing magnetospheric phenomena. The current is divergence free for phenomena we are dealing with, and therefore we need to consider a current system rather than a current itself as a local parameter. Furthermore, current systems determine the electromagnetic energetics of the magnetosphere.

This is the right time to have a conference on magnetospheric current systems. At present there are many new satellites making measurements in various regions of the magnetosphere, and the distribution of ground observations is unprecedented. Advanced measurements of electromagnetic fields and particles by new low-altitude satellites have brought us new insights about magnetosphere-ionosphere coupling processes. The simulation field has benefited from increasing computer capabilities to reproduce the dynamics of the magnetosphere. Magnetic field models have benefited from decades of accumulated spacecraft observations, while new findings of planetary magnetospheres continue to excite us. This Chapman Conference will provide an ideal opportunity to discuss all these achievements and will foster communication among people working with different approaches.

The following is the member list of the Scientific Program Committee for this Conference:
Cowley, S. W. H., (Leicester Univ., UK); Friis-Christensen, E., (Danish Meteorological Inst., Denmark); Fujii, R. (Nagoya University, Japan; Co-chair); Greenwald, R. A., (JHU/APL, USA); Haerendel, G., (Max-Planck Inst., Germany); Kamide, Y., (Nagoya University, Japan); Kan, J. R., (University of Alaska, USA); Lyon, J. G., (Dartmouth College, USA); Lysak, R. L., (University of Minnesota, USA); Marklund, G. T., (Royal Institute of Technology, Sweden); Mukai, T. (ISAS, Japan); Ohtani, S. (JHU/APL, USA; Co-chair); Opgenoorth, H. J., (Institute of Space Physics, Sweden); Rostoker, G., (University of Alberta, Canada); Russell, C. T., (UCLA, USA); Sauvaud, J., (CESR, France); Siscoe, G. L. (Boston Univ., USA); Slavin, J. A., (NASA Goddard SFC, USA); Tsyganenko, N. A., (NASA Goddard SFC, USA); Walker, R. J., (UCLA, USA); Wolf, R. A., (Rice Univ. USA).

We dedicate this conference to Dr. Thomas A. Potemra, who passed away on April 3. He was a member of the Program Committee of this Conference, and was the convener of the Chapman Conference on "Magnetospheric Currents" (1983).

Ryoichi Fujii and Shin Ohtani (Conveners)
Ryoichi Fujii: rfujii@stelab.nagoya-u.ac.jp
Shin Ohtani: ohtani@jhuapl.edu

An increasing number of researchers are interested in the human causes and impacts of global environmental change, as well as recognizing that local and regional scales are critical for their studies. Following two successful international meetings held at Duke University in 1995 and at NASA in 1997, the 1999 Open Meeting aims to promote exchanges of information on current research and teaching and to encourage networking and community building in this emerging field.

The meeting, hosted by the Institute for Global Environmental Strategies (IGES, Japan), will be held in Shonan Village, an international conference center in a scenic setting southwest of Tokyo.

Plenary talks and commentaries on the following topics are planned: Conflict and the Environment - the interaction between conflict prevention and resolution and environmental issues; Lifestyles, Attitudes and Behavior - their role in driving global environmental change and the potential role of alternative development paths;
Decision-making Processes in Response to Global Environmental Change - in particular the linkages between the international, national and local scales and the obstacles to the transfer of policy instruments and norms from one region to another;
Land Use and Land Cover Change - the social dimensions of changing land use, human settlements and land cover patterns;
Valuation of Ecosystem Services - current thinking on the values that can be attributed to services such as climate regulation, water supply and recreation;
Demographic Change and the Environment - the relationships between population growth and other demographic factors, for example migration, and environmental change.

In addition to plenary talks, there will be a large number of sessions devoted to the presentation of research results. The International Scientific Planning Committee welcomes the submission of abstracts for individual papers as well as proposals for entire sessions. Selection of the proposals/ abstracts will be based on quality and the need to create a coherent, balanced meeting agenda. The Committee encourages the participation of researchers from a broad range of disciplines, including researchers from developing countries and countries with economies in transition, as well as young researchers from all over the world. For these latter categories of researchers, the aim is to provide financial support for some participants whose abstracts are selected for the meeting.

For further information on the meeting, including instructions for the submission of abstracts, please consult the IGES Web Site (http://www.iges.or.jp/), or send an e-mail to hdgec@iges.or.jp, or mail/fax your inquiry to Mr. Yasushi Itoh, IGES at Shonan Village Center. (Fax: +81 468 55 3709). The deadline for submission of abstracts is November 1, 1998.

The official address of "Shonan Village" is 1560-39, Kami-yamaguchi, Hayama, Kanagawa 240-0115, Japan. Shonan Village Center is a building complex consisting of modern and pleasant conference rooms, lodging facilities, and restaurants. The conference rooms are equipped with high-tech devices (e.g. copiers, fax machines, OHPs, projectors, VCRs) for presentations.

The Center is located on the Miura Peninsula which divides the Bay of Tokyo and the Sagami Bay. It is an hour's ride on the JR train (Yokosuka-line) from Tokyo Station to Zushi Station which is the nearest train station to the Center. Local bus is available directly from the Zushi Station to the Shonan Village Center. The bus ride takes another half an hour through the local town of Zushi and Hayama, known as the site of the Emperor's summer residence. If you are arriving at the Narita International Airport, there is a direct train line that connects the airport and Zushi Station. The timetable connecting the flights and the trains will be sent to the participants. The Center is located on the top of a hill, offering a fantastic view of Mt. Fuji and the Sagami Bay which is dotted with bathing beaches and marinas famous for marine sports. There are other sports facilities nearby, including golf courses and tennis courts. Misaki, located at the end of the Miura Peninsula is famous as the Tuna fishermen's harbor, and early morning tuna auctions can be seen at its fish market, one of the biggest in Japan.

The Center is only half-hour away from Kamakura, one of the most famous sight-seeing spots in Japan. Kamakura was the ancient capitol of the Samurai era, and is full of temples and shrines. Other famous sites are accessible from the Center such as the exotic harbor city of Yokohama famous for the Chinatown and the Hakone mountains.

Caroline Nunes, Office Manager LUCC International Project Office, Institut Cartografic de Catalunya Parc de Montjuic s/n 08038 Barcelona, Spain Tel. 34 93 4252900 Fax. 34 93 4267442
lucc@icc.es or carolinen@icc.es
http://www.icc.es/lucc

This session will be held during the Assembly of the International Association of Geomagnetism and Aeronomy (IAGA.) It will address the possibility of a comprehensive synthesis of science studies across the variability in the Sun's history in the last centuries. Topics will include history, archaeology, solar physics, astrophysics, aurora physics, geophysics, meteorology and environmental aspects. It deals with the so-called minima in the Sun's history (Spörer, Maunder, LaLande, and Wolf Minima) and other variabilities during the centuries.

Deadline for abstracts is January 15, 1999. For additional details contact the convener, Dr. Wilfried Schröder, Hechelstrasse 8, D-28777 Bremen-Roennebeck, Germany.

CALENDAR OF EVENTS

June 1-5: International Symposium on Space Plasma Studies by In Situ and Remote Measurements, Moscow, Russia. Contact: M. I. Verigin
(verigin@iki.rssi.ru)

June 22-July 3: 1998 Cambridge Symposium/Workshop on the Physics of Space Plasmas, Lisbon, Portugal. Contact: Mary Terhune (mst@space.mit.edu) July 6-10: International Working Meeting: Cooling and Sinking of the Middle and Lower Atmosphere, Moscow, Russia. Contact: T. P. Prisvelaya (gcras@wdcb.rssi.ru)

July 12-19: 32nd COSPAR Scientific Assembly, Nagoya, Japan. Contact: (COSPAR@paris7.jussieu.fr)

July 13: COSPAR Symposium C2.2: Extra-Terrestrial Influences on the Ozone Layer, Nagoya, Japan. Contact: J. Lastovicka (jla@ufa.cas.cz)

July 14-15: COSPAR Symposium D0.6: The Transport of Galactic Cosmic Rays on the Heliosphere: Observations, Simulations and Theory, Nagoya, Japan. Contact: Z. Fujii, Solar Terrestrial Lab., Nagoya Univ., Nagoya 464-01, Japan.

July 16: COSPAR Symposium E2.3: Magnetic Reconnection in the Solar Atmosphere, Nagoya, Japan. Contact: Masahiro Hoshino (hoshino@stp.isas.ac.jp)

July 17-18: COSPAR Symposium D0.5: Space Weather: Physics and Applications, Nagoya, Japan. Contact: G. Rostoker (rostoker@space.ualberta.ca)

July 17-18: COSPAR Symposium C3.2/D0.9: Planetary Ionospheres and Magnetospheres, Nagoya, Japan. Contact: A. Nagy (anagy@umich.edu)

July 19-20: SCOSTEP Bureau, Taipei, Taiwan, Contact: J. H. Allen (jallen@ngdc.noaa.gov)

July 21-24: Special Session on Space Weather: 1998 Western Pacific Geophysical Meeting, Taipei, Taiwan. Contact: (psong@engin.umich.edu)

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: (date to be announced) Fifth Latin American Conference on Space Geophysics (COLAGE-V), San Jose, Costa Rica. Contact: Jose Fco. Valdes-Galicia (jfvaldes@tonatiuh.igeofcu.unam.mx)

January 11-15: Chapman Conference on Magnetospheric Current Systems, Kona, Hawaii. Contact: R. Fujii (rfujii@stelab.nagoya-u.ac.jp)

June 24-26: Open Meeting of the Human Dimensions of Global Environmental Change Research Community, Kanagawa, Japan. Contact: Caroline Nunes, (carolinen@icc.es)

July: Long- and Short-Term Variability in the Sun's History and Global Change, Birmingham, UK. Contact: W. Schröder, Hechelstrasse 8, D-28777 Bremen-Roennebeck, Germany