UIDDLE

ATHOSPBEBE

PBOGPAH

Edited by

C. F. Sechrist, Jr. Cbaixun n4P Publiutionr Carrittee

Publirhed for the ICSU Scientific Camittee on Solar- Terrestrial Phyrics (SCOSTEP) with financial arsirtance io part froll the World I(cteoro1ogiul Organization, in part from Unesco Subvention 1981-1983-DG/7.6.2/rub 13 (SC), adin p8rt fram the National Aero~uticrand Space Administration Grant NASW 3646. Volumer 6 and 7 were printed and dirtributed by NASA.

Copier available from SCOSTEP Secretariat, University of Illinois. 1406 W. Green Street, Urbms. Illinoir 61W1 CONTMTS COWTM lS ...... iii

ACBQIm...... v

P(LBf 1 MP STEERING CO-EE IEETIISC CONDERSED KfhTTLS. OTTAWA. MY 1982 ...... 1 PART 2 APPROVED AND PROPOSED MAP PBOJECf BEPORTS ...... 15 PART 3 NATIO!CAL BEWETS ...... 55 PART 4 CmmEREPORT ...... 77

PART 5 PW ARD lEG SPORTS ...... 79 PART 6 WORKSILOP BEPORTS ...... 95

PART 7 mUNCE!ENTS AND CORRIGMWW ...... 149

13-LVG PAGE BLCW NOT FnAfEO AXA Antarctic Middle Amosphere Progr~

ATUP Atmospheric Tides Middle Atmosphere Progrr

CAW Cold Arctic Ilcsopaur Project

DYNAXICS Dylurica of the Middle Amsphere in riinter-Coordioated Studies

GLOBlJET Global Xeteor Observation System

GMBUS Global Budget of Stratospheric Trace Constituents

GOSSA Global Observations and Studies of Stratospheric Aerosols

GBAW Gravity Waves and furbulcace in the Middle Atwsphere Progrr

MC Middle Atmosphere Cooperation

ULV&ACS Xeteorological and Chemical Variables as Zonal Averaged Cross Sections

I(AE Middle Amosphere Electrodynamics

lIAP fiddle Amosphere Progra

WCIEO XAP Central Infomation Exchage Office

MPWL IUP Rcvrletter

HAP SC XAP Steering Camittee

kSG MAP Study Group

OZW Obaervations of and Sources of the Spatial and Taporal Variability of Ozone in the Middle Atwsphere on Climatological Time Scaler

PW Pre-IMP Project

SSIM Solar Spectral Irradiance Ilersursents

SIRATbLERT Stratospheric Warring Alert

STBATWARM Stratorpberic Warming

SWAIB Stratwarm Xesospheric Project

WINE Winter in Northern Europe Project naP STEEBIIK; COIWmE IEETUK Ilmby, thy 17, 1982 1400 - 1800 burs

1. Chima S. A. khill velcond the attendees to the meeting. & mentioned that this vu the first WSC reeting since the beginning of WIP on Jmry 1, 1982. All indications are MP is off to a resounding start. PMPs and l6Gs have ken very ruccessf ul in catalyzing vat in dif fercot areas of the riddle atmosphere, and the Colllittee vill hear reports fra the groups during the courr of the meeting. Be also briefly described the progress ude in the Publiution, Dyummics C.1ead.r aad Data Wgment CQLittees.

2. The ninutes of the last Steering Caittee Ilceting, at Edinburgh, US., August 13-16, 1981 vere apprwed.

3. Pollwing 8 decision r&during the iast Steering Colrittee lketing, thc Cbixun vrote to the Ctnixmen of RlPs and IsCs asking tha to decide m the future of their groups md report to the Steeri~ Mttee. The follouing are the brief reports and propouls of the group8 aad actions takem by WSC on their proporls:

P1B-1 - Dr. K. kbittke: PMP-1 hs coopleted its job; vorkmhops have be- rucces.ful; it .bould continue as a MP project emtitled "Dy-ic8 of the Middle Atmosphere in Winter - Coordi~tedStudies" (DYIUHICS) vith incrurd membership. Thc Caittee agreed.

PHP-2 - Dr. I. Birota: Previaus reports of the Project bebeen published in Volume8 1 and 2 of the MP Eandbok. Further diacusaions and suggestions vere rde at Ester Park during the Workmhop thy 10-12, 1982. The project vill be disaontinued but the study of equatorial wave dynamic8 vill continue throughout W. The Clittee agreed to dis- continue the Project.

PMP-3 - Dr. J. Gille (report u& on by 18, but included here for con-inuity): Past activities concern six or seven erpcrhents involving SAGE, m, SAH-11 and LIB. Future activities appear to be lw. USA is becomiag more active in the area. Tbere vill be sae experirntr f ijing on the Space Shuttle. .ad some planned for OARS. Pmpow the Group isme a final report urd discontinue the project; agreed by the Colrittee.

PHP-4 - Dr. 3. Bunett (report made on Hap 21, included for continuity): The project should be continued as a MP project. It is now techniully possible to carry out the study, but more manpower is needed. Dr. Bovhill vill discuss the problem vith Drr. Buctt, lhous and Gille and report to the amittee. (Note: After the SC meeting, Dr. Bwhill talked to J-es Russell who agreed to serve as the Orgmirer of the Project .I

PW-5 - Dr. P. Simon: During the Yaksbop at Yuhingtaa, D.C. the previous veek, all participants agreed that the activity should be continued as a W project vith the ..re title. MAPSC apprwed the pr. ect vith the recorcndation that the group should be reconstituted vith mlargtd mahership.

-1: Dr. Holton had propord (by uil) to discontinue the gmup. Fi-1 report vas presented last year. WSC agreed.

-2: Dr. Il.hlun bd proposed (by uil) to discontinue the group. Fi~lreport vas presented last year. MAPSC agreed.

IISC-3: Dr. Geller - Report was publimhed as part of llbP Baudbook 3. The group should be d%rcontinued. Two new llbP pro jects will be propomed. WSC agreed to discontinue the gmup. m-4: Dr. Vollurd - The report vas published in lULP Handbook. Thc group should be continued as a ocv W project vith a new Cbirun. Tb Ckttae agreed that the vork should continue. The Chairun will contact the aew Chirun to ask him to sutmit a prospectus for the ocw project .

IISC-5: Cammication from Dr. Arnold stated that the Study Group should continue; he suggested Dr. P. XcCorrick as the co-ch8i-n md Dr. E. Arijs as a new uber of the Group. MF'SC agreed. Dr. hold also mentioned that a report on IM;-5 is being prepared and should be received for publication in a UAP Handbook in the near future.

4. Reports of HAP Projects: The approved lfAP projects are W/VIIIE, GLOBUS, MA, a;d CAW.

?!!/WIRE: Dr. U. Von Zahn reported that the original coordinator of the project. Dr. Krankwsky, hs resigned. The Coaittee agreed that Dr. Von Zahn will succeed him as the coordinator. Dr. Von Zahn presented the status of the project.

W/GLOBUS: Dr. U. Von Z&n reported that the coordinator of the project. Dr. Seiler, has resigned and the Camittee agreed that Dr. D. Offermann vill be the new coordinator. Two integrated c-pmigns are presently in the planning stage. Details are included on the Nations1 MAP report of FRG (to be included in Volume 7 of Handbook for W).

MAP/U: Dr. T. Ragata reported the activities for Dr. Hirasava, vho could not attend the meeting.

W/CAUP: Dr. G. Vitt reported the activities for Dr. Bjorn. 5. CJcv W Projects:

Global Obsemation and Studies of Stratospheric Aerosols (cOSSA) : Tk project was origi~llyproposed in Emburg last yeu. The Chimn h.8 received apprwal by mil ballots f ram -bra of the Steering hittee. llrc aphuis of the project is entirely on the coordination of experhts making ruuraents of stratospheric events for morphological studies. The Corittee apprwed the project. Dr. P. NcCormick will k the coordinator.

Amospheric Tides Middle Atmospheric Progrm (ATHAP): This is one of the rrcv projects propord by -3. Dr. Geller presented the proposal to the Carittee. Dr. J. Forks agreed to coordbte the project. The dtteeapproved the project in principle, eubject to an urderstl~ding vith IMIA of IbnaP.

Gr8vity Wave and Turbulence in the fiddle Aaosphere Progrr (GEARUP): This is the second of the new projects propord by IM;-3. Dr. Geller presented the proposal to the Camittee. Tbe project vas approved by the Ckttee. The Cluirun will discuss with Dr. Geller the reber- ship of the group.

Global Hetear Observation System (GLOBIET): The project was originally proposed last year in €dinbur&. The SCOSTLP Buruu has appointed an ad hoc committee to study the proposal. At its meeting this week, the Buruu decided that GLOB!ET should be in MP. Drs. Roper and Isshchew prepared the planning docent. Tk Cwittee approved it as a ocw lYLP project.

Stratwan Hesospheric Progrm (SYW): Dr. Offerunn proposed this progr8m of coordinsted winter wasuraents of atmospheric parmeters (temperature, wind, etc.) at wsospheric beights for the period December 1, 1981 to spring 1984. It will k a sub-project of the DWCS project. Tk Camittee approved the proposal.

Spogtic Ozorr bps: During the Steering Camittee Meeting last pear. Dr. A. D. Belwnt propoaed this project. Sae rwisions were suggested, resulting in a new propoul to the Committee. Dr. W. I. Godson commented that Y1D has considered the effort of setting up global networks for ozone measurments to be too expensive and will not be supported by member ~tions. It was suggested that the Chaiaan should discuss the question with interested scientists and report to the Colrittee by mail.

Transport: (Discussed on by 21, included here for continuity.) Dr. J. Gille proposed this project re study the transport of species. It was recognized that, to some degree, this is similar to Dr. Belmont's proposal. It was suggested that Drs. Gille and Belmont discuss this matter and define the project more clearly and submit a written report to the Steering Caaittee for consideration.

6. Ucv IMP Study Groups:

~surcrcotsof Middle Atmosphere Parreters by Lmg Duration Ball00~ Flights: During the 6lrhurg Xeeting last August, Dr. J. Blront pro- peed the project. Tht task of coordinating such long duration circupolar flights interaatiomlly is difficult. HAP cm certainly make a contribution. The proposal was aunounced in the last isme of the HAP Reusletter; tvo proposals have been received from France. Follcrving the decision at the last Steering Collittee Meting, the Chinun polled the member. of the Steering Cmittee by nil. A favorable but mt wmniwur responw vas received. Thc Ckttee approved a Study Group to firm up the plaus for mercuraents, to include more intermtiom1 groups aud to extend the scope to both herrispheres.

Intermtiom1 Equatorial Observatory: As an out- of the Vorkshop at Estm Park, a ow ST radar in the equatorial region was propord. The aim is to study tide., equatorial wnes, gravity waver, strato- mesosphere interactione, etc. The Carittee suggested that the scope be brcxdened beyond just an STradar facility. Other types of facilities such as Lidar, etc. should alw be included. The Camittee :pprtied a Study Group on Scientific Arpccts of Interrutiorvl Eguatorial 0b.ervatory. The Cbirun vill ask Dr. bto to chair the group.

Amospbcric Penetration of Solar Radiation in the Range of Schumnn- Punge Bauds: (Discused llly 18.) Dr. J. E. Frederick propord this project last year. The Camittee suggested that the study ahould not be limited to just SchuunrRmge Bmds. It approved the proposal. Dr. Predcrick will be the Chirun.

A-spberic Chemistry. (Discurrd on 11.9 18 aud May 21.) Dr. Simon originally suggested the Study Group last year with ozone chemistry rs the main subject, The Camittee suggested the study be broadened to atmospheric cbcristry and to include the wsoephere, especially the meaop8u.c. Tbc Carittee approved the establishment of the Study Group vith Dr. 6. Witt as Chirun.

7. Data huagstot Camittee Report: Co-Chairman Drs. Kirota and brtuun reported.

Several circular letters started the activities in October 1982.

J. E. Allen of UDC-A-SfP Boulder, has agreed to serve as Secretary of the MAP-Data Xmugment Caouttee and to isme and circulate the nccerury information in cooperation vith the two Co-Chiaen Dr. I. Eirota and Dr. G. Eutunn. At Ottawa, first discu~sionivill be started on a revised "NAP-C Chaptern for the Guide to Internrtioml Data Exchange vhich vill be discussed by the ICSU Pael for World Data Centers in Septaber.

A short questionnaire vill be prepared for the next HAP Newsletter to get latest information from the MW Principal Investigators (HAP PI). If necessary, this questionmire might be issued by J. E. Allen (VDC-A) rather than with the IUP Nevsletter.

8. Publications Camittee report: The Secretary presented Dr. Sechrist's report to the coatnittee:

Cdttee hbership: C. F. Sechrist, Jr., Chaiman, R. D. Bojkov, R. J. liurgatroyd, and V. V. Viskov.

MP Nevsletter: The HAP Nevsletters are now published as Special Issues of the Upper Acrospheric Progras Bulletin vhich is funded jointly t*~the NASA Upper Atmospheric Research Progrm and the High Altitude '01 lution Pmgra of the Federal Aviation Administration. IUP Ncumlett~rswere published and distributed in July 1981 md in January 1982. -'he aext isme of the HAP leusletter will contain condensed minuter of tht MP Workshops and HAP Steering Cmmittee Meetings held in Hay 1982. It vill be distributed in August 1982.

H~ndbookfor W: Volumes 1, 2 and 3 have been published and distributed. Voltme 4, covering the W Asserbly and UAP Open Meeting. van published and distributed in April 1982. Volume 5, A Dynamic Clktology of the Stratosphere, was published in early Hay 1982. It vill be distributed during the latter part of by 1982.

Proposed Future Topics for Volumes in the Handbook for UAP: MP Directory (~olmc6, July 1982); MP Workshops and Symposia (Volume 7, September 1982) ; Satellite experirents including SAGE, SHE, WOE, A'MOS, LBIR, W, DE, WS-C (Volruoe 8, January 1983); and ground- bard techniques including partial reflection ionization drifts, middle- atmosphere radar, laser radar, meteor radar (Volume 9, April 1983).

Contributions for the W levsletter: More contributions for the MP levsletter are urgently needed, in order to publish the Newsletter on a regular schedule.

Suggestions and Contributions for Handbook for MP: The Publications Coorittee velcmes suggestions of future topics for volumes of the Handbook for MP. Suggestions and contributions should be sent to: Professor C. F. Sechrist, Jr., Department of Electrical Engineering, University of Illinois, 1406 W. Green Street, Urbana, Illi-,air 61801 USA. The question of the MP Newsletter was discussed. The Coasittee decided on the follwing dates for publication of the Nusletter: 4 issues per year, August 1, Novmber 1, February 1, md by 1. Dead- lines for receipt of contributions in Urbana: July 1, October 1, January 1 and April 1. The Committee agreed unanimously on the usefulness of volumes of the Handbook. Tuerday, Hay 18, 1982 1000 - 1300

1. Dynamic Calendar Couittee Report: Dr. V,'m Zandt reported that the llbP calendar for 1983 ir under preparation. It will have the aanr farut ar the me for 1982. He arked that cr~mmentrand information be rcnt to hir vithin the ncxt 2 to 3 weeks.

2. llAP Workahope:

PXP-1 Workshop (Drs. Labitzke and Gille): The workshop was held at NU&, Boulder, Colorado, Hay 11-14. Tventy 8c;entistr from FBG, France, Jap, United Kingda and USA participated. Data from four satellites were -pared vith conventional data. Three selected dayr were dis- played for discurrion (1/2/79, undirturbed; 1/26/79, wave 1; 2/16/79, vave 2). Good agreement was obtained, erpecially for 1/2/79, but more difficult for disturbed days. Dr. Labitzke will write to USSR for data exhange. Dr. E. R. Schmerling mentioned that if preselected days are poerible, USA CUI work vith tvo days' notice. This will be considered by the DYNAXICS project . Later Workshops were suggested.

Workshop on Solar Spectral Irradiance Xeaaureolents (Dr. P. C. Simon): The Workshop was teld in Washington, D.C., Way 12-14. W measureolent calibration procedurer and new methods were discussed. Plane vere made for future long term mcarureolents to prepare for experiments on the Space Stlut tle and OARS. Standard calibration procedures should be follwed by each group.

Future Workshops vere proposed. Workahop on Equatorial fiddle Atmorphere )Iururmentr and fiddle Atmosphere Radars (Drs. Hirota, Kato; local arrangeaente, Drr. Balsley and Van ~andt):nay 10-12. There were about fifty participants from Australia, Canada, France, India. Japan, Taivm, United Kingdom, and USA. Six sesrions and two panel dis- cureions were held. The future of middle atmosphere radar was dircursed. The need for an equatorial &ST radar was addressed.

Swrier of the three Workshops will be provided by the organizers and publirhed in W Handbook Volume 7.

3. Icw IUP Workshops:

PelWorkrhopr: Drs. Labitzke and Gille proposed to hold two more PMF+-1 Workshops. One similar to the first PMP-1 Workshop, is planned to be held rometime in March-April , 1983 at Oxford, UK. The Oxford group vill hort it. Another more elaborate workshop is planred to be held at Haburg, PBC, during IUGG, August 1983, with emphasis on scientific rerultr derived from data. The Committee approved the proposal. Workshop on Technical AbpectS of MST Radar: Inspired by the successful Workshop at Estes Park, Drs. Bowhill and Liu propocred this Workshop to concentrate on such topics as the optimization of design parmeters; lumped vs. distributed systems; nature of the target? and econcmic aspects of global network, etc. The Workehop will be held in Urbna, Illinois, Uay 23-27, 1983. Dr. Van Zandt mentioned that a symposium on waves and turbulence will be held in March/April 1983 at Boulder, Colorado. The Urbana Workshop may also be timed with respect to that symposium. Drs. Bowhill, Liu, md Van Zandt will discuss the matter. The Cornmitttee approved the proposal. Dr. Witt reported that CAMP is planning a Workehop in the summer of 1983 which might be the same one planned by Dr. G. Reid. He will coordinate and submit a formal propo~l by July 1st.

4. MAP TWO: Because of the long lead time necessary in many countries in planning scientific progrms and also due to the cxpected delay of some projects in HAP, HAP TWO was suggested at Edinburgh. The Chairman has polled the Steering Committee on this question by mail and has received responses from many mcmbers with varying degrees of support of the idea. He presented a time scale; MAP 1982 - 1985, using existing facil'.ties and techniques to study the climatology, processes and interaction of the middle atmosphere; HAP TWO, 1986 - 1989, using new networks of stations and new techniques developed during HAP, to measure new paraneters of middle atmosphere and solve related atmospheric problems; TESS (Transfer of Energy in the Solar System), after 1990, using all solar-terrestrial measurement techniques to understand the energy budget of the solar system from the surface of the sun to the surfaces of the planets. National Representatives reported the approximate time schedules for new MAP facilities in their countries that vary from late 1983 to 1965. The continuity of the project and the need for long term time series to study atmospneric phenomena were pointed out by several Representatives. Dr. K. D. Coll, the President of SCOSTEP, explained to the Committee the operational philosophy of SCCSTEP. Each scientific progran goes through three phases; the planning phase, the experimental phase and the data analysis phase. SCOSTEP provides different levels of frnding for the different phases. MAP is now the principal project of SCOSTEP. After the extensive observation period of HAP, MAP TWO cannot expect the same level of funding from SCOSTEP. After the data-collecting period of MAP, time will be needed to digest the data and to study the physics. Dr. Bowhill then proposed the following resolution:

The MAP Steering Committee, CONSIDERING that many new measurement facilities will come into existence only near the end of 1,IAF'; CONSIDERING the requirenent of atmospheric observations for a long time series; RECOGNIZING that SCOSTEP may initiate new prograns in the late 1980~;and ANTICIPATING that XU rcientirtr will fully participate in tho- progrrpa with the new technique#; BEQUESTS the Bureau of SCOSTEP to approve further period of XU (MP TWO) for th time period January 1, 1986 through December 31, 1988.

The Caoittee voted to pOltpOm! the decision on the rerolution until the next rraion on Friday, ll~y21. Friday, Play 21. 1982 1000 - 1300 hours

1. Hiddle Abasphere Cooperation (MAC): The resolution put forward ky Dr. Mill during the last sesclon was discussed. Dr. Godson suggested an rendrent to change "WP NO" to "Uiddle Ahasphere Cooperation (HAC)"; this vas pas== L the Coaitte. Dr. Bovhill explained that the level of ftmdiag durin!: MC vill be negotiated vith the SCOSTEP Bureai. Also iF UARS is launched during ?989, then UAES-related ground-bawd progras ceuld be lULP contributions to IESS (or sow other equivalmt SCOSTEP progra). The Conittee approved the wtion. The request will be sent to the SCOSTEP Bureau for approval. (It was subrcquently approved by the SCOSTEP Bureau. Saturday. by 22.)

2. Ilatio~lReports : Representatives from tvelve countries preaented their artio~lMA?' reports. They vere:

Czechoslwakia Dr. V. Bucha Finland Dr. S. Urpo France h.. M. L. Cbnin FRG Dr. li. Von Z.bn (reported May 17) CDR Dr. J. Iaubenheim Hmgary Dr. P. Bencze (vrittm report) India Dr. A. P. Witra Sveden Dr. G. Kitt Japan Dr. S. Kato Taivsn Dr. J. I. Cho (vritts. repcrt) U.K. Dr. L. Tbous (reported Hay 17) U.S.A. Dr. H. A. Celler

The vritteo reports vill be published in HAP Handbook Val- 7.

3. Regionrl Consultative Groups: European Regioarl Conrultetive Craup: Dr. Chanin reported the activities of the group during the lart year.

This grnup was constituted in Edinburgh vhere its first meeting vat held. A second meeting took place in Paris, Prance, on December 16. 1981. The European participation in CAlIP and VINE vere widely discussed, and suggestions of camplaentary experiments by groups not already involved in those progras vere wde. A discussion on the role of EISCAT in the HAP progrm was also discussed, as well as the role of r long-life balloon progrm in HAP. Sae preliminary ideas about the way the Europe- countries uv the evolution of the GLOBUS progrm were discussed.

A short meeting was held in Ottawa on Tuesday, May 18, 1982. The main topic of discussion was the participation of the USSR in the VINE and CAMP proerms, which could not be discussed at *he Paris meeting. A short excha2ge of views about the GLOBES progra was started, but the group did not intmd to interfere with the Steering Camittee of the progr-. This discussioa was carried on later in Lhe week in more detail mder the directicn of the acw CLOBUS Chirun. D. Offemann.

Keeping in mind that this group should not overlap with the activities of the different Steering Camittees of the MAP progras inwctvicg Eurcpem contributions, it is propoaed to uintain the existence of this group with the possibility that my of its meb?rs may suggest a meeting which may te necesnry for topics which are not included is 8 recognized MAP progra, WSC agreed to keep the group in elit-:ence. Dr. Chanin will continue to be the Chairperson.

Asian Kegiornl Consultative Croup: No meeting took place since Edinburgh. Dr. Kato rentiooed that there were eschoges of information between Japan and Taiwan and he expects more interaction in the future. These. houever, were local. The Ccamittee decided to dissolve the group, but the members can vrite to the Chairman asking t~ revive the group if aecesnry.

4. Future Symposia:

Ground-Based Studies of the Middle Atnosphere: Ray 9-13. 1983. Schvcrin, GDK; Dr. J. Taubenheim. Organizer. The First circular in- cluded as an Attachrot. Will not overlap with UCA, IWmeetings in

Joint IAGA - IAHAP Symposium on Uiddle Atlosphere: August 20-26. 198-1. Bmburg, FBC; Dr. R. Hegill, Organizer. Topics arc similar to the Edinburgh Symposium. Tbere will be 11 sessions.

Intenutiounl MP Symposium in Japan: 1984. Kyoto, Japan; Dl- Kato. Organizer. Tte first circular included as an Attacbrt. The emphasis will bz on comprehensive coverage of all topics of HhP. To decide on the dates Dr. Kato will coordinate vith thc Ozone and Radiation Camissions of W and COSPAR to avoid conflicts in timing with their symposia. Re will also seek co-sponsorship fra SCOSTEP, COSPAR. URSI. IAGA, and IAMP. Coordination with Equatorial Aeronmy Sympc)s;um, Uarch 1984, Bang Kong was also suggested.

W Symposium, First Achievaencs of W,in COSPAR: Uay. 1984, Craz, Austria ; Dr. K. Labitzke. Organizer. SCOSTEP Co-sponsor ship is being swght.

5. WCIE OFMCE:

Following the successful information exchange center during XIIS, MAP has planned to establish such an office to provide a focal point for providing timely inf orution concerning events, urprig~s,etc. Let ters have been wnt out by Dr. Bojkov to rteorologiul services and by Dr- Cole to Academies of Sciences of the nations to ask them to consider sending scientists to UDC-A, working 1/2 tire on research and 112 ti- on WCIE for a period of I to 2 years. Two tatative replies have be- received, one fra the FUG and one from 'Ladia. Dr. A. P. nitra presented 8 mw proposal fra India. If the WCIE could be louted in India, thco his country vill be able to absorb the tct.1 clsts in opcating HUCIE, including the publication of the MAP Ilcusletter. Tht Corittee accepted the offer by acclration. Details to be vorked out by Drs, bhill, Uitra and Daniel.

6. J. E. Allen reported thct Dr. itrtnann, co-churun of the Data hgaent Carittee, hs interacted vitb IOIISEE. A set of questionmires vill be distrihrted in the UPKcvsletter to surrey the HAP c~mityon data information.

7. Dr. J. Gille hlggested a testatire vorbhop on Eu1eri.n ad Lagrmgian descriptions of ahospberic chemistry problss. Be vill dimcuss this vitb Dr. Godson to finalize the ideas.

8. Kelt Meeting of WSC: The Corrittee voted to hold the rvxt WSC meeting tte week before 1M;G at Emburg, FBG, in August 1983.

9. Lext Assably: The Chirun propcoed tc hold the wcond naP As~lblyin late 1984 or early 1985 to discuss the future of MAP. Dates sod place to be decided. Approval of agenda

Hitmtes of previous mretings

Pcconstituted PlIP reports

Peconatituted USG reports

MAP Project reports

Deporte on Natio-1 llhP activities

Proposals for new MAP Projects

Proposals for mu MSGs

Data Uuugement Canittee report

Publications Co~mitteereport

micCalendar Camittee report

Deport8 on Workshops: USI-Equatorial W measureaents PnP-1 Solar spectral irradiancce

Future Workshops

Future Symposia: Graz, with COSPAR Japnn GDB, UCA-IAlW FILG, UCA-IAIIAP

Question of HAP TWO

WCIE Off ice

18. Date and location of next meeting Ottava, Cmu& by 17, 18, and 21, 1982

ATMDlmx LIST

AF~LIbnOll

L. A. Aleundrov MP, USSR J. x. Allen YDC- A J. J. Barnett NhP A. Belloat mw G. Beyaon SCOSTEP S. A. Eouhill SCOSTEP G. Brasseur Representing P. Simon, IAU A. Brekke SCOSTEP V. Bucha Representing J. hstwicka X. L. Chin Ratioml Representative. France J. K. Cbo Nationa 1 Represent8tive. Tuvm K. D. Cole SCOSTEP E. R. Dyer SCOSTEP X. Geller MP J. C. Gille COSPAB U. L. Godson lam J. B. Gregory SCOSTEP G. Xartmann UAP I. Hirota IdlUP S. Kato National Representative. Japan K. Labitzke COSPAB C. R. Liu SCOSTEP Secretary L. R. Hegill IAGA A. P. Uitra Representing Y. V. Sauyajulu T. N-gata SCAR E. R. Schnerling NASA P. C. Simon UU A. V. Shirochkov Representing E. S. bzimirovsky N. Smdararoan UAP Coordi~tor,USA J. Taubenheim IAGA I. Thomas National Representative. UK E. V. Thrane National Representati..-e. Norvay S. Urpo COSPAR T. E. Van Zandt WSI 8. Volland nhP U. Von Zahn UAP National Representative, FRG X. Uada IUPAP C. Vitt nhP .At the IW Steerin%Colaittee meeting held at El-pton, Virginia in Hay 1981, the Antarct~cXiddle Atmosphere (-1 progrr vu adopted as om of the coogcratire internrtioml IYP rewarcb projects. Dr. 1. Bira~vaof the Natioual Imtitute of Polar Otuarcb, Tokyo, btue the internrtioarl coordinator.

At the W Assably in Edinburgh, Dr. T. Eirauva presented an outline of the Scientific aims of AW. Thee include investigations of dymiu. structure, atmospheric amposition, particle precipitation, middle atnosphere-lw ionosphere interactions, atrospbric pollption, aod northern-southern polar atmosphere ccprisons.

HAP projects could be usefully coardinmted in the Antarctic and Sub-Antarctic regions. as follws.

Ground-Bard Obsenrations:

Ra&r observations of the electron density aod electric field irregularities in the laver ionosphere. (~ustralia,Jap, OSSR, DSb)

Spectroscopic 0bSe~ati0nSon the visible md infrared region for the wasursmt of variaus atrospheric species. mch as CR4, m20. CO. 0 urd NO . (USA. JAPAN) 3 X Li&r observstions of vertical profiles aod time rariabit_ities of air oolecules and minor constituents, mch as aerosols aod or- in the stratosphere ad alkali metal atas and aerowls in the usospbere .nd the lover theaosphere. (~uatralia.Japan)

Observations of particle precipitation; a11 sky uera, auroral zenith photometers; geagnetic wridiaa scanning pbotaeter; high sensitive TV caera; vertical incidence ionosonde ; riometer. (Australia, France. Japn. Neu Zealad, U11, USSR, USA)

Bal loon Experiments :

Several ballom c.~paignsare foresee0 to be devoted to dynamics, structure, aerosols, atmospheric species, electron ad ion densities, electric field and auroral X-ray studies. (France. South Mriu, FRG, Japan, UK. USSR and USA) Sac rocket esp.igns are scheduled to orb the follouing measur6cnts: dynsmiu .nd structure of middle amosphere. 03, SOx density, electron density and electron taprature, electron and proton energy spectr=, flux of high eaergy particles dc electric and umtic fields. (Japsn. USSR. USA and others)

Otber Propord Projects :

Fropord cruir by USSR ship along dntarctic act, Lgingradskaya to Iblodeth~ya. Caordiaation vith the W obwrvacioos at ground uatim is most desirable.

Joint oboerr*tioas to uudy the kthAtlantic Ibouly. Oboenations of urglw, electric fields. ion composition and X-rays vill be .chedulcd to be carried out balloons. (Argentina. Brazil. South Afriu arid others)

Projects vhichvauld k coordinated bet- couth md north polar Wbe observations.

The desirability is ctresrd of southern-narthern polar atmosphere cajwrrsons. The coordination with other interrutionai and rutioual W projects in northern polar region such as Winter in Northern Europe Project (UIUE). Global Observations and Studies of Stratospheric Aerosols (COSSb), Cold Arctic Hesopause Froject (CUP) and USSR Arctic llhP obaerrationm, is nw mder consideration.

progr .ad practiul vays for tbe effective coadinrtion of AUA project will be discusrd at SCbP Upper Atmosphere Physics E meeting to be btld in July 1-3. 1982 in Leningrad. J. U. Forbes

Amapbcric tides. oscillations in wteoralogiul f ields occurrint at wbhuronica of 8 solar or Itmar day, caprio a ujar component of middle atrosphere global dyanica. Tbc MtUre of ahospheric tides requires iwestigations and coardirvtion on a global, ahd hence inter- rutiod, aule. purpose of aRlhP is to create an interaction mong obrrvatiomlista,- data analysts, theoreticiros and rodcllers working towards the follwing gals: - To deli=ate the global rrphology of ti&. in the middle atmosphere including taporal and spatial variabiliry on varicus scales;

- To construct models fac the me- .od time variable tides; - To elucidate the .mle of tides in affecting mea winds and temperatures in the riddle atmosphere;

- To eluci&te the role of tides in giving rise to gravity waver and turh~lcncethrough nonlinear cascade and instabiiity processes; and

- To erraim the influence of the w.n wind and taperacure fields on tidal wave propaytion.

The focus for this interaction will be a series of 1-2 week global obrrvatioml upmigna involving gromd-based raote sensing ncthods. The rcchcir for interchage will be vorbhops or symposia dealing apcifiully with the interpretation of these rasuraents. In addition, st.ndardirations of data farutting and analyses will be de- fined to facilitate the exch~geof inforution.

Anticipated intenutioml participation includes:

kruda USSR Jaw India USA France Australia Taivan United Kingdom Peoples Republic of China GDR I taly PRG COLD ARCTIC mSCPAUSE PBWECT (CAW)

L. Bjorn

The project (Cold Arctic ICcscpaume Projcct) proceeds according to plans. The wd active period of observations vjil be July 26 - August 16, 1982 when the rocket cupsign is scheduled at ESEAUGE. Host rocket experiments are built and tested. The rocket indrumentation will contain positive and negative ion mass spectrometers, uuuraeats of total plasma density and ior-'ring radiation, optical instruments for detecL ~f #LC .ad derivation of KLC particle size, and ~casursentof neutr. density and ataic oaygen concentration. It will, further, conta: lliug sphere experiment for derivation of tsperature and wind .no a Li-trail experkst also for wind retrieval. Tbere will be 8 net of ground-bawd measurements, the extent of which is still to be defined. Attapts vill be ude to measure stratospheric and possibly mesospheric density and tslprature (LIDAR) and of IR-sissions with both spectr-ters and interferolcter.

An experkt vill be carried out with EISCAT during this period. All EISCAT rakr countries will participste ad the airs of the experiment will be:

- to detect the upper boundary of the mytive ion reg* - to try to neasure extraely hcmy positive ions - to try to measure D-region electron densities - to measure wave and wind activities.

Th experiment will amplement the ground-based experiunt, and give a picture of the eesopaur region during the period of field measuraents with regard. to neutral and plasma properties. Two aircrdt will be used - oor for wnitoring and photography of ULC and one for -king microwave radiaetry of woospheric B20 and 03.

Finally, utellite data will be urd to the extent it shows possible. Priurily S1Z: data on NO, 03, WLC occurrence and if possible on ALC particle size distribution vill be included in the data. Tbe latrqch criteria for the msin rocket salvo will be the presence of NLC over the launch area snd lw gecrugnetic activity. Monitoring of NLC Photography Microwave Radiaetry (E20, 03) mx-A IAP-B

GROUND BASED

IR Spectrometer UV, HLSU IR Interferometer USU, msu Fabry-Perot Eulon UCL Li&r a. EISCAT UCV, CNET, UIO Meteor Radar US

SATELLITE

SIE No, 0 mc LASP, NCba 3'

S37 (2) Im Crmposition W Clll8 (1 Positive, 1 iiepa::\e) (likeorion) Plasma Density UIO Energetic Electrons U I0 Im Mobility KfSU NLC-Photaneter WSU

SW (2) Gas Density (ArSonde) lILSU (Pikeorion) Gas Density (Xe - Og Sonde) UISU Atomic Oxygen Concentration BAL NLC Particle Size Distribution WSU Gas Tsperature UCW

EAL (1) Atomic Oxygen Concentration BAL (Petrel) Electron Density RAL Gas Temperature UCW

SISAFAH (1) Ion Canposition WI-K (Nike-Orion)

TAD (1) Temperature (Falling Sphere) AFGL (Nike-Orion) Density, Winds. Turbulence Li-Trail UCL

181-K (1) Ion Canposition (Petrel) GLOBAL METEOR OBSERVATION SYSTEM (GLOBST:

R. G. Roper

FOREWORD

The Global Heteor Observation Syetem (GLOBPET)project is a complex progrim of meteor research for the eighties, first proposed by the Soviet Geophysical Committee in 1981. It was discues~dat the IV IAGA Scientific Assembly in Edinburgh in August, 1981, by the UGA Working Group V-2 of IAGA Section V, by the UGA Executive Committee md at the business meeting of the M4P Steering Committee. These discussions resulted in Resolution 9 of IAGA, which recommended, in part, that international cooperation in meteor reeearch be undertaken through a Global Heteor Observation System. The project draft was also discuseed and endorsed by the 111 Scientific Assembly of IMUP in Hamburg in August 1981 (IWResolution No. 1).

Following these recommendations by IAGA and W, the Scientific Committee on Solar-Terrestrial Physics (SCOSTEP) created the GLOBkET Ad Hoc Committee, with representatives from UGA, IW, IW and URSI. The 'omittee was assigned the task of preparing the GLOBMET Planning Document.

This version of the Planning Document was produced after due consideration of several irmendments and proposals by representatives from most major centres of meteor research.

The ad hoc committee charged with its preparation was headed by Dr. B. L. Kascneyev. Members of this committee were Dr. W. G. Elford (IAU), Dr. S. P. Kingsley (URSI), Dr. V. I. Nechitailenko (Secretary), Dr. R. G. Roper (IAGA/IAHAP) and M. Simek (COSPAR).

At the SCOSTEP and MAP Steering Committee meetings in Ottawa in May, 1982, GLdBXT was approved as a MAP project, with R. G. Roper as interim coordinator. The first GLOBMET meeting will be held during the Schwerin, GDR, Symposium on Ground-Bascd Studies of the Middle Atmosphere, May 9-13, 1983

INTRODUCTION

The Global Heteor Observation Project is aimed at intensifying research in Meteor Geophysics and Astronomy in the eighties by making wider use of the latest achievements in this fie:- a~,: expanding inter- national coordination in meteor research.

For many years, the existing global radar network has been successfully providing in£ormation that had proved especially useful in various internationel geophysical projects. The data obtained hae made it possible to datermine the basic characteristics of atmospheric cir- culation and metecrid flux within the 80-110 km height range. Moat of the difficulties associated with data collection, reduction and analyris have been resolved, and the basic parmeters necessary for a viable global observatioael network detarmined.

Howwer, a number of important problems pertaining to the con- struction of adequate models of circulation in the meteor zone and its correlation with the processes ta'.ing pi-ce in the lover atmoapher ic layers remain unsolved.

Only a greater degree of cooperation between existing observatories. and methodical expansion of the global network, including partial reflection drift . asurements, MT radars, rocketsondes and other appropriate techniqu can further our understanding of the dynamics of this region. Wn. e global measurenent of atmospheric paranetere is, in principle, beat done with orbiting satellites, the fcct that current (and proposed) satellite instrumentation does not have adequate height resolution at these altitudes makes a ground-based network our only alternative for the foreseeable future.

Radio meteor data are subject to the influence of various factors of rlelectional, astronomical, equipmental and interpretive nature. Standardization of hardvare, observation techniques and algorithms of interpretation is important in a global progrm.

In most instances, correct interpretation calls for knowledge of the structure of the meteor flux, which cannot be obtained without undertaking a simultaneous meteor astronomy program. Such research will make it possible to ensure a rapid accumulation of the experimental data necessary to resolve problems facing Meteor Geophysics and Astronomy.

The present Project envisages simultaneous theoretical and experimental studies of closely related phenanena, and Gef ines the organization necessary to achieve those ends. The project will continue and expand on the research that has been carried out under the GBMJSP progren and by the IAU/IAGA Special Committee on Radar Observations of Meteor Flux and Radiants and Anomalies at the Base of the Thermosphere.

The main objective of the project is to organize a network of meteor observatories. which will provide experimental data: (1) for testing of models of atmospheric circulation which include the meteor region; (2) on the inf iux of meteors and the distribution 3f meteoroids in the neighborhood of the earth; and (3) for testi~gmodels of neteoroid/atmosphere interaction. THE PRINCIPAL SCIENTIYTC OBJECTIVES OF GLOBNET

(a) In Meteor Geophysics

- To create global models of seasonal changee in basic characteristic: of dynamical processes in the upper me~caphereand lover thermc- sphere, considering not only prevailing winds, planetrry -;aves and tides, brt also i~terealgravity wave; a.~d turbrlen~r.

- To investigate the variation : space and time of atmospheric dynamical processes in the seteor zone and their role in the global circulation at 70-119 km altitude. - TO study the relation between dynamiccll processee In the meteor zone of the atmosphere snd thcse in the other atmospheric layers and betwecn the former and aclar gemagnetic variations.

- To stutiy latitudal-and-seasonal fluctuations in temperature, pressure and density at the mesopause and in the lover thermosphere. - To study the physics of the interaction of meteor- with the Earth's atmosphere and to devise techniques for determini~gatmospheric parmetere using meteor observation results. - To study disturbances in the Middle Atmosphere cau~dby cosmic and man-made bodies.

- To atudy the inf lwnce of large meteoriods on the pollution of the upper and middle atmosphere and the dependenca of dust-producing capacity on the mass and velocity of such meteors.

- To determine the time and Jpace structure of the near-Earth meteor complex.

- To determine the flux cf meteoroids over 10'~~for each month of e gear.

- To determine the radiant distriL-tion of meteoro~dsover 10-~gfor each month of a pear.

- To estimate the flux density of rteteors over 10-4g as a function of the longitude of the Sun for the Quadrantid, Geminid. n-Aquarid and Orionid meteor showers and to study their fine structures. - To study deceleration, ablatioi;, structure and me-hanism of Inter- action with th2 atmosphere of decimetre bodies ac 120-20 km heights. - To carry out complex observation of uteoroids and the atmosphere using radar .od television techniques abined with geophysical rocketsondes.

(c) Applied Tasks of GLOBIET - To create reference model atmosphere for the 70-110 km height range turd on data obtained from an appropriate observatio~lradar net- work, and to umbine than with standard atmosphere models for other heights.

- To construct forecast models of wteorologiul prreters at the mesopause and in the lwer thermosphere using the data obtained by the network of meteor radars and psrtial reflection stations. - To investigate the possible use of reteor radar data for long-tern weather md climate fareustr.

- To study the fine structure of rteor influx in different mass rmqec and to create wtea hazard forecast models.

- To create wdels of radio-vme meteor propagation, and standards and protocols for rttar radar data exchcge using meteor scatter links betwee stations.

The unplex of tasks to be solved by w~lsof a vteor network deteaines essentially the choice of criteria for optimization of both the nctvork proper and the prrreters of the measuring systems. The obwrved meteor flux possesses similar sprce and time scales to the atmospheric circulstion. namely di.~rrul,wasoml and global variations. The mechmia of transformation of the genuine wind f Lsld to the observations obtained by radars contains information not only on the imestigated wind field, but also on the investigated tracer, the latter distorting the wind estimates. This distortion is a function primarily of the radar systa used, although the interpretive algorithms used to deduce the wind field from the measured data un contribute to such distortion. The greatest single contributor to the minimization of this distortion is the earursent of echo arrival angle, and the height of each echo. The mcessity of using inforution on afmocpheric 6aamiul regime erpcially on the height gradients of the vind velocity. for 8 more accurate derivation of the velocity and coordi~teeof individual meteor radiants, calls for the organization of a progra em;harizing both geophysical and astronaiul aspects.

Thus, the basic methodological problas to receive priority of attention under GLOBWT are: (a) To Perfarm a Comparative Analysis of Software and Budware for Ysteor Research

- To analyze the co~patibilityof data on the wind regiw in the meteat zone obtained by the Ecteor radar method and other o~thodn.

- To ana1:rze the influence of a=tronaiol and harbare factors oo the accuracy of wind regir parreters obtained by the radar method.

(b) To Specify the Dependence on Parmeters of the Physical of Mereors as well as on tire rheory of Radio-wave Scatter by the Plasma of a Pkteor Trail in Determining the Selection Effect8 in Hetear Obrervations. Including:

- The study of the interaction of meteor trails with both the neutral atmosphere and the geaugnctic field.

- The study of the influence of irregularities in ionization on radio- wave scattering, and the pheajreru taking place in long-lived trails.

(c) TO Standardize and Cpticize Keteor Radars and lkteor B.&r Uetvak Parmeterr

The meteor radar method is characterized by considerable sensitivity to both the directly registered propertier of a meteor and the psrmeters found using the corresponding interpretation procedurcr. The real distribution of meteor substance in the solar ryrte cannot be observed directly. Is it possible, by studying meteors fram the Earth, to detect variations in the original distribution of meteors? Can these variations be measured by meteor radars? In order to define reasomble dands or the lwel of standardization of vteor radar parmeters it appears necessary to solve another set of probllr:

- To determine &.e lovest threshold variations of the real dis;ribution of meteor parreters belw whict interpetation in rmreaso~ble.

In addition, in interpreting meteor geophysical obsemation data, consideration of astronatical selection factor' is rrceded. This giver rise to the follwing tanks:

- To determine the threshold estivtes of the real meteor parmeterr above which interpretation of geopb-ysiul observation uring the properties of a meteor flux ae a neutral tracer is urreaso~ble.

The carrying out of the proposed GLOBIET observations by vann of a meteor radar network, organizing an effective meteor data exchange and creating data archives naturally calls for wlving a nnber of other problecls defined in the Kmual on Meteor Radar Obrervationa (in preparation). - To define meteor radar chuacteristiu affecting tbt pmrretern of a recorded ulrplex of rtea bodies. mad thor invariant to thew para- wtera, and to conmtruct on this basis a generalized Udar Hetear Ikta Index (P1D-Index).

It#)-Index, a8 it is defined in the Ilmllud on Wcteor P.&r Obmrm* tioos, is a generalized cbuacteriatic of a met of dat. uod as a criterion of cmptibility of sets of data produced by differat types of radar. - To obtain effective estirtes of the hsic prreters of a rtea radar, i.e., the threshold registered radio uwitudc and tbe para- meters of effect~veobserrration area for different regimes of observation and different rteor radars.

- To optimize mettar radar p.rreters in or&r to deduce the original distribution variations fra the astronaiul observation of rctearr. and, to ensure the correct interpretation of geaphysiul okerrrr tions.

- To compile propouls for optirkation of the structure of glohl rteor radar netvork designed to praote the study of dynamic processes in the meteor zone.

(d) Development of Effective Interpretatior~Algorithm to Ensure:

- Obtrining inforution on the rttar activity and the properties of the meteoroid influx from the observation grid provided by meteor wind radars. - Excluding pwudosynoptiul drift observations and other effects connected with varistions in the mettar flux structure from the wind results.

The qourtitative sulyais of thew effects un be done usiw imitation erpcriwntal data obtained by rodeling the vteor as a tracer of the rdiu. l'be experinltsl tat ullr for holding simultamous oboemations of the circulation using various techniques during the well-knm meteor shouerr. - Obtaining correct estimates of radiant ooordiuates while measuring atmospheric disturbances in the meteor zooc.

(e) Wadcling Studies of &tear F'henwna

This requires the developmt of aathaatiul models that include a11 three oonatituentr, i.e., %dimu (atmosphere, its physiul and dynnic char~cteristics).*tracern (uteor flux with account of artronaiul, physiul and geaetric selectivity factors; and "radar" (including selectivity characteristics, observation and processing procedures). Swh models can provide spcifiutions for various ob- servation progrrs. There are three possible approaches to the problm: - A model that gives inforution as to when and hw of ten measurements rust be taken;

- A model wbor output is used for including its data into ieal or hypothetical measuring systas (networks). beof the systs bia8es due to various errors or sampling limitations can then be estiwted;

- A model that combiner both simulated and observed data sirult.neously. Thus, simulated data and observatio~ldata coexist in the dlto produce a -re realistic analysis.

OBSERVAIIOIAL lElXODS AND THE SETflAG UP OF AN OBSERVING WELYORK

(a) Observatio~lHethods - Radar methods of estimating the parmeters of meteor trails (meteor velocities, ionization profiles and inferred masses) position of the reflection point, wteor radiant coordinates md the velocity of meteor trail drift in the atmosphere at 80-110 km heights.

This will constitute the bulk of obeervatio~l&fa under the GLOBtET Calendar. The meteor radar method combines measurments important for both Heteor Geophysics and Astroncmy.

- Optical sethods of meteor observations including photographic, kge- intensifier and TV.

- Partial Reflections Drifts Method (PRD).

Inclusion of the PRD under GLOBWT serves three objectlvrs: (1) it enables a more detailed study of the physics and dyuscics of atPosphere in the meteor zooe, including the study of short-period gravity waves, (2) it will provide further intercomparirons of the two methods. and (3) for several hours around noon, vinds can oe determined dwn to 65 h.

- Recording of meteor activities by receiving distant VBF broadcas:isg stations.

This method enables meteor fluxes to be monitored with simrler equipment and lwer operating expenses.

(b) The GLOBlET Observing ::etwork

The GLOBPET observing network proposes using the following measuring systems:

meteor wind radars, multi-purpor meteor radars, partial reflection radars, meteor and mlid photographic patrols, imageinteasif ier md N qstems, meteor forward scattering radars (prrticularly in the Soviet Union, wbtre uny stations are within forward scatter colluiiution distance of another (other) station(s)).

Ow of the main considerations of GLOBlET is the installation of 8 aetvork of wteor radar observatories which will prwide the best possible eat iutes of the mridioml and zonal profiles of the riddle atmosphere wind field, in addition to recording the distribution of meteor radiants wer the whole celestial sphere.

Om of the major tasks involved in the carrying out of the recommendations adopted by UGA, IdllbP and IbU for eqmndirrg the network is the introduction of additiozml observing systss (statiomry or mobile) It ruch geographical points as would, in combination with the eristing radar aetvork, ensure the necesaary spatial sampling 86 to comply vith the purpose of the drrft Project. Taking into consideration the existing network, the possibilities of participation by IUCG ~ti0~1camittees and existing research institutions, the progress being made in the development of new auto~rticwteor radars (of the fourth generation in particular), the positive experience pined by expeditions (e.g. to the Equator, Arctic and Antarctic) and also that ground-based radars present feuer logistic difficulties than shipborne radars, the following reco~oendationsare made:

(1) Along the 35" meridian. where a group of Soviet radars is already in operation (Obninsk, Kharov, Kazm, Volgograd and Holodezhya) additional radars in the vicinity of the Arctic Circle, the tropics and the Equator;

(2) Along the 135" meridian, with current operation in Khabmvsk, Kyoto and Adelaide, additional radars on the Arctic and Antarctic Circles ;

(3) 75" meridian (Northern Hemisphere). Currently operating are stations in Dushanbe md Frunze. Additional radars should be placed close to 67ON, 50.1 and 23'N;

(4) SO0 parallel. In the neighborhood of this parallel is a group of European observatories as vell as some P.S. meteor radar stations, and a Canadian PRD facility. A worthwhile expansion would be the placing of radars close to 70°E a~d105%. These proposals for expanding the existing radar network hwe taken due account of (I) construction of a regularly operating network of measuring points for reliable verification of global circulation models, (2) distributing measuring points along the meridians and parallels within a half of the radius of correlation of weather systecs that should emble the production of circulation patterns along the 33'E. 135'E meridians and the 50.N parallel.

Up until nw. regular observation in the Southern Hsisphere has bear conducted only in Adelaide. Christchurch and Molodezbnaya. *tear wind and meteor influx observations in Africa and South hriu. especially around the Southern tropic, are of special importance. Such observations, interesting by themselves. will become doubly so when considered in the context of GLOBET.

The installation and operation of facilities in countries lacking the appropriate expertise would require various bi- or multi-lateral research projects. including expeditions to different parts of the globe.

PRINCIPAL RECOHl€NIKTIONS FOR THE GLOEIIET CALENIIAB

The basic criterion for the choice of observation intemals and umpilation of the calendar is to obtain the maximua mount of useful infomation (both geophysical and astronaical) throughout the GLOBIET network.

The total observational interval. as envisaged by the Roject. should last for at least one cycle of solar activity (1980-90). During this period, the greatest priority should be given to the Intensive progrrs during the nxixsrm and ainimua solar activity periods, with special emphasis being given at these times to the deployaent of mbile rabrs. Tk principal limitations to the achieveint of the objectives of GLOBIET is fimncial. Hence the mphasis on the extremes of the solar cycle fa1 ling in this decade. The experience gained by the Swiet Equatorial Meteor Expedition, together with the current circulation models suggest the propoeed twcryear intervals as optimrm for intensive (especially expeditionary) observation, with no less than 8aonth intervals, including both Equinoxes, for observations on the network located parallel to the Equator.

In choosing observational intervals, due consideration must also be given to (1) the geophysical value of the period, (2) the inclusion of other techniques sampling other altitudes, and (3) the feasibility of organizing and urrying out expeditions (possibly ship as well as ground-based) to interesting geographical points. Olrc of the most interesting intervals in the coming years is the second half of the naP obsematioml phase (1984-851. This iaterval should be considered the First Internal of the Highest Priority uader CLomET.

Considering the need for clor coordination of the geophysical p.fi of GLOBBET with IlbP, the GLOBIQT Dymic Calendar should be based on the W qnric Calendar vhich, in its turn, is an adaptation of the Intemtioml Geophysical Calendar to the needs of W.

lk wgested CLOBIET Dynamic Calendar hs be- prepared SO as tc uximke the mount of inforution for all of the proposed tasks, while requiring the minimam roMt of ti* and f\mds, especially in those cars wbcre continuous observation anat be ude. Thus the bulk of obrnatioml data is to be obtained arouad Regular Ccophysiul Days (Pm)) and Regular Uald Days (RUD).

The study of mesospheric dyrumics by mans of rtem radars and otkr techniques should concentrate on the PCDs and PYDr and Priority ms ~POMs).

brideration should also be given to the follaving: since obseming rmr of at least tea days are needed to study planetary waves and tides it is recacnded that such nms be centered on PRWls with Quarterly World Days (QVDs) so as to ensure marina correlation vith rocketsoder .nd incoherent scatter rasur-ents. Several problss un be studied only by wntinuous observations during long periods of time. If continuour obrclv~tionsare not feasible, long period observations rharld k initiated by a mGSTOBW or STPATYARW alert.

The Calendar for Meteor Flux Observation* by Statistical Wethods coincides vith the Ca1end.r for Meteor Trail brift Observations.

Gawral Hetear flux obwrvationc and the study of pseu&synopti~.l effect. should coincide either vith the Calendar of Meteor Shovers which io -pacot prt of the Intermtiom1 Geophysical Calendar or vith the forecast of possible nteur showers associated vith the return of long-period coeets.

The correct interpretation of =tear showers requires consideration of the background; therefore oboemations should be held for 1-2 day before .nd cfter the shover occurs.

Recaended for regular observations are the Quadrantid (Jan. 2-61 md Gahid (kc. 3-17), n-Aquarid (Hay 3-10) and Orionid (Oct. 16-26) rhowers. Tbe former two provide the best opportunity for calibration of mearuring oyctas and the latter coincide with the orbit of Halley's bet. (a) Data Conception

The data neeaed to ensure tbc ampletion of the abovtwntioxed tasks requires haogareity in reduction and a~lysis,md the availability of m adequate global obsenatioml grid of wtea radars. These requiraents can be met adequate regulation of rtrologic and space-and-time characteristics including (1) the stmdardization of measuring system parmeters, algoritbrs and techniques for observation, (2) the structural optimization of the network and (3) the propowd observation calendar.

Realistially, the first uep touards structural and technical ctm&rdization of the edstiog radars should include oaly minim1 demands. This minim involves the mifiation of a11 radar par-eters that ur. be deterrined by their relation to the rteors recorded, md the estimated atlospheric parmeters, i.e., the mini- recorded meteor radio magnitude; the selection chuacteristicl with respect to nxinr and niniru values of velocities md other parreters mder study; heirht resolution; md scanning regi.cns, .nd methods .ad schemes of observation.

These requiraents will be detailed in the Hmrul on Hetear bdar Observation vhich. while making no drastic vtrologiul or other requirements for &ta .rulysis within the GLOBE. ;rmevook, fixer the definitions of: estintes of basic parmeters that rbould be regarded as most desirable for the existing measuring installations, including obserrratioml methods .nd data reduction and interpretation algorithms; spcifiutions for development of new hrdvare and software; and representative foruts md &ta exchmge procedures.

(b) Data Exchmge

In li~ewith the ICSU Cmeral Asscmbly Resolution (1978) concerning dat. exchange for a11 new interdisciplinary ICSU progrms, YIiC-A and VDC-B will be the rdir of international data exchange for GLOBISS.

Within the hierarchy of bta exchmge adopted by the above two centres, the GLOBIEI data falls in the follwing three categories:

The First Level: - average hourly wind velocity estirtes - meteor activity record.. The first level data obtained for each year is to be exchanged uacondicio~llyand transferred to UDCs within six months after the corresponding observation period ends. Hctcor rabr &ta presented to VDCs must mdergo the standard editing, procerriag and a~lytingprocedures recaunded by the Il.llual On lktcar P.&r Okcrvations.

The Second hn&: - individual eotirtes of wind velocity and reflection point coordinate8 - reaults of rasuring physiul properties of meteors and the atmosphere - meteor radiant, orbit and flux density oboervations. The data will be filed in the archives of pnrticipating orynizations and will be mailable upon request. Tbe information on the data in posrerion of these organizations will be wnt periodically to the appropriate UDC to be cataloged.

The Third Level:

- data (such as reports, etc.) assigned to the UDC to be u.cd by visitiog scitntists rather thm disrrhuted to urrs.

The description of data types and forutr as vell as the rount and ti- of presentation of each type of data to the archives is to be found in the Guide to Intenutioasl Data Exchmge (Meteors) and other Wnualt that are to be prepared and agreed upon during the preparatory stage of GUBIEI.

IAGA Remlution lo. 9 Edinburgh. 15.08.81

IKA, noting that moet radar meteor systms are nw autouted, con rider^ the need for a more effective geographical distribution of radar meteor stations and recognizing the high degree of coordi~tion W!CeSSarg to mdertake sirultaneous worldvide observations recollnds that (1) IAGA member countries be encouraged to support and extmd the radio meteor netvork.

(2) internatioo.1 coordination be undertaken through a Global Meteor Obeervation Systs (GLOBST) and that this coordination be effected in the kdiate future through the Middle Atmosphere Progrm in SCOSTEP

(3) a corittee be formed vithin SCOSTEP vith representatives fra UCA. UWAP, IAU and URSI to produce a GLOBHET p18nning docurcn t . IAMAP Resolution No. 1 Haburg, 27.08.81

W,noting WCA resolution concerning the Swiet Geophysical Committees' Global Meteor Observation (GLOB~T)Syrtm propoul passed at the Edinburgh Arsably, Augurt 1981, ad conridering the need for simltmeous vorldvide obremationr of mesopause region dynamics, recoscnds that:

(1) IAUAP member countries be encouraged to support and extend such observations, using all practical techniques and

(2) IlWLP accept the invitation extcnded by IAGA to further this cooperative effort by endorsing a cormittee to be formed within SCOSTEP with representatives Eta SAGA, UWP, UU and URSI to mdertake internationn: coordination through a Global Ueteor Observation (GLOBBET) Syst~. TEE PLANWED ACTIVITIES UNDER GLOBlGT first version of the GLOBMET Project: general, scientific objectives

discussion of the Project, preparation of the Guide to International Data Exchange through the YDCs (meteors) I ! .tie discussion of Project at IAGA and W Assemblies

GLOBET Preparatory Phase (81-82)

preparation of the GLOBUET Project and Manual final version by the GLOBMET Ad Hoc Committee

business meeting of the SCOSTEP Bureau, adoption of the final versions

the phase of analyzing the methodological experiments,

GLOBlT Symposium at IUGG Assembly

the First Observational Phase of the Righest Priority (OPEP)

the analysis of the I period

Symposium (analysis of the 1 period observation results)

?LIP ORSEH\'ATIOSAL PHASE GRAVITY WAVES AND TURBULRJCE IN THE MIDDLE ATBIOSPHERE PROCRAM (GBATIUP )

U. A. Geller

SCIENTIFIC BACKGROUND

The HAP Planning Document briefly addressed the importance of understanding gravity wave and turbulence structure in the middle atmosphere. This was expanded upon later in the MAP Study Group 3 Report on tides, gravity waves, and turbulence. Thus, this section is only a brief update on the discussion in those documents.

Gravity waves and turbulence are intimately related in the middle atmosphere. Gravity wave breaking generates turbulence which in turn limits the gravity wave growth with altitude, when viewicg spectra of the middle atmosphere motions. It is difficult in many cases to clearly distinguish interacting gravity waves from a saturated turbulent medium. What is very clear, however, is that gravity waves and turbulence greatly influence the global middle atmosphere structure. They redistribute momentum. They both redistribute heat and give rise to conversions cf mechanical energy to themal energy, and they also give rise to transport ot minor constituents in the middle atmosphere.

It is the goal of the proposed GRARUP to delineate the global morphology of gravity waves and turbulence in the middle atmosphere including geographical and seasonal variability and to develop physically based parameterizations of the influence of gravity waves and turbulence on middle atmosphere taperature, wind, and constituent structure.

GRAlIIAP AS AN IhTERNATIONAL PUP PROJECT

It is logical that GRARUP be an international MP project for the followiog reusons. The global scale of this project transcends aatioaal boundaries. The different rutions of the world have different areas of expertise to apply to GRATMAP, but no single country possesses all areas of expertise. Internatioaal commmication in such areas as standardization of data analysis procedures and in arranging workshops is required. Since strong interactions among theorists with observationalists and modellers is required to meet the goals of CRAW, and different nations have different strengths in these areas, international cooperation is desired. Finally, an international MAP project will facilitate multi-national, multi-instrument campaigns. It should be noted that such campaigns need not be carried out synchronously around tb - world as is the case for tides due to the seasonal nature of gravity wave and turbulence effects. PROJECT ACTIV ITIES

It is proposed that a steering committee for GRAW be set up initially to plan measurement programs that are aimed at accomplishing the project ' s goals; e.g., determining the morphology of mesoscale gravity vaves and turbulence in the middle atmosphere. They vould determine the required accuracy, spatial (both horizontal and vertical 1, and taaporal resolutions of the measurements. They. or a euccessor group, vould then coordinate the measurement efforts of GRATNAP. Later activities vould then involve looking after the analysis and exchange of data as vell as subsequent archiving of data. It is emphasized that t'nese group8 must include theorists, observstionalists, and modellers to accomplish the GBAW goals.

ANTICIPATED INTERNATIONAL PARTICIPATION

GUTMAP requires the participation of radar, lidar, balloon, rocket, and aircraft experimenters as vell as theorists and modellers. Countries having, or planning, significant efforts in these areas include the follwing: United States, Norvay. Peru, Federal Republic of Germany, German Democratic Republic, Japan, United Kingdom, Australia, New Zealand, India. United Swiet Socialist Republic, Peoples' Republic of China, Taiwan, Canada and France. We anticipate a11 would contribute representatives to GRATW. We envision the steering committee of GRAW to be smaller, hovwer, perhaps six to eight, to facilitate its effective functioning in its planning and coordinating functions. STRATWARM bTSOSPHERIC PROGRAM (SWAMF') (a sub-project of DYNAICCS)

3. Offermann

Stratospheric Warnings are well known as the strongest disturbances in middle atmosphere parameters (as temperature, wind, etc.) during Northern Hemisphere winters. Not too much is known, however, on how these phenomena extend into the higher atmosphere, i.e. the mesosphere and lover thermosphere. Considerable modification of vertical temperature profiles are expected here (see for instance Cole and Ksntor, Air Force Reference Atmosphere, 1978). Vary substantial changes of the wind fields can also occur, as is for instance demonstrated by the recent measurements of Schminder and Kurschner, (Gerlands Beitr. Geophysik, 1, 22, 1981) and the earlier dqta of Gregory and Wanson (J. Atmos. Sci., 32, 1676, 1975). Interesting wave and turbulent activity at mesospheric heights has been observed by the SOUSY-FlST radar during a minor stratospheric banning (Ruster et al., Geophys. Res. Lett., 7, 939, 1980).

It is obvious, that a stratospheric warming and its effects at higner altitudes cannot be determined just by measuring a vertical profile of one atmospheric parameter. This is because during such events many atmospheric parmeters vary in three dimensions sn~in time. It is well known. for instance. that the phase nf the tmperature vave changes with height, resulting in a 180" shift ~etweenthe stratosphere and mesos~i~ere(mesospheric cooling, see for instance Hob, Quart. J. Roy. Met. Soc., 104, 1, 1978). This phase shift has, however, to be carefully monitored because deviations from this rule appear to be possible: During the peak of the recent very strong stratos2heric warming in Jan./Feb. 1981 the mesopause temperatures obtained from OH* emissions were just normal (private comr.unication: G. Lange, K. J.abitzke, J. Barnett). Therefore the phase variation with altitude of this and other atmospheric parameters, and the medium scale horizontal variations inked to it should be a very interesting scientific objective.

There are quite a number of proven techniques available in Europe today, which are able to measure from the ground upper atmosphere ?ammeters which are influenced by a stratospheric warming, e~chas temperature, winds, waves, and turbulence. These include radar, lidar, and other Doppler techniques as well as plasma drift and absorption and airglow seasurenients. Obviously E combined operation 9f such a network of stations for the study of stratospheric warnings/ mesospheric coolings has not yet been trred in Europe. It is therefore suggested that a program of joint winter measurements be started beginnrng in December 198i and extending at least .anti1 spring 1984 (SUM = -Strat~arm bJesospheric zrogrrrm). The operation scheme of the progr would be very simple: the inurmnts should be re~dyfor operation early in Decaber each winter. They should take some referace measurements by that time. Aftervard. they would be kept on stand-by =ti1 a aratwam occurs, ad detailed informations/ recorendations for operations are received by TUX. Stratalert inforu*ionvill be supplied by I. Labitzke. Berlin. After each oboematiom period (in spring or early s-r) a short workshop for data comparison should be held. A by-product of "SWAMP" might be the development of an improved alert -heme for the rocket launches of the upcooing W/WIHE Clpaign (winter i983/%4;.

A lie of ground-hoed stations with possible interest in participation in SWbKP is attached. The responee from rxperimenters contacted wa8 very positive. Cacnts and suggestions for the progra. itr =ope, duration, organization, etc.. are welcome. - -- Meteor Radar Shef f ield 1Eul ler, Kinsley . Akrdecn Univ. SScffield

Felloua, CUET, Paris

Cevolani. CWB, Bolotpu

Taubenheir. BBI, Berlin

Putial Ref lec- tion Radar

Incoheret Wind St. Sacitin Sutter Radar Tsperature

Incoherent Wind Thane, IDRE, Xjeller Sutter radar Temperature Kohl, 181, Lindau

Kind Bottger et 81.. Turbulence 181 Lindau

EF-CU Doppler Leicester T. I. Jcmer, Univ. (hfjord?) Leicerter

LF ion drift W ind Col lm Schinder . Oniv . Lei pz ig

De Bilt Veerur. De Bilt

10 kHz re- Tromso (?) f lection height

1. B. Jones, Univ. Leicester

Volland. Univ. Bonn

Ionosonoe f Dickinson, Rutherf ord min Network and Appleton Lab.

61, A3 11: Lindau Schueotek. WI Lindau absorption

Taubenheim, HHI Berlin Friedrich. Univ. Grat u,A3 l.2 absorption n n De Bilt Vesuur, uRa. k Bilt

n n n Akrystvyth E. R. Villi~s, UC Vales

Density, Temperature

v. Z.hn. Unir. Bonn

Fabry-Perot, Tsprature, Beer. UC London 5577 A V in$

it. V. Smith, Ulster College

airglw 0. RO, 08' G. Uitt. Univ, spectrometer Stockholm

airglw 0 Lauche. WI Lindau pbotaeter

IR spectrometer Temperature. imge, Univ. Vuppertal oat, o,(- l:.) Bunett, Univ. Oxford

Ber 1in Labittke. RI Berlin

Partial Wind A. Wwn, J. Gregcry. Reflection Univ. Saskatchewan Radar SYNOPTIC OZORE WS*

A. D. Belront

Ozone is one of the major parretern in the radiation balance of the riddle atmsphere. In recent years it has become possible to obtain hlobal uasur~entsof total ozone, its vertical distribution fra about '5 to 50 h, and with recent techniques to obtain prof ilea fra 10 to 30 m using total ozone and wteorologial pmreters. The riddle atmosphere is the region in which most ozotr is found. All models of the middle atmosphere rust mnsider the vrriatioas in otoac. Uitbout ozone there would likely not be a wan layer of the atmosphere which we all stratosphere. Detailed obse~atiomlstudies in four dirasions vill provide a basic frrevork to help develop dynamic models of the riddle atmosphere.

Prelirirury techniques for preparing lower stratosphere profiles have bem discussed, mat recently, at the Ozone Spposiu at Boulder in 1980. Thew techniques cm be greatly improved if ozolusode. total ozone, and radiosonde profiles can a11 be taken within a few hours. One of the present difficulties is that regressions of thew data are not corpletely valid because the data are taken at widely differat tius. A remedy would be to organize a otwork of ozonesonde uationc which vould take their obse~ationsmar the tir of 88tellite werp.Ss, as vell as being near aorul radiownde observation tirs. As radiowndes are taken at 00 rod 12 Greenwich and limbus satellites take their obaemations near local noon, the longitudes within about 45' of Greenwich md of 180. would be nost suitable. Tbcw vould include all of Europe and the Western USSR, wst of Afriu. and Japan, Australia md Alaska as regions fravhich regression data could be capiled. There are other utellita which observe total ozone and which hedifferent observation tira vhich may be convenient observation tirs for other localities.

Intematioml cooperation will be required to establish thew coordinated observations, both for the purpsr of establishing improved regressions in the early phases of the project md later to aerve as ground truth with which to verify the ups produced to verify the- regressions.

The preparation of daily synoptic maps at selected altitudes, which could include the years since 1970 is too large a project for a single group. Furthera~re,regressions can be developed independently by several groups using different tecbniques. From these the best could be aelectad for application to uppreparation. Thus, scientific collaboration is esrntial.

*Proposed at Ottawa MPSC meeting. The final results of the derived ozone fields vill be the basis of a three-dkensional climatology which will not only describe the changes in ozone globally. but can serve both as input and verification for the uny different middle atmospheric dynamic models which are currently being prepared.

In a preliminary manner this proposal was introduced at L'rbana ard Hau~burg. It is now being proposed more formally, having received indications of interest from scientists in other ccuntries. as a FAP project . WINTER IN NORTHEW EUROPE (WINE) PROJECT

U. von zahn

HAP SCIENTIFIC GOALS

The middle atmosphere is comprised mainly of the stratosphere and mesosphere. and is the region of the atmosphere about which ve knw the least. The reasons are partly the coop!exity of the physical procesres and partly the inaccessibility of the region to satellite investiga- tions. It is the region where tvo strong energy sources interact: solar ultraviolet light absorbed by the atmosphere to give chemically active constituents. and wave motions forced from the troposphere into the stratosphere and mesosphere.

The major aim of the Uiddle Atmosphere Progrr will be the develop rnent of an adequate description and understanding of the middle atmosphere, from altitudes of about 10 to 100 h, particularly in relation of the global fields of: (a) density, pressure and t-perature; (b) composition; (c) lotion (on all scales); and (dl the interact ion between these fields. The progra vil 1 require observations which are both intensive. so that interactions may be determined. and extensive. so that the global picture is complete. Theoretical models will be required, and thee must be adequate to describe both dyuaiul and aeronomic aspects of the middle atmosphere. Since both the troposphere belw and the thermosphere above influence the stratosphere and mesosphere, middle atmosphere research must be conducted with regard to the study of the former regions, both in respect to theory and to observational progras. Also, it will be necessary to consider a11 physical and cheutical prOCeSSeS in the light of signifiunt tiw and space scales, including those appropriate to climatic chmge for which long-term observations may be necessnry.

ORGANIZATION OF IW

W is being sponsored by several international scientific bodies vhose disciplines are related to the science of the middle atmosphere:

World Ueteorological Organization (M)

International Union of Radio Science (URSI)

Internations 1 Association of Ueteorology and (IIUUP) Atmospheric Physics

Internatiour? Association of Geomagnetisa ( IAGA) and Aeronomy

Committee on Space Research (COSPAR) Inter-Union Comisaion on Xadio lkteorology (IUcM)

Scientific Camittee on Solar-Terrestrial Physiu

During its 17th General Assably in Septsber 1978 the Internatiolul Council of Scientific Unions (ICSD) officially approved HAP as a major intenmtional cooperative research progrr.

llbP is nov carried out mder the auspices of the Scientific Camittee on Solar-Terrestr ial Physics (SCOSTEP) . Planning and coor- dination of naP activities is pcrforrcd by an intenmtiooal HAP Steering Camittee (naPSC), which is presently chaired by Prof. S. Bwhill (University of Illinois, Urbana, IL US). Specific I(bP projects are to be propowd by individual scientists or research institutions for atdoroematt by che UAPSC and aQption as an official llhP project. Funding to carry out thew projects has to une. hovever, from the natiorvl sgmcies involved in the respective research progrms.

Planning and coordination of the German UAP activities is performed by the Caaission of Ahospheric Sciences of the Deutsche Forschmgsgcreinsch.ft (DFG). The Gaun representative for HAP is presently Prof. U. von Z.hn (Physilulisches Institut, Universitat Bcmn, 12, lurnllee, 5300 Bomn 1. PBG).

SCEEmLE OF ACTIVITIES

The years 1979 to 1981 were designated 8 'Pre-MP' interval in which a oum3cr of special research projects (PWPs) have ken carried out and lllV Study Groups (lSGs) were wt up. The major observational progrrs of UAP are pcrforred in the period January 1st. 1982 to Decsber 31st. 1985, f ollwed by an analysis phase of about 2 years. In addition, the WSC is currently considering a second phase of HAP to take advantage of experiunts scheduled after 1985.

mF I(AP PBOJEm 'V~EPrn NOKl'EERN EUROPE (tW/wrnE)'

(a) HAF'/VIlGE Scientific Aims

During winter at high latitudes the structural paroeters of and the dy-ic processes acting in the middle atmosphere display a strong variability, in contrast to fairly steady conditions during summertime. hch of this variability during the winter season can be interpreted as being due to an enhanced level of wave activity on a very wide range of spatial and temporal rcalee. A well-lmovn e-ple of this variability is the occurrence of sudden stratospheric warnings. The causes for the enhanced wave activity, however, are not we1 1 understood. Furthermore, observational data on conditions in the winter mesosphere are rather scarce. In order to get a deeper insight into the causes and effects of this winter variability one needs to measure as completely as possible the structural parmeters of the middle dtmosphere (pressure, temperature) and the dyaaaical processes of global scales (planetary waves, tides), wsoscales (gravity waves, jet strees) and mall scales (turbulence).

For many years meteorological satellite data have provided important information on global scale processes. The more recent development of ST radars, lidar sounders, and sophiatiuted rocket- borne density measuring devices make it now possible to measure at least at selected sites also the mall scale and mesoscale dynamic procesws on an almost continuous basis. Furthermore, special high altitude radiosondes, meteorological rockets. wteorvind radars, and sounding rockets cm provide for additional and vital data which are not routinely wailable from UKI observations or remote sensing satellite experiments.

Hence during a full winter season a coordinated and international study will be performed of the structure, motions, and composition of the middle atmosphere betveen about 50° and 70° northern latitudes. The northern Europe sector is considered particularly well suited for this study because the stratospheric polar vortex is usually shifted in the European sector of the Arctic. Therefore the stratospheric jet flowing southward of the polar vortex is located over Scandinavia, In addition within this sector the disturbances of the middle atmosphere during sudden stratospheric warnings appear to be most intense due to the prevailing tropospheric circulation being blocked by a high pressure system in the North Atlantic region.

The project HAP/WINE is directed toward a better understanding of

- the interaction of planetary waves of tropospheric origin with the mean flow in the stratosphere and mesosphere, - the temporal and spatial development of sudden stratospheric warnings including the pre-warming conditions and the trigger mechanism for the warning.

- the temporal and spatial development of mesospheric cooling events in conjunction with stratospheric warnings,

- the vertical and horizontal transport of minor constituents like trace gases, excited species, and charged particles,

- the effects on the chemistry of neutral and charged species of the large temperature changes occurring during stratospheric warnings and mesospheric coolings, - sources of turbulent energy in the mesosphere and turbopause region, - the taporal and spatial development of turbulent layers, and - the contributions of dynamic81 proceraes to the heating and cooling of the resospheric and turbopaurc region.

A list of ahospheric paraeters to be measured during the MF'IWINE project, as well as their altitude range m: location of observation is attached 86 an appendix.

(b) Organization of MAP/WINE

The project IfAPIWINE was originally propomd to the WSC by the Carrission of Atmospheric Sciences of the Dl%. It was forully approved as part of the international HAP effort by the MAPSC during its meeting in August 1980. Dr. D. Krankowsky has been the initial intenutioual project coordinator. He is now succeeded in this job by Dr. U. von Zahn (University of Ban, Bonn. FRG). An internatioual MIWINE Working Group has been set up which is responsible for planning and coordinating the specific research activities to be performed during the W/WIIIE project. The following members of the Working Gmup have been nominated so far:

Dr. U.-L. Chanin, Serv. dlAeronmie du CNRS France Dr. D. Krankowsky, 181;-K FRG Dr. R. Philbrick, AF Geophysics Laboratory United States Dr. E. Thrane, NDRE Norvay Dr. E. Williams, Univ. College of Wales United Kingdom Dr. G. Vitt, Univ. Stockkolm Sweden Dr. U. von Zahn (chaiwan) , Univ. Bonn FRG

(c) Workplan for HAPIWINE

The project W/UIRE will ceilter on the study of the middle atmosphere during the winter 1983164. The observations will concen- trate on liorthern Europe from about 50°N to 70DN. As MAP/WINE is performed within the scope of the international )ULP progran it should be possible for data collection to make maximum use of existing meteorological and geophysical facilities in many countries. This shall allw the investigation of phencmena of both mall and large scales (up to hemispheric). Observing methods will include

- ground-based facilities, - airplane-borne, balloon-borne, and rocket-borne experiments, - renote sensing techniques from satellites. The project IUPIWINE is to proceed in three phases:

1. Preparatory phase :

- Some new experi-nt techniques have to be developed or be made operatiom1 in northern Europe (e.g. parachute-borne mass spectro- meters, lidar sounding of stratospheric and mesospheric parmeters). - Ground-based facilities (e.g. ST radars, partial reflection stations, ionosondes, rirrmeters, apectrocneters md photrmeters, ozone sounding stations) have to be installed in suitable areas. - Appropriate progrrms for processing and analyais of the data from meteorological rockets, balloon-, rocket-, and utelliteexperinents have to be prepared.

- Theoretical models of c:~e proceasts acting in the middle atmosphere and the respone of the structural parmeters to various forcing fmctions have to be set up, e.g. for large scale dynamics, gravity waves, turbulence, and photocheaiul procesecs.

2. Observational phase :

- Remote sensing data acquisition by ground-based and satellite obsenrations during the winter 1983184 (approx. Nwember 1983 to March 1984) allowing the description of the general etatua and development of the middle atmosphere. By participation of many internationnl groups these observations will cover the area of high latitudes over the whole Northern Hemisphere. Suitable reote sensing satellites are: Solar Uesosphere Explorer, W-E/F, DHSP 5D, Dynamics Explorer. - In-situ measurements of middle atmosphere parmeters by means of special lletbcket lamchings. At least 3 sites north of 55'N are desired and the follouing locations have been selected:

Andoya (approved) 69'N / ldOE Lista (approved) 58"N / 7'E Thule (under consideration) 77'N / 6g0W

Datasonde lamchings are to take place once a veek from each station in the time period November 1, 1983 through brch 15, 1984. Additional launchings are planned in use of the occurrence of a stratospheric warning. In addition Robinsphere launchings are to take place once a veek frw the AnJoya Rocket huge in the time period Nwtmber 1, 1983 through March 15, 1984 with an intensified launch schedule in case of the occurrence of a stratospheric warning. Besides these soundings especially performed for MPIWINE supporting data are expected from regular HetRockets launchingo from the follwing sites:

Primrose Lake 5S0N / llOOW Poker Flat 65-N / 141°W Shemy a 53-N / 175-E Heir7 Island 81'N / 58'5 - Intensive field crmpaigns as the kernel of the IUP/YINE project will be performed in December 1983 and in Jmuary/Februry 1984. I~situ measuranents of structural, dyuamical, and chemical parmeters ~f the stratosphere and mesosphere will be performed with the aid of balloons and rockets which are to be launched from aeveral places in northern Europe (see Table 1).

3. Data processing and analysis phase.

W/WINE CONTRIBUTIONS FROM TEE FEDERAL REPUBLIC OF GERMANS

In late 1980 the Deutsche Forschtmgsgeneinuchaft (Dm) approved special funding for MAP activities. More specifically for WIWINE the DFG vill support :

- t3eoretic.l studies and model development (5 projects approved no far),

- the installation and operation of new ground stations in northern Europe for remote sensing measurements of the middle atmosphere (3 projects approved so far: lST radar, IR spectrometer/ photcrmeter, sodium lidar for temperature measurements in mesopause region).

- analysis of data obtained from US remote sensing satellites.

In early 1981 the Bundesministerium fur For schmg und Technologie (BlQT) has a[ !d to fmd thow German investigations required for MAPIWINE whicn can only be performed by sounding rockets. These resources will be administered by the Deutsche Forschmgs- und Versuch~nstaltfur Luft- und R:~fshrt e.V. (DWLR), Bereich fur Projekt-Tragerschdten (BPT). There will be both purely German payloads as well as payloads comprised of an international complement of instrument. Table 1 gives an overview about the current planning status of the sounding rocket activities.

W/WINE CONTRIBUTIONS FROM NOWAY

In a meeting on Hay 19, 1981 the Norwegian Space Research Committee approved Norwegian scientists participation in lounding rocket . experiments for blAP/WINE as given in Table 1. Furthermore, NTNF is actively studying the possibility of installing a MetRocket launching site at the southern tip of Norvay for regular NetRocket firings during the IW/WINE winter.

Ground-based mearurements : - Routine optical and radio measurements by Tromso University, - Monitoring of the mesospherelionospheric Jbregion by means of the KF partial reflection radar operated by Tromso University (turbulence. electron densities),

- Possible use of EISCAT for mesospheric studies. - MAP vill be supported by the routine observations of the Norwegian Meteorological Office.

WIWINE CONTRIBUTIONS FROM FRANCE

The Middle Atmosphere Working Group of CNRS has approved a progrim of ground-based observations for MAPIWINE in the Tromso area using the following instruments : + ++ - Michelson intelferometer for monitoring of OH , Na , 0 , tempera- ture from linewidth, and winds from Doppler shifts.

- tunable, xarrov band lidar for density and temperature measurements from about 10 to 100 km altitude, - photweters for airglov emissions, - all sky camera. In addition, the inetallation of a French meteor wind radar station in northern Scandiuavia is under consideration.

The ground-based observations at the Observatoire de Haute Provence (M0N/6 "E) vil 1 continue and may serve as reference measursnents for midlatitude conditions.

MAPIWINE CONTRIBUTIONS FROM THE UNITED KINGDOM

The University of Sheffield will participate in MAPIWINE by absenting "meteor winds" continuously throughout the winter 1983181 from tvo stations:

Shef f ield looking NW and NE Aber deen looking SW and SE The station at Sheffield is already in operation and installation of the Aberdeen station is in progress nou.

UAPIWINE CONTRIBUPTONS FRO;! ME UNITED STATES

Various contributions from the U.S. are currently under consideration. They range from the launching8 of MetRockets and participation in sounding rocket experiments (see Table 1) t: the con- tribution of data from remote sensing satellites.

UAP/WXNE CONTRIBUTIONS FROM AUSTRIA

The Technical University Graz will perform electron density measurenents on each of the eight M-T payloads through ground-based observations of the Faraday rotation at three frequencies, emitted from the k+T payloads.

MP/UINE CONTRIBUTIONS FROM THE GWDEMOCRATIC REPUBLIC

The Central Institute of Solar-Terrestr ial Physics and the Geophysical Observatory Colh vill perform upper mesosphere/lover thermosphere wind measurements, using the meteor radar technique and spaced-receiver 1.f method, respectively.

UAP/WINE CONTRIBUTIONS FROM CANADA

The University of Saskatoon will perf om near zontinuous measurements of vinds in the 60 to 100 km altitude region using Saakatoon HF radar. Table 1: HAP/WIhE rocket mounding. (Abbreviations: ree helow) ------. --.---- - .------"- --- ry1na.l M-ll I-I WS N-Y I(.c kQ Mi .*$#nrltnn (rlro$koIr) ----..--.- ----. ---.------ncdcur 01 rW .ant* ,*utrun re, Irrud *nnl ifrl) eon8 Lnrl tnlirrl tmt lml rant Lral au#a.~tr* sr~ml.4 rvlnad US y~111~1p~lin8nsu,wsl*J . . ." - - .-A -"------. --.- tn.lfuw~~~sIsb8n I III I t"I In ~pvrlrn- I #II I rhrfl bnon* 11 l.rrt1wl.1. splwl r ..tnJ. * rlrhlr. 8UcArl llllBMHX, rlrr hrno YDS YI8uI.I 0 sedr 0 re*-• I*. .~d ~~IIICI~,~~IRI, sp*r~r.rtarr r*.tm~.r. Jal. c.rdion praL.. srwuo prael~lrn prtlrl. rmualer. 8rndr. 1af.1.v .nlmnr. f~llLn# k p.k. .))*I.. ------. ------. . .. .--A ------*- ---.------+-. *------.mnlfl..i b . It% L. I,* (I 0 I,VS b 111 1'1 ronll~bulbnfi I0 pa, l6.ad - -" -.-. -A -- - .** .-.. -. ------" " ----.------m - -- ! 8 2 2 &I IU I w ...... *.------.--- ".- ----"- --- -.--.---- - 5~e.1 Lnb L~hrortun Ioraranl Orlm YI~. Ofl~n k*.r Lub~ b*A Taurus orlr -__._._ ____- " - -_ _. .,.* .--- 1"11.- .--- - .------ll'"ll-.lll-l , *~r** IUD bm I30 lu 180 ha ?$ lu IW bm IW hm ?% b~ 110 hn .___ -. -- "" --1.-1-- l---..lllp-l-i.LI- "-- -I.I I----- Irum h AIR LIS~J lhule MI t SI 111 UU Ma UI UI 811- lurrav Wofrrv o.enl.d 11-1- .1 --me--- _-I-_. I. -_. _ "-. -.--.. _ ---.----.------* Cmna. 1CWl8l.i .crv.~-crlel narrrvllnl 11 p!rl.rlrr ~Ysln A lr~lltl Wu1T1 . Lnn mtiv*r~i~v#re naltavt 1.1 lurbrl*nc~and (. Id. Wpubllr 01 mwnv lurh.*p*uw Inve.1 I, ?Ii.116 I bf~8v IQIUI .~bn urn sprcr.rlrr (rrvcr~lrll US Llnlt.4 Blrcr~bl Irrier All. M&vr bCb*t Ran@* tSI .I~rann?

V,,ur M-1 patlr&lr vtll 1614 latn Ih. WWnl in~lrurnl,W law rlll rmlrln Ik. 1WMS ~IIDIIWII List of acmospberic parwters to be runred during the wIYm project. w. 5 r-:n 1 - -r- 1 er - a.- 5 -; I. .-.l 7~1.':t.. 41% i=ar* * '.,:, %O (w.pur.;r! A . I.- -' f . . -- *Rb * 1~ I me- aria !.ST~:- .. I , L.f 2- I'3IL.Ut.r w , L' --11cI1. # 6.p rt r.1 r; - -r.i La;:. .d 7- :-:s . c r.6.t irm' 62-w rlr.rrr cirltr t:txru- i 1

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be S)C 1 - 1 ~l.1 m CZECHOSLOVAK ACTIVITY IN HAP

J. Lastwicka

The Czechoslwak nrtiolul MP progrr consists of 7 scientific sub-progras. One of thea has bem preliminarily approved as a I(AP project :

Disturhnces of the Atmosphere at Eeights of 120 to 40 h by Penetration of llcrtoriods of Metre sad Deciwtre Dieasions - Dr. Ceplecha (Astronaica; Institute, Czech. Acad. Sci ., Oadrejw) : Regular observations at 18 station6 in Czecbo8lwaki.8, 23 stations in FRC, 6 stations in Holland and 2 stations in Aurtri.8 yielded multistation records of 12 wteoroids in the f irst three months of 1982. Fwr meteoroids penetrated the vbole middle acrosphere. These observations are coordinated md evaluated by the Astronaical Institute in Olrdrejov.

The evtheoretical concept of the paetration of nteoroida through a general model of abospheric density could provide inuantaaeaus valws of ahospheric density, particularly at 70-40 b. The influence of the earliet neglected devi.8tions of inatstaneous amorpheric density frcn the rode? density rttaies several kiltmeters along the path, vhich is much rrre than the uncertainty in photographic ob.crvations. This ukes a realistic deterrimtion of instantroeaus dcnsity profiles possible.

Other sub-progras:

Winter Anomaly - Dr. hstovicl. (Ccophysiul Institute, Czech. Aud. Sci., Prague): On the basis of 22 years of A3 absorption measurcs~entsat the P.11.L. Ves Observatory. the ujor stratospheric waaings and related chcger in the prevailing zorvl wind in the upper mesopauw region have bem found to decrease rather than increase the radio-wave absorption. Tk PUP-1 vinterr of 1978179 and 1980/81 have heen fadtypical vinters with a well-developed winter auauly. The winter of 1981/82 is strongly "cont.riolted" by extreme geougnetic activity. The vinter of 1979/81 displays the most exceptiorvl pattern of the vbole 22-year period studied, partly due to the distribution of the geaugnetic activity and stratwan-ro~lwind ef fects.

Acronaic Studies with the Ur of Ground-Based Ibsuraents of Radio-Wave Propagation - Dr. Lutooict (Geophysical Institute, Czech. dud. Sci., Prague): As input data, the AE-E satellite Lyman-alpha reasurmcnts were corrected and the role of X-rays and Lyman-alpha radiation in the 1539 Uz radiarme absorption vaa aswswd.

The Interpl~etaryHngnetic Field Effects in the Iaaosphere mid Amospkre - Dr. kstovicka (Geophysical Institute, Czech. Aud. Sci., Prague): The effect of the IMF sector boundary crossings in the aid- latitude lwer ionosphae lus be- found to be raso~llyand diurnally depcndeut. It is of geaugnetic type at night, of tropospheric type ao the winter day, and ue observe no effect on the equinoctial day.

The Geougnctic Activity Influence on the Troposphere, Clinte and Yeather - Dr. Bucha (Geophysical Inotitute. Czech. Aod. Sci., Prague): The best correlation (correlation coefficient 0.65) betuee the getmagnetic activity and the atrosphcric pressure at the 500 =bar level has bean found over the northern auroral oval in sat selected periods. rtre geaagnetic activity wnes in fact as an indiutm of psrticle penetration, vhich is responsible for the observed effects. The periods uader study aut be carefully elected to rupprur possible werlappiag by intern81 rcteorologiul effects (filtering of the Possby vmea etc.

Airglw Variations - Dr. Rybanaky (Astronaiul Institute, Slovak Aud. Sci.. 1atrm.L. mica): A photouter working in laboratory conditions is being tested now. Catinwus observations are expected to begin in the autumn of 1982.

The Vymaica of Pactration of hvective Cloud. icto the Strato- sphere - Lr. Podtiorsky (Eydronteorologiul Institute, Bratislava): The prirry radar data on radic echoes fra upper boundaries of the cmr;lonirbus type clouds penetrating into the stratosphere vere cralumted. The relative occurrence of thew penetrations was computed for Ccntral Europe with respect to orograph? and airlines. 4 hypothesis was developed on the relation betve~increasing occurrence of ctmulonilbus putration into the stratosphere and uin airlines crossings in Central Europe; in other word., on the influence of tropopaur-region contoination (by jet plme~)on the curulonidus development above the level of spontautmeous crystallization.

In surrry it rybe mid that a11 the Czechoslovak MP sub-progrrs are under way and making god progress. MAP ACTIVITIES IN ME FEDERAL REPUBLIC OF GERMNY

U. von Zahn

UAP research activities in the Federal Republic of Germany are focused on two intenmtiounl MAP projects:

WINTER IN NOIWERN EUROPE (Urn)

The uin scientific aims of the WINE project are the exploration of the structure ad dyrumics of the wintertime mesosphere and stratosphere over northern Europe. In addition, the neutral and ion chemistry of the middle atmosphere will be studied emphasizing the investigation of those constituents which measureents yield supplementary informtion on transport processes acting in the middle atmosphere. The observations will be gathered during the winter period November 1983 to Harch 1984 and shall cover the more regular winter conditions in Nwember/Decaber, as well as the generally disturbed period from January through brch. Obsen ing nethods will include ground-based and satelliteborne remote sensing techniques. and in situ oeasurePents by balloon-borne and rocket-: rne experiments.

The WINE project is sponsored by a herof European countries. the US and Canada. An internatioaal ?UP/WINE Steering Cmmittee has been set up, so far consisting of C'. von Zahn (FRG; chairran), K.-L. Chanin (France), D. Krankovsky (FRG). R. Philbrick (US). E. Thrme (Nomay), E. Willims (UR), and G. Witt (Sweden). The former coor- dinator of the WINE project, D. Krankowsky (Max-Planck-Institute for Nuclear Research, FRG) resigned frm his pcsition in Harch 1982. His successor is U. von Zahn (University of Bonn, FRG). A more detailed description of the project WINE is available as 2 separate document.

GLOBAL BL'DGEI OF STRATOSPHERIC TRACE CONSTITL'EXTS (GLOBUS)

Two integrated cmpaigns of various experiaental techniques are presently discussed concentrating on two specific objectives of the MA?/GLOBUS project:

- Cooparative and complementary measurements of stratospheric trace gases. The aim is to check on the accuracy of the various experi- wntal techniques. determine the natural variability of the trace gases, and, if possibie, determine the tine scale of this variability. It is presently being investigated whether or not this cmpaign could take place in Aire-sur-llAdour in 1983.

- lleraurerrents of latitudillal distribution of stratospheric trace gases. The aie is to perform near simultaneous balloon flights at low, medium and high latitudes. Flights from equatorial sites, Palestine. adCanada/~lar& are being diecused to be performed in 1984.

laboratory experiments, model activities, and the prepration of ground-based experbents are well under way.

The coordinator of this project, Y. Seiler (Il.rP1anck-Institute for Chemistry, FRG), resigned frcm his position early in April 1982. Bis job was taken wer by D. Offeruns (Wuppert.1 University, PPG). A steering commit tee for M/GMBUS is presently being formed. Mmbers so far are D. Offelunn (FUG), H. Ackerran (~elgiu),J. E. Buries ([IIC). and U. Schridt (FBC).

Planning md coordination of the Gerun naP activities is perforred by the C-ission af Atmospheric Sciences of the Deutsche Forschrmgsgaein.cha€t (Dl%). The Gmnrepresentative for is presently U. von Zahn.

Our activitien in the UhP projects WRE and GLOBUS have received special furding fra the Deutsche Forschrmgsgaeinuhaft (DRG) and the Bundesrinisteriu fur Forschtmg und Iechnologie (Dm). A total of 27 individual research projects have been fmded, each contributing touardn the scientific aims of either WINE or GLOBUS, or to both. The latter applies in particular to efforts towards imprwed models of the riddle atmosphere. Of the approved projects four are laboratory studies of photochemical reactions ad of questions concerning the technique of grab smpliag, nine involve in aitu reasureents and eight reote sensing measurements of middle atmosphere parreters, and six are aimed at improved theoretical and mpiriul models of the middle atmosphere.

On February 24 and 25. 1982 the progress and a feu initial results of our HAP activities vere rwieved in a well-attended vorlrshop in Bonn-Bad Codesberg, vhich vas sponsored by the DFC. MP ACTIVITIES IN FINLAND

Finland has no special HAP-progrm, but the follwing works going on or planned may be of sme importance for the intermtiom1 Uiddle Atmosphere Progra.

1. The incoherent scatter facility EISCAT started observations in 1981 and will be in operation for several years recording different prreters in the ionosphere, also its lw levels.

2. Lwer iwels of the ionosphere are monitored continuously using a chain of rimeters in Finland. One station is situated in Spetsbergen.

3. A chain of magnetmeterr will be installod in Finland and Norway in September 1982 to monitor the electric currents in the ionosphere.

4. A vthod has bem developed to use all-sky photographs for the deteminrtion of the altitude of auroral arcs and thus the pene- tration of auroral particles into the atmosphere.

5. Studies of ahospheric electricity and its relations to ionospheric phmmeru have be5 started.

The national contact for MAP-activities in Finland is the Finnish National Committee of XUGG, address:

Finnish Natioml -it tee of Geodesy and Geophysics c/o Finnish kteorological Institute Postbox 503, SF-00101 Helsinki FIWD THE HAP PROGRAH IN FRANCE

)I.-L. Chanin

The French W progra has also been described in detail: in Handbook for NAP Volume 1, the list of the terns involved and the description of the main topics of research and the means existing or in development were given. The organization put in place to allow the realization of the national prograpl was described in Voluee 2 of Handbook for MAP.

The main scientific themes of this progrm are: the variability of stratospheric minor constituents; the stratospheric-tropospheric transport; and the middle atmosphere dynamics. Each of these topics either has already been the object of a successf ul action or is being planned for action in the near future. Let us mention briefly:

- the canpaign of ozore intercomparison using conjugate ground-based, balloon and satellite observations involving about 10 different techniques. Two workshops were held to present and discuss the data. After the release of the definite results this surprper, decision on a new cmpaign in 1983 is Likely to be made.

- An intensive study of Dynamics: planetary vaves, tides, gravity waves, and turbulence has already started using radar, lidar, balloon- borne anemmeter, photmetry and star scintillation techniques. Several projects are planned in the next few months: Intercomparison of NOx measuraent techniques with NASA; latitudinal variability of stratospheric constituents - project STRATOZ; and a study of strato- spheric minor constituents at tropical latitudes by balloon-borne IR spectroscopy.

- A series of long-life balloons (K.I.R.) in the Southern llemisphere to study radiative budget, dynamics and water vapor content is planned for the end of 1982 and it is hoped to be the start of an important HAP Progrmn.

In parallel with those national activities should be mentioned the participation in internatiounl progrms, PHP-1 (recently renamed DYNXNICS),CAW, WINE. and GLOBUS.

This report is not meant to be exhaustive and doesn't mention long-term developments which will be reported at a future meeting. HAP ACTIVITIES IN THE GERHAN DEWCRATIC REPUBLIC

Stud!-r? of the middle atmosphere in the GDR are carr..ed out by

ZISTP : Central Institute of SolarTerrestrial Physics (Eeinrich Hertz Institute) of the Academy of Sciences of the GDR

GOC: Geophysical Observatory Colh of the Karl llux Universit y Leipz ig

Coordinator of the MP activities is Prof. Dr. J. Taubenheint, ZISTP, DDR-1199 Berlin-Adlershof. GDR.

During the entire MP period, the existing ground-based observatiouml programes will be continuourly maintained for the monitoring of: radar meteor winds at Kuhlungsborn (ZISTP. Prof. K. Sprenger 1; ionospheric drifts by spaced-receiver IF method at Collm (COC, Dr. R. Schminder); and ciuracteristica of the D region by radio- wave propagation methods, e.g., phase height and absorption at Kuhlmgsborn md ionogras 0.2 to 20 mz at Juliusruh/Rugen (ZISTP, Prof. K. Spraiger).

Frcm these obaervationa, data are made available for MAP Projects: the Coordinated Studies of Dynamics of the Middle Atmosphere in Winter

Theoretical. modeling, and data analysis studies are carried out at the ZISTP on - planetary waver and circulation in the tropo-, strato-, and mesor~here.-. - photo;h&al energy tranrfer and neutral/plama interaction in the rerosphere and lwer thermosphere, including the ionospheric D region.

Rerultr of middle atmorphere research have been presented at the fiddle Atmosphere Pgnamicr Syaposium at Urbana, 1980, the IAGA and UlUP Scientific Arsemblies at Edinburgh and B~burg,1981, and the Solar Terrestrial Physicr Spposim at Ottawa, 1982. Related papers have been publirhed in Volume 2 of the Bandbook for W,in J. Amor. Terr. Phyricr, in the publication rrier 'Physiu Solariterrestris' in the Zeitrchrif t f . t4eteorologie and other journals (nee the attached reference lint1.

RECENT PUBLICATIONS FROU TEE GERMAN DEII)CUATIC REPUBLIC REWTED TO MDDLE AmSPBERE RESEARCH

Sclmitz, G. and N. Grieger, Uodel calculatione on the structure of planetary waves and associated mecm meridioml fluxes in the middle atmosphere, Bandhok for W, Vol. 2, 79-86, Urbana 1981.

Taubenheim, J., K. W. Greisiger, R. Schminder, D. Kurschner. C. von Cosmrt, and G. Entzian, Variations in mid-latitude atmospheric structure adwinds at mesopaure heights during winter 1979180. Bandbook for W, Vol. 2, 110-116, Urbma 1981.

Kruger, W. and G. Schmitz, About the rweraal of mem zonal wind during the stratospheric warming of 1970/71, Bendbook for HAP, Vol. 2. 175-183. Urbana 1981.

Schminder, R.,'K. W. Greisiger, E. S. Kazimirovaky, D. Kurschner, V. D. Kokourov. and V. F. Petrukhin, The 1978179 winter half year in the circulation of the upper mesopaur region wer Central Europe and East Siberia, Physica Solariterr, Potsdm, No. 12 (19801, 92-96.

Schminder, R. and D. Kurschner, Wind field ancrmalies in the upper mesopauw region over Central Europe and the major stratospheric warning in February 1981, J. Atrnos. Terr. Phys., 43. No. 7, 735-736, 1981 . Schminder, R. and D. Kurschner, Seasonal variations in the wind field of the upper mesopause region in 1979, Gerlandc Beitr. Geophys., Leipig, 90, No. 1. 22-32, 1981.

Bremer, J., K. Evers and J. Taubenheim, Experimental derivhtion of effective recombination coefficients in the lwer ionosphere, Gerlands Beitr. Geophye., Leipzig, 90, lo. 4, 295-304, 1981. Greisiger. K. n., 2- and 5-day oscillations in the wind field of the mid-latitude lower thermosphere from radar meteor data (in German), 2tschr.f .neteorol. 31, No. 5, 280-285, 1981.

Grieger, N., W. Kruger, and G. Schmitz, The rtructure of stationary planetary waves determined by observations and model calculations for the winter northern hemisphere, Part I: The geopotential, 2tschr.f .Heteorol. 31, No. 5, 286-293. 1981.

Kruger, W., I. Grieger, urd G. Schmitz, The structure of stationary planetary waves determi~edby observations and model calculations for the winter northern hemisphere. Part 11: The meridional fluxes of momentum md sensible heat, 2tschr.f.Heteorol. 31, No. 5, 294- 299, 1981 Schmitz, G., Transport of chemically active constituents by transient planetary vaves in strato- and mesosphere (in ~erraan), Ztschr.f.&teorol., 31, No. 5, 300-305, 1981.

Dethloff, K. and G. Schmitz, On the determination of the meridio~l circulation of troposphere md stratosphere on the basis of a zonal syrmeetric model (in German), Ztschr.f.Meteoro1. 31, No. 5, 306-321, 1981.

Entzian, G. and K.-8. Grasnick, Ozone variations and solar cycle, Zt~chr.f.kfeteoro1. 31, No. 5. 322-325, 1981.

Singer, W., J. Taubenheim and J. Bremer, A test of IRI lover ionosphere models by comparison vith radio propagation data, J. Amos. Terr. Phys., 42, 241-248, 1980.

von Cossart, G., K. kf. Greisiger, K. Sprenger, Yu. I. Portnyagin, and S.A. Lysenko, The winter 1980181 in the middle atmosphere wer Central and Eastern Europe as seen by ground-based measurenents, Physica Solariterr., Potsdam, No. 18, 77-82, 1982.

Lauter, E. A. and G. Entzian. Winter anomaly 1980181 a8 an example of a strato-mesospheric couplinq, Physica Solariterr., Potsdam, No. 18, 83-90, 1982.

Dethloff, K. and G. Schmitz, A zonally averaged circulation model of the middle atmosphere, Physica Solariterr., Potsdam, No. 18, 91-111, 1982.

Dethloff, K. and G. Schmitz, Model calculations of meridionel and vertical vind components in the winter mesosphere and thermosphere and consequences for the transport of nitric oxide, Physica Solariterr., Potsdam, No. 18, 112-114, 1982. MP ACTIVITIES IN WNGABY

Researcb activities relevant to UAP has been carried out according to the plan approved by the Hlmgarian National Committee of SCOSTEP.

Thus, balloon measureents of temperature, pressure and humidity were carried out at stations of the State Meteorologiul Service. The total ozoae content has been measured by means of a Dobson spectro- photaneter in the Central Institute for Atuospheric Physics, Budapest. For the study of the electrodynsmics of the middle atmosphere the atmospheric electric potential gradient, point discharge currents have been recorded at the Geophysical Observatory near Nagycenk of the Geodetical and Geophysical Research Institute, Sopron. The recording of the vertical air-earth current is planned to begin in My. Similarly, in the Geophysiul Observatory near Nngycenk the ionospheric absorption of obliquely incident radio waves in the LF range and relative phase height have been measured for the investigation of changes of solar and meteorological origin in the mesosphere and lwer thermosphere.

In connection with the study of changer of solar and meteorologiul origin in the mesosphere and lwer thermosphere the level of atmospheric radio noise has been studied after gemagnetic disturbances. It has been shown thnt follwing selected gemgnetic disturbances the level of atmospheric radi J noise at midlatitude stations shows increased values lasting about a fortnight, if simultmeously a clear atom aftereffect is observed in PC-1 type pulsations. PC-l type pulsations are used as indicators of increased plasma turbulence in the plasmasphere resulting in the precipitation of energetic electrons.

The turbulence at the top of the middle atmosphere has beon studied by means of a method based on the parmeters of sporadic-l layers. The mothod has been applied for the determination of turbulent parmeters above midlatitude stations at first in gemagnetically disturbed periods. It has been found that this method gives results agreeing with other investigations and indicates the decrease of turbulent parmeters above 120 km in thtse intervals. The approximations and procedures are now proved, since the computations give values of the turbulent para- meters too lw as compared to the other methods. However :e advantage of this method is its applicability for synoptic investigations. IItDIAU HIDDLE ATMOSPHERE PROGRAI. (IMP)

A. P. Hitra

In the recent past, Indian scientists have made valuable con- tributions to the investigations of ionospheric phenaeru, geaaguetism md meteorology. S;rci.l rntion uybe ude about the studies which heinprowed our mderst.tiing on equatorial electrojet, ionospheric irregularitie*, geaugoltic field variations lad monsoon circulation and eacrgetics. Also. Iodian scientists have had good experience in executing cooperative rercarcb projects; notable aoagst these being ICY (1957-583, IQSY (1%3-64), ISHEX-1973, HMtZX-77, IMnX-79, A=-6 radio kac0n experiments and the rocket crpaign during the solar eclipse of February 16. 1980. As a result of these efforts. md the progress ude in space technology, fairly umprebensive infrastructural facilities and trained unpovcr hebeen generated in Iadia for carrying o*lt further research in the fields of atrospheric sciences. Sae of the important e58ting facilities ioclude ground-based airglw photmters, atrosjhric and ionospheric radars, atmospheric LIDAB systa, three sounding rocket rsnger at Th~mha. Srikarikota and Brlasore, ballooa- lamchin: station at Uyderabrd upable of launching plastic ballxms urryiag hemy pylab for studies in aeronay and astronmy. a netvork of meLemologiu1 balloon stations of IMD, ballcon. rocket urd satellite pajyl-d dcpeloprnt facilities at 8 few institutions md expertise on design, dcteloprnt and launching of utellites in 15110. It is vith this b8ckground that the atmospheric scientists in India have placaed to p8rticiplte in the Interxutioml Xiddle Atmosphere Progra (MP)by utilising the existing facilities, adtrained mnpover oof developing a fcv nore facilities needed specifically for there iavestigations.

Following the successful coopletion of the f~t~KU8tio~lMagneto- spheric Study (IS), the Iut,-rwtioml Uitdle Atrosphere Progrr (HAP) bas beea approved by the Inter~utiormlCouncil of Scientific Unions (ICSU), as a coordinated scientific endeavour to investigate the atrospbcric pbenaena and processes in the height region of 10-100 k during the period January 1982 - Deccrhr 1985. The main objective of this progrr is to obtain a corprehensiv- understeading of the structure, chemirtry. energetics and dynamics of the middle ahosphere.

Rewgnizing the importance of investigating the middle atmospheric phenomena of f lmdrcntal importance and the wcio-econmic benefits that are likely to accrue out of the role of the middle atmosphere ia clintic variation, aasesment and iontrol of mvirol.p+ntal polluzion, radio and satellite commcmiutions ad rcmote sensing of earth's resources, tbe Indian Kat io-1 Camittee for Space Research (INCOSPAR) set up a Latioual Steering Caoittee to recorrnd the scope and mature of Indian participation in XAP. The report subritted by the Caeiittee contained the necessary justification and scientific elaents, but sac highly abitiwr in teas of its cost and implementation as a cohesive .ad integrated progrr. A series of meetings of scientists then took place to sharpen .ad crystallize the scientific elaclrts mder the constraints of limited fhncer. resources aoC practicability of implarentation within the the schedule of four yeus. This resulted in the formulation of the basic frrewark of the multi-iastitutioual Indian Xiddlc Atmosphere Progrr (IMP) costing about Rs. 2.3 crores. Based on this. IMP bs been approved as a rmtionml progrr with the participatior, of adfinancial contribution from DOS, DST. CSIB, DOE. DOEn, IUQ adUGC.

Follwicg the approval of IMP, a detailed project report has been prepared prirrily through the ef forts of ten IMP Working Croups (U;S). six of tha dealing with different scientific aspcts of the middle at-ospheric processes - radiation, atmospheric dynmics, unor constituents and atmospheric ckistry. ionization and electrody-it., rodelling of the middle atmosphere and of tropospbercffratospbcre circulation, and four of tha dealing with techoological rsprcts of the progrr - ballooar, rockets, utellite datr and wftware and 1- inforut;-= ;-! 1. The individual W; reports coctaining info-tion on rc;r.ttif ic object;-:es, identif iution of ongoing expcrirnts and theFr continuation during IW, proposed depelopr?lt of ncv expericntr. obserratiolnl plans and tir schedules, ident ifiution of individuals and groups in different in~itutions/uaivercitiesfor conducting the erpcriwnts and investigations, ~elling/theoreticalstudies, require- ment of balloons, rockets for exper-hats and satellite data hebe- integrated in the project report, the alimt details of which are smrized in the follwing sections.

SCIERTIFIC OBJECTIVES OF IW

The broad frrework of IMP scientific objectives has been structured within the basic praise of the fntexmtiool Middle Ahospbere Progrr (PUP) that scientists will collaborate inter mtiomlly:

1. To determine the structure md cosyosition of the atmosphere in che region 10-100 h, ecpcially in regard to t& minor species of irportance.

2. To deterrice the interaction of radiation frop thr sun,. the earth and the atmosphere with the middle atmosphere. .nd

3. To investigate motions of the middle amosphere cn a11 scales, in- cluding the interaction with troporphere .nd ugaetosphere. an' to conitor these wtions on a contiauiog basis.

W, by virtue of its global character, thus aphasizec the rmder- standing of various pbeaae~on a glob.1 rule, achievable through the coordinated efforts of MP projects by differmt countries md through satellite remote sensing observations, giciag wider sprtial and taporal coverage and repeatatility of he rasurscats of various atrospberic parmeters.

Tbt main uientif ic objective of IM? is the investigation of the lw latitude middle abosphrre io relation to its (1) radiation transfer ad exchoge procesrs including tropo8pber-iddle atm~sphcrecoupling and roles played b.I aerosols .nd radiativel~active atmospheric minor constituents iih ;tome, carboo dioxide, n&ic oxide etcl, (2) atmospheric dynamical features including gemeration, ~plitudeand phase variations, propagation .ad aplifiution, reflection and dissipation of planetary waves, equ~tori.1 waves, tides. gravity mes a~dturbulcoce. (3) structure ma camposition including ozom chcrirtry. role of una constituents in controlling D-region ionization prousas and rcle of aerowls in influcnciag earth's radiation beet 8nd in ionic reactions in the stratosphere, (4) ionization .nd elutrodyruriu includiog D-region ionization state, umples ion cbaistry of the stratosphere md mesosphere md the role of solar and nowsolar sources and their chmges an t5e electric field in the middle atmosphere and its i~plicationson the glob.1 electrical circuit. (5) mdelliw of the distribution of neutral amosphere, mioa constituents, dpmiul unpnents (winds md w.res), ionization md ion camposition md effects of perturbations due to variations of oec a more of these oo otbers and (6) rodclling of troposphere-stratosphere dynuical coupling including mean flw .ad wave irteractions, radiative enlunge md transport pbmo~crubetvea these tvo regions.

Tk activities of cooductiag differet experiments .rd obervationr during IWcao be mrized as follws:

1. Radiation studies include (1) ground-based lidar and rultiv.rt length radiaetric w88uraattS of taprature profile. aerowl density aod their scattering properties giving aerosol psrticle size distribution, radiometric measurements of wlar W-B radiation received on the earth ad influenced stratorpheric ozoac md ~nitoringof airglou emission fram 03(l:g) and 05 at infrared wnelaogths, (2) balloon-borne experhents for ruuring terrestrial upuelling radiation, aissions fra 02(l.1. 1, molar W radiation md optical scattering iry ~~TOSO~S,(3) rocget experiments for wuuring w scatter at .3;. W intensities between .2-.3u and -22--2% w.veleogth bands giving ozooe and 10 profiles, respectively, Lyman-2 and 02(1~g) emission fluxes md (4) satellite data reception fra IWMA to derive temperature profiles betveca 15-45 km and use of UImUS-7 satellite datr for deriving the prof ilea of vertiul taprature sad risol constituents md estirtioa of inccming solar radiation and outgoin= earth's radiation.

2. Studies of amspberic dyluriu include (1) ground-based experiments of rteor wind md prtial-reflection radars For ruurement of wcoapkric vinds. udFabry Paot interferometer to wlurcr hrglav emission from vhich winds and taprature un be derived, (2; balloar borne urruramts of rteacologiul parreters using high altitude rubber ballocms md chemical puff release esperiwnts using polyethylene balloons fra Byderabad for eddy diffusion coef f icient md vertical winds, (3; rocket-borne w~sur~cntaof rteaologiul paraeters using U-100 and RE-2QO rockets and of vinds in the therrospbere usiw Rib300 and OH-560s rockets md tapratore uroursenta in the stratosphere/ usoapbrre wing P%MO/I)-100 rockets for the study of stratosphaic vamiogs md (6) utellite -#at.for vertiul profiles of trprature.

3. Studies of minor constituents and atmospheric chairtry hcludt (1) ground-bawd reuuracnta of total ozoac~antatwing bbsoo's spectrophotaaters, urglw airsions of 02f l:, ) for stinting wso- spheric ozone content indirectly md of 08 aiisioas, (2) ballwo-borne rusurcleats of ozooc profiles wing electrochemicrl deurried in high altitude rubber ballmas, uuuraents of verticrl profiles of a nuder of minor constituents 0, HJ, 02(': 1, lIBOj, 10,, aerosols etc., using pbotaeters sad pbotoionization aasB spectractks, (3) rocket- borne wasursents of vertiul profiles of ozone and nitric oxide using osiul oronosoade and y-band photcmetry payloads, respctively, md (4) ur of data from M)bb-6 -3 RIlUlUS-7 utellitea for deriving the prof ilea of ozone md of a number of minor constituents such as CD,,- CO. M), water vapour. X,O- and CEA. I. Studits oi ionization iod elec:rody*aics inch& (1) ground- baaed measurement of D-regron electron-density profiles using p.rtiai reflection, cross modulation md Al resorption experiocats (2) balloon- borne measurement of electric fielda and ions in the stratosphere using double Langmuir probe, Geraian condenser md Blunt probe and (3) rocket-borne measurement of electron density profiles and their variations witb wlar zenith mgle using Laarpuir probes, propagation experiment and Cerdim wndenrr and of electric fields using double *.ngruir probes.

5. Welling studies of the middle atmosphere include (1) generation of time-independent rodels involving distribution of cbaiul species prticularly ozone, aerosols, electron and ion dmsities, solar and terrestrial radhtion fields .ad dynamiul fields of winds and waves, (2) generation of 2- and 3diamnsional photo- chemical models incorporating vertical eddy dif fwion coef f icentr, latitudiml gradients, dependence on time. and intoractions between chemistry, radiation and dynnica by incorporating a simplified chemical scirae in the general circulation lodels. (3) generation of two- dinlsioml models of s anber of important rina species for vhic5 the lifetivs are large and (4) efforts on threedirnsiomal modelling vitb interactive radiative. cbmical and dpoiul procesrs.

6. lbdclliq studies of troposphertstratosphcrc circulation include (1) interaction betve~vne motions on different tir and space Uales, (2) respoor of stratosphere md the lwer rsosphere to forcimgs by energetic systas in the trcposphere. (3) effects of clouds and aerosols on the cnergylheat budget of the riddle ahosphere and (4) vertical propagation of planetary vne cnergy fra the troposphere.

Vuious individusl elsets of ewriunts and obsenations lcotioacd above hebeg integrated vith the werall activity of W. Efforts hme been initiated to ensure the nailability of various experbeats during the IMP tirfrme and broad rqucnces of obsemations, multitechiquc and rultiprrcterbrwd obsemations to study a spcial riddle abospheric phcnacnon and coordinated data a~lysisand interpretation hne also been planned. In order to achieve this task it has been agreed that the activities of IWbP vill be kple- mted prirrily, (1) by conducting studies csing past &:a to consoli- date the inforution relating to certain specific aspcts of physical and cbsiul procesrs in the riddle atmosphere, md (2) by carrying out vell plmned uprigns of experiwnts/observations identified for investigating certain specific phenae~of the riddle atmosphere. A number of sach coawlidation studies and upigns hme been plrnmd to be carried out during IXILP, some of vhich are suarized in the follwing sections.

(a) Coosolidation Studies

Upwelling Radiation: 11Q)has been conducting ground-bawd and ballocm-borne Pcasuraents of terrestrial radiation from 8 feu locations in India. The results vill be consolidated taking into account inter- calibration of i: struaents, variations vitb season rnd different types and extent of cloudiness.

Studies on Airglw Emissions: Observations of airglw cnissir~nsof 6300 A and 5577 A h8vr been carried out by PRL and POOM University for more than a decade. Thew sissions take place from layers of the atmosphere around 250 and 100 b, respectively. From the intensity and Doppler line width r;surgents, it is possible to indirectly determine the atoic oxygen con~entratio~sand tmperature at these altitudes. In addition, observations have also been carried out on intensity measure Pcnts of emissions from sodim and Oii molecules. Results obtained from these studies will be consoli&ted. Rocket Data on Atmospheric Temperature and Winds: Since 1970, weekly II-100 rockets have be- coctinuously la~mchedfra Thmba. Using these data, a number of investigations bebeen cooducted dealing with different aspects of tsprature structure and dynsmiu of the riddle amospbcre. The results reported u, far will be smrized and a con- solidation report published.

Lou Latitude Ozone Profiles: A zero-base lode1 of ozone concen- tration profiles for the lw latitude region vill be ude using the e.i#ing Dobson's spectrophotaetric data, *ad obserrations from hlloao, rocket and satellites tra the stations in the globs1 ozo= n+ tvork.

Reference Minor Coostituents Ilodtl: Fmthe available global data a zero-bar reference rinm constituents model will be generated which is appropriate for the Idim region.

D-Region Electron-Density Profiles: From the available data on electron-density proiiles ruured using rocket-bcrc experirnts, ground-bard partial-reflection and cross-rodulation experiments, and International Refera-e Ionosphere data. a reference lw latitude D- region ionosphere vill be derived.

Aero.o?s: This upign vill include bal1oo~-bornewasuraets of aumber densities and scattering properties, rocket-borne uasursents of W scatter st .3u, extinction seasurements by ground-based multi- vavelcogth rrdicmeters ia the visible b.nd giving aemnal size distribution and ball- and rocket-borne ras-ots of stratospteric ions. The main objective is to characterize optiul properties of aerosols for radiation Sudget studies and for understanding the ion- aerosol react ions.

Radiation Budget: Coordinated reasuraents of balloon-borne upgoing and -coming radiation flux measurements, cloud wvcr and utellittderived cloud-top temperatures to study troposphere- stratosphere radiation exchange and radiative flux divergence in differmt layers up to the stratosphere.

Solar UV Radiation: Ground-based kUV and multi-wavelength radiooeter wasureaents including higk resolution W observations, balloon- and rocket-borne radiation measuraents of Wm (0.2-0.3~) and Lyw-a flux to study the W energetics of the middle atmosphere md to rmderstmd various photochemical and dyrvaiul processes governed by this solar radiation.

Stratospheric Warming. LIDAR-based, W100/RH-200 rocket and balloon-borne tmperature masurslents vill be carried out during a strong stratospheric varring event for a detailed study of the develop- ment and horizontal extent of this phenaaenon. SLult.aeous measure- ments of ionospheric absorption, D-region ionization profile using a partial-reflection experirnt and of stratospheric/mesospheric winds will aim be conducted to study the effect of this vaming on neutral and ionized regions of this middle atmosphere.

Nesospheric Temperature: With the help of balloon-borne taperature wasursents up to stratospheric heights, tezaperature measursents using It-100 rockets carrying USSR-=& scnwrs and 88-200 rockets carrying Indian-ude sensors, an interamparison experiment will be rmdertaken specially in relation to mesospheric taperature values vhich are not lmaun accurately at present.

Amospheric Tides: It is proporcd to have simtltaneous balloon and rocket wasuraents of vinds at least four times a day from a feu stations for elected months representing different seasons. This will help investigate the tidal patterns, their generation, propagation and dissipation in the middle ahosphere. This -paign vill be attempted rader a rparate proposal.

Ozone Interamparison: 1ntereolp.rison and measurements of ozone concentrations using various techniques of ground-based experiments. e.g., Dobson's spctrophotaeters and IR phocoeters for 1, balloon-borne electrochemical ozonosonde and rocket-borne W-a%sorption ozonosonde vill be carried out for at least tvo locations - Thumba and Balarore/SEAR. Tbe~obsenations vill help determine the relative values of meuursmts of vertical ozone profiles and its variations vithin the la, latitude region. Vhere-er possible the experiment timings vill be adjusted to coincide with satellite passes for further comparison with utellittderived ozone concentration profiles.

D-Region Imization: Intercomparison of electron-density measure writs vith different rocket paylosds (Gerdian condenser, propagation experiment and Lmgruir probe) simultanears with D-region electron- density measurements using ground-bawd partial-reflection, cross- modulation and multi-frequency Al absorption techniques vill be carried out.

Caaductivity: Hear-silultaneous measurments of thunderstorm activity, electric fields near the surface using Kytoons, at balloon and at rocket altitudes along vith ion-density lelsurements with balloon- borne p.yloa& vill be carried out for investigating the electro- dynaical procesees in the D region.

Uerosphere/Mesopause Processes: The near-sinultmeous measurments of various parreters will include ground-based meteor wind and partial- reflection radars for wsospheric vinds. blOO rocket flights for rasuretnt of temperature and winds in the mesosphere, IW-300 rocket measurements of electron-density profiles, ataic oxygen, nitric oxide and L-n-a flux. Tte main objective is to study various physical and chemical processes, and their interplay especially near the mesopause where the values of the above parmeters undergo considerable changes.

Based on the above-uentio plans of the six IW Science Working Groups and various campaigns, the detailed time schedules of individual experiments have be- worked out by the IlUP Technology Working Groups on balloons, rockets and satellite data and software. These vill be further refined, bawd on the readiness of various experi~entslp~yloads. availability of balloons/rockets etc. For an adequate flow and exchange of information regarding various activities of participating scientists and for providing the necessary interface with the International UP, the IMAP Information Cell will collect, compile. store and disseminate information of scientific experiments, data availability and progress made on coordinated efforts in mpaigns and consolidation studies.

PARTICIPATION OF SCIENTIFIC GRCUPS IN IHAP

Wore than 200 scientists working at different universities, national laboratories/institutions and government departments have already been identif ied for participating in various IUAP activities. These scientists are being supported by a large number of engineering and technical staff for design, developrent and operation of different experiments and for conducting scientific observations and research. Scme of the major groups belong to the follwing institutions - Physical Research Lat.oratory. Atmedabad, National Physical Laboratory. New Delhi, Vikra Sarabhai Space Centre, Trivmdrm, Space Applications Centre, Ahedabao, Indian Institute of Technology, Indian Institute of Science. India Heteorological Department, Indian Institute of Tropical kteorology. Paoust, Gujarat, Delhi, Andhra, Calcutta, Udaipur. Kerala. Nagpur, and Marathwada Universities.

It has been agreed that the vhole IW activity will be carried out vith the existing manpower in participating institutions and that Research Fellwohips/A~sociateshipsagreed to be provided by some of the funding Ageacies will be used for specific needs of carrying out experiments, observations, data analysis and interpretation. However, for running the progrrP in an integrated manner, a limited number of staff will be required to coordinate various activities, monitoring progress and tinre schedules, service to be provided by the Inforration Cell, operating the budget and keeping the accounts of expenditures incurred under various activities.

CONCLUSION

Thus, the atmospheric scientists and technologists a11 wer India are nw geared to concen:rate their research : civities on investiga- tions of the middle atmospheric phenomena and processel during the four- year period of 1982-85. Built on the strength of existing trained scientific and technical personnel and available large- and medim scale facilities, 1Wpromises to t one of the major cooperative exercises of scientific research in .ndia and has in store many porsibilities of breakthroughs in the field of atmospheric research which may have far reaching implications on our understanding of the earth' r enviroment. HAP IN JAPAN

The HAP coll~cmityin Japm is engaging in vrriour activitier. In January 1982 a IW Syrporirn war held at the Institute of Space and Artromutic Sciencer, Tokyo, with about 100 participant8 and about 50 paper presentation8 on dynamics, composition, aerosol, radiation and modeling. The Antarctic obrervationr were discurrcd in detail. Such a ayrporirn is planned to be held each year during the W period. IUP Pews bra been irrwd twice, reporting up-to-date rtatur of variour W activitier; NAP Ncvr will be irrucd periodically during the HAP period. In general, Japan'r national prograr for IW have started according to plans.

As to winds and waver. the Kvoto neteor radar has been in operation regularly, urually for a &uple of days per week and continuously during

campaign~.- period. ar in Novaber 1981. The data have accumulated to ruch an extent ar to be able to analyze lunar ti&~. We finished ruccearfully a Jiurarca radar observation in Nweber, 1981 in cooperation with an Arecibo observation by the Uax Planck group and others (upaign organized by ICIJOA). An observational network for HF Doppler mearurmentr by the standard radio method har be- organized, consisting of ~veralstations.

As to comporition, ground-based observations of ozone and other minor constituents by lrrer heterodyne rpectroscopy and ultraviolet libr is in preparation. Balloon sampling of the constituents will soon be in operation.

As to aerosol and radiation, aircraft and ballc-. .. -zperimente will rtart in 1982. Lidar obrervationa have already been active in detecting aerosols in intense fluctuationr by the Ht. St. Helena eruption.

The Antarctic Obaervation will be in full operation from 1983 as an internatiouul progra ar discurlied in Edinburgh last year.

The HU radar wnrtruction is progrersing at Shigaraki, to be complete in 1984 (to be partly in operation from 1983). The EXOS-C satellite will be launched, as scheduled, in rpring, 1984. Berider observation progrms, data uulyris, modeling and theoretical studies are rtrongly encouraged to drau marin- benefit f roll HAP observations. An international )UP ,ymporiua is planned to be held in early ruamer in Kyoto in 1984. MAP-BELATED RESEARCH IN THE REPUBLIC OF CHINA

T. Tny

1. Department of Atmospheric Science, National Taiwan University: - Wave oscil lations near the tropopauae in the nubtropical region.

2. Department of Atmospheric Physics, National Central University: - Theoretical study of atmospheric tides and acousric waves. - A VHF radar, which can be used both in the SAD (Spaced Antenus Drift) and DBS (Doppler Beam Swing) modes, is in the planning process and will be constructed on cmpus and in operation in the s-r of 1983. - Other experimental studies of ionospheric disturbances by using micro-barograph. three-component magnetometer and HF Doppler sounder will also be conducted.

3. Department of Chemistry. National Tsing-ha University: - Upper and middle atmospheric chemistry.

4. Telewmmmication Laboratory. Directorate General of Tele- communications: - Real-time HF Doppler sounder and microbarograph recording as well as observation of D-region absorption phenomena by riometer at Luaping Observatory (2S000'N, 121 '10'~). - Obnervational study of lightning flash counting. HAP ACTIVITIES IN THE UNITED KINGDOM

L. Thomas

A report on the UK plans for W,prepared by the British National Committee for SolarTerrestri.1 Physics, vas widely circulated in the SUa~mer of 1981. It foresaw activities in three areas: stratospheric composition, mesospheric and lower ioospheric :tructure and co~~position, and dynamics.

The stratospheric composition studies are to be bared on currenc UK experiments on Nimbus 7 and the Tiros N series of aatellites, ballwn and aircraft-borne experirents, and ground-based mearurements. Firm plans are now being formulated for balloon campaigns, both n3tionn.l and in collaboration with the Federal Republic of Germany and NASA.

As a result of financial cut -backs, the UK small rocket progrsm, on which the planned mesospheric and lower ionosphere studies are largely based, is being cancelled for two years from April 1982; for this period certain groups have arranged to provide payloads for foreign rockets as part of collaborative projects, and this procedure will help maintain expertise for the possible reinstatement of the UK progrcame in 1984. Thus the involvment of two UK rocket groups in the Swedish CAKP project t.as been confirmed and experiments will also be provided for the Canadian OASIS cmpaign. The latter represents an extension of the successful cllmpaign carried out on 23 Harch this year to study the excitation processes of atomic and molecular oxygen airglw emissions from the mesosphere/lower thermosphere; this involved six Petrel rockets launched from S. Uist and carrying experiments from the UK, Swedish and Canadian groups.

The transfer of the meteor radar from Stornaway to Aberdeen, to operate in conjunction with the system at Sheffield for studies of gravity waves and turbulence. is proceeding. Plans for carrying out studies of these scales of motion at lower heights. using a VHF radar system, have been considered and, a design study of such a system is in hand. MAP PUBLICATIONS COMUITTEE REPORT

C. F. Sechrist, Jr.

C. F. Sechrist, Jr., Chairman R. D. Bojkov R. J. Murgatroyd V. V. Viskov

MAP Uevsletter

Th2 HAP Newsletters are being published in 1982 as ?ecial Issues of the Lpper Atmospheric Progrllnr Bulletin vhich is funded jointly by the NASA Upper Atwospheric Research Progrm and the High Altitude Pollution Program of the Federal Aviacion Administration.

W Newsletters were publirhed and distributed in July 1981 and in January 1982.

The next issue of the HAP Newsletter will cont. n condensed minutes of the HAP Workshops and MAP Steering Committee meet gs held in May 1982. It vill be distributed :a August 1982.

Contributions for th* MAP Newsletter during 1982 should be sent to:

Bulletin Editor (AEE-300) c/o Dr. N. Sundarartman Federal Aviation Administratio ROO Independence Avenue, S.W. Washington, D.C. 20591 USA

Handbook for MAP

Volumes 1, 2 and 3 have been published and distributed.

Volume 4, covering the HAP Assembly and HAP Opel Meeting, vas published and distributed in April 1982.

Volume 5, a ayumic climatology of the st-atosphere, was published in early Hay 1982. Jt will be distributed during the latter part of Hay 1982.

Pro~osedPuturt!Torics for Volumes in the Randbook for MAP

OWDiructory (Volume 6, 1982) *W dorkshops and Sympsia (Voluae 7. 1982)

'Satellite expcrirents including SAGE, S#. BALOE. AmS, LPIP, XOM, DE. EXOS-C (Val- 6, 1983)

'Ground-based techniques including prrtial reflection ionization drifts, middle atnosphere radar, laser radnr, attar radar (Val- 9, 1983).

Contributions for the W Hevsletter

%re contributions for the MP Ncvsletter are urgently needed. These are needed in order to pub1i.h the K~sletteron a regrlar schedule.

Surutestions & Contributioas for E~dbookfor Uik

The Publications Caittee welcomes suggestions cf future topiu for volucs of the Bandbook far PAP. S*~gtstioasmd contributions rhould be sent to:

Professor C. F. Sechrirt. Jr. University of Illiuoir Departrent of Electriul Engineering 1406 Y. Srcen Street Urtuu, Illinois 61801 CSA PW-1 REPORT

RiE FWRTH UUTER OF PKP-1. 1981I82 : A UIhiER YIW SEVERAL IhTERESTItiC FEATL'RES

K. Labitzke. et al.

A synoptic descriptian is given for the fourth winter of PMP-1. 1981182. The -in characteristics of this winter are a Canadian uarning in the beginning of Decenber, a very strong minor warming in January. &~dan early final warning in mid-mch. In the spcood part the eddy -eat= budget, calculated from the daily height and tmprature charts, is discussed ia ternis of the divergence of the Eliassen-falm- Vector.

The winter 1961182 started with a Canadian warning in the beginning of December, which showed the oost intense development of height wave 1 (uoplitudes of teperature and height waves 1 and 2 at 30 mkar are shown in Figure 2b and Ze) observed since 1965. The maximum of this wave lies typically over Cawrda, as noticeable in the 10pbac chart of 5 December 1981. As the Canadian vancings are con£ ined to the lover and middle stratosphere the yak in the mrch of temperatures over the Horth Pole (Figure lb) was stronger at 30 nbar than at 10 rabar and the radiaace data of the uppermost channels of the SSC' (Figure la) did not show much of the warsing dc-irg this time. Moreover, the temperature grsdient between the H.)rtt Pole and 60% was r-ersed for a longer time at 30 rbar than at 10 =bar (Figure 2d). There was only weak upward directed geapotmtia: flux through 30 rbar at 60% (Figure Zc) but the eddy heat transport by the wave nusber 2 was strongly directed northward at 33 rbar (Figure 5). The mean zonal wind at 60% considerably weakened at 30 and 10 mbar, acd north of 75'N easterly winds wen occurred at 3u mbar (Figure 3).

In aid-Dece~ber a warning period was observed at the upper strato- sphere as car be seen by the radiance data of chrnnel 27 (naximuu weight around 1.7 mbar) of the SSU at the Eorth Pole (Figure la). aad the nort'lern hemispheric discribution of chrnnel 27 radiances shoved a reversal of the gradient betweer the Korth Pole and 60°K for several days (as an e-ple see tte chart of 17 December 1981, Figure 4). hring the same tipe the lwer .ad riddle stratosphere continuously cooled (Fig-ares lb and 3). the =an so-1 vind steadily lacreased (Figures Za and 31, and on ZC December a first wintertiw minimum of tmperature was reached. This was connected with .;r aplificatioa of tmperature and height wave 2 (Figure Zb and 2e) by which in the zonal Figure 1. ?larch of ratiances and tgmperatures over the Sorth Pole: a) Radiances in%!raAsr cm'l] of channel 27 and 26 of the SSf. vraximlln weight around 1.7 and 4 mbar (courtesy ?leteorolo~icalOfficc Btaciinell. Y.K.1 h) Temperatures [OC] at 10 a~d3'7 mbar (horizontal lines are long-term wnthlv means). Figure 2. %?rived quantities (daily :slues) describing the =inter 1981 '82: ar Yean zonal i-ind [m s-I] at 60"s. 10 and 30 nhar: 5) .hplltuOes of temperature vaies 1 a4 2 I'C! at 6Q0S. M mbai; c) Ceopote~tialflux 16p-21 ihro~r~:~30 tbar at 60DS: d) Temperature dif- ierences ;'i') Setwee2 Sorth ?ole and 60':;. 10 and 31 izbar: c) XnplltuLes of height waves . and 2 Igeopnt. r.; at ht'"'.. 30 nbar. 52 MEAN ZONAL WIND MEAN ZONAL TEMERATURE X)mborfm/sl anrbo PC 1

WI 70 60 SOW 40 3PI

Figure 3. ?;eridionai time sections ron ';or-eeher 1981 io Yarch 1982 cf xan zonal vind jr: s-I (shadtmd areas represent negative values. i-e., vinds from he cast) and -. 111 zonal temper?- cure ;"C] at 30 n.f.ar. MC~P~=as re11 as heat was transported northward (Figure 5). The geop.it,-.tial flux upward through 30 mbar reached a mxirum (Figure 2c) but the waning of the upper levels did mot propagate much dwnvard in rhe follwing tir, there was only a -11 temperature peak at the North Pole around the Christus days (Figure lb).

After a relatively quiet and cold period around the change of the years wbcre the rcond wintertie taprature minim aver the Imth Pole was reached (Figures 1 and 31, a strong waning occurred in January which developed within two pulrs. Until 10 January a very strong kight and taprature wave 1 developed (Figure 2b and 2e) while the height wave 2 concurrently shoved a pronounced minimu, which is one of the preconditions for the onrt of a uja waning, as pointed out by tbitzke (1977). Tbc radiances .nd tapratures at the North Pole (Figure 1) reached a mxirtm and the taprature gradient between the Pole md 60% was reverrcd for a short tir at 10 mbar (Figure 26) and ahe. The strong wave 1 transported not only hat but 8100 mcmenttm nathward (Figure 5) and the ro zonal wind at 60% (Figure 28) was decelerated only to a lull mount (the mmentam budget will be diuusrd later).

During the follwing ten days the lower rtratospbere cooled again over polar regions, leading to the third taprature rinirmr of thir winter on 25 Jmuary Vb8 the strongest mgative taprature difference between tke llorth Pole and 6011 war oluerved beuur the second warning pulw si~ultmeooslyoccurred wer rid-latitudes (Figures lb, 2d, 3). Tbt wm 2-1 wind strengthened and reached the wintertir uxi~ betveen 60 and 70% with mre th.n 50 4s at 10 mbar (Figures 28 and 31, and the geapot~tialflux through 30 mbar upusrd reached the highest value of this winter (Figure 2c). It was during this cooling period that the Europe- Centre for Wiu Range Weather Foreustr at Reading, U.K.. predicted a split of the polar vortex within the next week bared on the initial H)+ar analysis of 17 J.nuary (Klinker, 19821, md 8 major waning was predicted by the daily SIRATALERT me~ugesof Berlin. As can be wen in Figure 2b .nd Ze, a very strong taprature and height wave 2 developed and the l0-rb.r chart of 22 January 1982 shws the clhx of thir wave with the split vartex and strong mtiqclones associ.ted with sam regions wer the northern Pacific and Atlantic 0ceIIs.

The waning of the polar region progresrd within the next days and the radiance chart of chmnel 27 of the SSU show the strong therul ridging across the Pole om 24 January 1982. Three days later the peak of the waning was reached at the lwer and riddle stratosphere (Figurer la and lb) but the taprature gradient beweu~the Pole and 60% again was only reversed at 10 rbar (Figure 2d) and above, and a circulation reverul (i.e., rmzoml wind from the east fra 60.1 to the Pole) was not observed klw 40 h altitude. Tbc w.n tom1 wind at 60.11 and northward only veakened considerably in the lover stratosphere (Figures 2a and 3). The 10-b.r chart of 27 Jmury 1982 shows the circulation on the day with the strongest tmperature gradient reversal and the lovest rem tonal wind at 60'N. As can be seen by Figure 5, there was a strong northward directed heat and mmentum transport by wave 2, while the transports by wave 1 cimultmewsly were directed southvard. The maentua budget tnd its effect on the change of the mean zorul wind will be discussed in the second section. Finally, no break-&wn of the polar vortex war attained and this event should be called a strong minor waning.

During February until the middle of &rch the tealrrature distribution at 10 mbar .ad above rapained slightly disturbed and two waning pulses were okerved at upper levels in mid-Febrary and in the beginning of arch vhich did not much penetrate downvard (Figure 1). On the contrary, the 30-bar tsprature aver the North Pole was quite belar the lollsterr r.n during this period (Figure lb). Tbe radiance chart of chmocl 27 of the SSO fra 13 February 1982 shows one of these waning period. (Figure 4) during vhich the warp centre at the l0qbar level was situated over Europe, as tbe axis tilted westwards with increasing height.

in rid-lkrch an early final warming began. At the lOabar lwel the van centre cwer northeastern Asia strengthened (as uully is observed during final warnings) and spread northeastward over the CuL.di.n Arctic tward the Pole. The tsperature wer polar regions iacrused (Figures 1 and 3) and the reversal of the tenperature gradient between the Pole and 60% (Figure 2d) continuously propagated downward reaching the 5O-rb.r level at the end of Iluch. The radiance chart of channel 27 of the SSII. from 30 March 1982 (Figure 4) and the 10-bar chart fra 31 March 1982 show the strong waning with temperatures vell above -rtir values. The rau zonal wind at 60% (Figure 28) and further to the north (Figure 3) steadily weakened (see Figure 5 for the routhward eddy uuntum transport by wave 2 and more intense by wave 1 during krch). The rasuraents of the prevailing vinds at rsopause heights wer Central Europe from the Geophysical Observatory Collm, GDR. shoved the trmsition to vinds from the east already in the middle of fir&, which war defined as a very early start of the so-called spring anaaly within the circulation of the mesopause region. At the lo-mbar level the tom1 wind at 60'19 reached negative values on 6 April adten drys later the wind reversal was accrtlplished at 30 mbar, too (Figure 28). Thus, a vesk zonal f lw from east to west governed the region from 60'1 to the North Pole from 30 mbar upward at the middle of April . CALCULATION OF TBE MIENTWII BUDCET

Tbe planetary waves (see Figure 2 for mplitudes at 30 mbar st 60.1 0: vave rurbcr 1 and 2) transport heat and rapcntum and are able to chmge the ran soml wind. But the mem reridional circulation 2 Figure 4. Charts of radia-ices [mW/m sr cml] a* channel 27 of the SSV, maximum veight around 1.7 mbar (courtesy Xeteorological Office Bracknell. C.K.) O E C x u N-c m 0 mum 3UO c b x CC uO:o bGb s m TbO: u r: o z8 UilL S m i C) 02.C-G m fi 4LZ2 >. Q OOO: C E 3 PIC& >mm 0 n Z- E sirultaneourly forced by the steady conrcrvative waves compenmtes these ecdy transports by the steady waves (adiabatic temperature change by the Coriolis torque of the horizontal component), so that only transient waves are rerponsible for the weakening or strengthening of the mean zorvl wind by interaction with the waver. Andreus and HcIntyre (1976) introduced a transformed urrentum equation which show8 that for qrusigeortrophic assumptions the change with time of the me= zonal wind is caused by three procesrca being frequently of opposite sign: - - Change with latitude of the mean eddy mmentur trantt u'v' - Change with height of the mean eddy heat transport v'T' - Coriolis torque of the mean horizontal meridional circulation?, vhich is derived by subtraction of the uneffective parr due to the steady waves fror the mean north-south velocity.

The fornula for the computation is (with A = radius of the earth and 9 = potential tmperature).

where the veccor F, named Eliassen-Palm-Vector, represents the flux of wave energy, the eddy forcing on the zonal mean flow is contained in the divergence of this vector : Divergence (convergence is causing acceleration (deceleration) of the wan tom1 wind.

The budget of the three terms in the transformed momentum equation was umputed from the temperature and height charts of the middle stratosphere during this winter. In December, January. and February the mean eddy momentum transport as well as the mean eddy heat transport was mostly to the north (Figure 5). but the former predominantly accelerated the vesterly wind while the latter caused deceleration (Figure 68). Illurtrating the budget for the change of the mean zonal wind with time Figure 6b shows that at 10 mbar periods with continuous deceleration of the wan flow were caured by the waves because the Eliassen-PalaFector was strongly convergent (6 Jan, 21 Jan, 4 Feb, 21 Feb, 28 Mar). The mean meridionnl wtion compensated partly the effect of the waves but the direction of the change (negative sign) was determined by the convergence of the Eliassen-Palm-Vector. This total convergence happened on those days when - besides the mstly convergent vertical component - the horizontal component was convergent, too (Figure 6a). Tb deceleration of the westerly wind by interaction with the waves did n. lead to a breakdown of the stratospheric polar vortex during this winter. But the flw of wave energy into the polar cap in the middle of March, indicated by the northward directed Eliassen-Palm-Vector (eddy momentum transport to the south, as seen in Figure 5 for 30 mbar and in Figure 6a for 10 mbar ~rkedby N), led to an early reversal into sunmerly circulation features with the breakdown of the westerly winds of the polar vortex. Figure 6. a) Divergence of the Eliassen-Palm-Vector at 60°N at 10 mbar a - [m s-l/dayl - horizontal amount --(-;.-os$vlul), a- a. Aces; a+ --- vertical amount f -(v'B1/-), b) Terms of the transformed ap ap quasigeostrophic zonal mean nomenturn equation [m s-l/day] - change of mean zonal wind a; -at* --- divergence of the Eliassen-

Palm-Vector V-F, --• Coriolis torque of the residual meridional motion fi*. For monitoring the rtratorpheric-rpcrorpheric vintertiw circulation and preparing the daily STRAT?ILEltT meruger we obtained the follwing additions1 inf oruti,n. - from the )Ictecrologiul Office Bracknell, U.K.: Daily chartr of radiances for the Northern Eairphere of chrnnelr 26 and 27 of the SSU (Stratorpheric Sounding Unit) onboard the NOM satelliter and the prelirhury 10- and labar height chartr derived from these data. - fram the Clarendon Laboratory. Oxford, 0.K. : Retrieved temperature distributions over the Northern Hmirphere at 1, 0.3 and 0.1 mbar from the SIllCS (Stratorpheric and Hesorpheric Sounder) onboard Nimbus 7. - from the Geophyrikal Observatory Collm, GDR: Prevailicg vindr at meropaure t-ightr over Cmtral Europe from lw frequency drift mearurementr.

- from the Physics Department of the Univerrity Yupprtal: Tmpraturea at 85 IsP altitude measured with a ground-bared infrared rpectrooeter at Wuppertal.

All thir support ir gratefully acknwledged. We thank the aaberr of the Stratospheric Research Group (Berlin) for the prof ersio~land technical arristance.

Andreus, D. G. and H. E. HcIntyre (1976). J. Atmor. Sci-, 33. 2031-2048 Klinker, E. (19821, ECM Nevsletter, 14, 6-7 Labitzkt, K. (19771, Urn. Wea. Bev., 105, 762-770. PW-2 REPORT

EQUATORIAL WAVE DYNAHICS

I. Hirota

Pre-MP Project 2 (PW-2) was proposed and accepted in 1978 at the first !fAP Steering Camittee reeting held in Imsbruck. This report briefly describes the activity of PMP-2 during the past four years of 1978 through 1981 and ccne s-ientific problms to be studied further.

The =in purposes of PHP-2 were as follows:

1. To survey current problss related to the dyoamics of the equatorial middle atmosphere, as an extension of the review on this subject presented in the UAP Plrnning Docment (1976).

2. To continue observati~~nalstudies with use of available data sets such as those cbtaine~from satellites and rockets,

3. To develop theoretical and numerical models to clarify the nrture of equatorial waves and their interaction with the mean zooal flow.

4. To carry out special experimental progrrs with the aid of high- power radars located in the tropical region, ad

5. To propose further measuraent progrrs for oevly defined probleus.

An interim report on ites (11, (2) and (3) bas been published in the Volume 1 of Handbook for HAP (19811, and a brief rwiw of observations of equatorial vaves also appeared in the Volume 2 (19811.

During the i960s. the dynamics of the equatorial stratosphere. especially the generation of the quasi-biennial oscillation of the mean zonal wind, was extensively studied in terms of the wave-mean flw interact ion.

Rwever, as pointed out at the HAF Planning Conference (19761, there were large gape in our howledge of the nature of the wind and vaves in the equatorial mesosphere and lwer thermosphere, mainly becauae of the lack of adequate observations in this height range. In particular, the lwchauiw for generating the westerly £1- associated with wmiannual oscillations around the stratopauae admesopause was one of the most outstaoding problas concerning the dynamics of the equatorial ciddle atmosphere.

Since theoretics1 studies iodiute the possibility of upward propagation of various equatorial wave modes into mescspheric levels, it was recocamded, at the starting point of Pre-HAP, that special observations were me&d to establish the nature of these vave lodes.

(a) The Saiaumal Oscillation and Kelvin Waves

The existence of the semiannual cycle in the equatorial middle atmosphere was reconfirmed by utellite infrared mearuraents from the limbus 6 PHt (Crane. 1979).

In order to test the theoretical hypothesis that the vertical propagating Kelvin wave is responsi;,e for the westerly acce1era:ion of the eqrutorial zonal flw in the uemiannual cycle. Birota (1978, 79) tried to find evidence of Kelvin waves in the Lpper stratosphere and usosphere by using rocket and utellite (Nhbus 5 SC8) data. It was found that a Kelvin wave with long vertical scale (15-20 L)md zonal vave n\raber 1 is predominant .nd mwes eastward vith a short period (4-9 days).

Nucriul Eodclling by Dmkerton (1979) shoua that such a Kelvin wave gives rise to the observed westerly acceleration associated with the semiannual zoml wind oscillation.

(b) Planetary Rossby Waves

On the other hd, it has been considerea that the equatorward propagatiog, planetary-scale Rossby vme is responsible for the easterly acceleration of the semiannual 20-1 vind oscillation, in addition to the effect of the global-scale re- meridio~lcirculrtion in the middle atmosphere.

Recently, using :he Tiros N SSO observations, Hirota (1981) shoved evidence of the wmiannual cycle in the horizontal eddy uentru flux coover&cnce at the tropiul etratopaur level associated with planetary Rosrb* vaves in the vinter baispberer.

N~lleriulsimulations of the semiannual oscillation in the equ~torialmiddle atmosphere have been made by global adels (Bolton and Wehrkin, 198)a. 198)b; Hahiman uid Sinclair, 1980).

(c) Upper llcscspheric Waves

Regarding the dymmics of the equatorial upper mesosphere .ad lwer thexmorphere, houaer, very little is known about the lyture of waves and their inter-relation to the raa flow.

Recent progress in VBF radar okrvrtions made it possible to obtain rsospberic wind velocities. From continuous observations at Jicuru (12s) md Arecibo (18~)~aidence of the by-to-d~v variation of mesospheric winds in the height rmge of 60-90 b has be- obtained fra a speck1 observation p13gr1 by the Kyoto Uoiversity group .nd the Hu-Planck Institute group (FuL.0 et al., 1980; Birota et al., 1982; Pottger et al., 1982). This wind variation bs a characteristic tir scale of about 5 &ys or w, and is considered to be due to the p~cnge of travelling planetary Rossby waver.

Ibrtorer, a simultmeous observational progrr at Jicuru and Arecibo was carried out by the two groups in Ilwaber 1981. and the data obtlined are currclltly under investigation.

(dl Gravity Waves

The momentum dissipation by -11-scale wtions is also a very important mechanism for the pcm flat variation in the tropics as well as in middle and higher laritudes. In particular, upward-propagating gravity waves are consider-d to plap an important role in the long-term variation of the wan +om1 flw in the mesosphere.

Recently, theoretical development on this probls h.6 been m~deby several authors (Lindzen, 1981 ; Xatsuno, 1982 ; Bolton, 1982 ; Dunkerton, 1982). Rerults of these studies strongly suggest the nced for the delineation of global and rasoml morphology of gravity wave Podes in the middle atmosphere. Only fragmental evidence for the predominance of short-period wind fluctuation has been obtained from the VBF radar observations, in relatior! to the me= zonal vind and its vertical shear (Bottger et al., 1981; Iirrota et al., 1982).

YDitKS80P ON EQUATORIAL WIDDLE ARlOSPEERE IEASUREHEttTS AND MDDLE A~SWEBERADARS

As var mentioned above, for the purpose of studying the dynamics of equatarial waves, further observations are needed, and the newly cmergirg middle atmosphere radar tect-nique would be very premising for the peasuramt of winds and waves.

In this connection, a workshop was held in Hay 1982, as a part of the P18-2 activity, under the sponsorship of MAP. The goal of this workshop was to improve our knowledge of the equatorial middle atmosphere dy-ica and measurement techniques. and subsequently to develop proper methods to obtain useful data for the study of out- standing problems. huiag the period of Pi@ (1978-19811, some signifiunt improvsento hne bem obtained in both theories and obervationi of .he dynsmics of the equatorial riddle atmosphere. Ccmwquently, problaz to be studied in the mar future becre wre definite. In addition, reccnt progress in obeerring techniques such aa tSI radars and satellite limb infrared wuuraents has allaued the detailed structure of various wave modes to be imestigated both in space md ti-.

Therefore, although PIIP-2 does no longer continue, the study on the eqcutaial wave dymiu will be extensively continued during the period of nu'.

Fi~lly,it is aphasized that mny efforts have to be made inter ~tiomllyon mlysia, exchmge and archiving of data.

thmkerton, T. (1979). J. Amos. Sci., 36, 32-41.

Dtmkerton, T, (1982). J. Amos. Sci., (to be published).

FoLao, S. et al. (1980). J. Ceophys. Res.. 85, 1955-1957.

Birota, I. (19781. J. Amos. Sci., 35. 714-722.

Eirota, I. (19791, J. hhos. Sci., 36, 217-222.

Eirota, I. (19811, Paper presented at the 3rd TMM Assembly. Hmburg.

Hirota, I. et a1. (1982). (to be published).

Boltar, J. R. (19821, J. Amos. Sci., (to be published).

tlolton, J. R. and Y. I(. Vehrbein (1980a), Pure and Appl. Geophys. 118, 284-306.

Bolton, J. R. and W. W. Vdrrbein (1980b). J. Amos. Sci., 37. 1968-1983.

Lindzem, R. S. (19811. J. Geophys. Res., 86. 9707-9714.

Ilrhl~n,J. D. and R. W. Sinclair (19801, Paper presented at the 17th IUGG Assembly, Canberra.

Matsu~lo, T. (19821, J. Keteor Soc. Japan. (to be published). Rottger, J. rt a1. (19811, J. Atmos. Terr. Phys., 43. 789-800.

Rottger, J. et rl. (19821, (to be published). 1M;-7: ArnSPIIERIC PENETRATION OF SOLAR UADIATION Ih' mE WEOF SCHUlWN-RUNCE BANDS

J. E. Frederick

In recent yeus there have beg ujor effort* in measuring the extraterrestrial wlar irradimce for ur in atmospheric studies vell as in photochemical dels. The quantity of iudiate relwance to theoretical studies is the muber of photons vhich reach a given altitude in the middle atmosphere. Current dels ccnpute the attenuated radiation field but the cross sections available for the ujor absorbers, OZ .ad 03, often colc fra experiments that are nw quite old. Solar ~rradiroce~casaraents ude in the middle atmosphere un provide a check on the ulculations. Ewwer, there has been relatively little work done tward mking in situ observations of the attenuated irradiance even though this quantity is the fuudoental driver of photochaiul processes.

Balloon rasurementa 6hw sac signifiunt differerces betveen the predicted and observed ultraviolet radiation field betvea! 30 rod 60 Lm. Such discrepancies vere reported as early as 1965. In addition. it is nav videly recognized that the radiation field which results from Rayleigh scattering and reflection from the ground and cloud. is 8 significant factor in the dissociation of weakly bound polyataic gacea. Yet the vay thew procesrs are included in calculations varies from one modeling group to another.

The wavelength region tc be studied by the Study Group includes Lyman alpha plus the rmge 175 nm to the visible. Specific topics to be addressed include:

(1) Om present mderstanding of the cross aections of the ujor absorbers, O; md 4. This vould include the Schum8nlrRuuge bands as a subset.

(2) Caparison of in situ reasuraents of the attenuated radiation field vith calculations.

(3) The relewance of the scattered and reflected radiation f ields on riddle atmospheric procecrs. WORKSHOP ON COMPARISON OF DATA AND DERIVED DYNAIIICAL QUANTITIES DURING NORTHERN HEHISPHERE (PW-1) YIhTERS

J. C. Gille and K. Labitzke

The vorkshop vas held at the Natio-1 Center for Atmospheric Research (NCAR) in Ba-lder. Colorado from 11-14 Hay. 1982. Approxi- mately 20 scientists from the Federal Republic of Germany, France, Japan, the United Kingda, and the United States attended. The list of attendees is included as Appendix 1.

The purposes of the workshop were the intercomparisons of the basic meteorological variables taperature and geopotential height, and the quantities derived from them for application to stratospheric dynamics. The data for comparison were those fron conveutioual sources (radio- sondes and rockets), the Limb Infrared bitor of the Stratosphere (LIk6) and the Stratosphere and Kerosphere Sounder (S1L)6), which £1- on Nimbus 7; the Stratospheric Sounding Unit (SSJ), and data from the U.S. National Meteorological Center (NnC) fra NOM 5 and TIROS ti Sounders (including SSU). For the satellite inetrmnts, of course, the tenperature and height are themselves derived from radiance aeasure ments.

Data from the winters 1978-79 through 1981-82 vere discussed, but most attention was devoted to days during the winter of 1978-1979, the first of the PW-1 winters, and the only cne for vhich LIB data are available. For other systems this period is not necessarily typical of rzsults to be expected at later times, due to changes in the instruments and analysis methods.

In order to cover the range of situations in the atmosphere, .n earlier decision had been made to concentrate op one day believed to be relatively undisturbed. 2 January, and two strongly disturbed days, 26 Jaf~uaryand 26 February, a11 in 1979. Participants vere requested to bring maps and croes sections of tenperaturee, height, zonally averaged winds, wave 1 and 2 amplitudes and phases, heat transports, mmentum transports, and Eliassen-Palm fluxes.

The agenda for the meeting is attached as Appendix 2. The participants responsible for data production brought most of the re- quested information. During the first day, there was a general back- ground discussion of the experiments, including methods of data reduction and analysis. In the follwing days, the data were posted, and all participants had the chance to compare and discuss the different data products. For some cases numerical differences were available. In general, the participants vere pleasantly surprised by the agreement between the data products resulting from the different experil~nts. As had been expected. the agreement tended to be better for undisturbed situations than for disturbed days and locations. Sae local differences were larger than desired, especially for disturbed days. The w-xkshop focused on the identification of problas, in order to provide guidance for future work to improve ~~e results, and reduce or at least understand the differences. Discussions of the data and of some particular comparisons are presented belw.

DESCRIPrlON OF DATA

hppcd products of temperature and height based on convcntioml radiosonde eeasurments vere available fra the Nations1 ntteorologiul Center (NW) of the U.S. and the Free University of Berlin. The latter are subjective analyses at 50, 30 and 10 sb, in the Northern Beisphere. The Nm: maps at 100 rb use conventioml &ta (with satellite data wer the oceans) in an optimal interpolation analysis schcre. At 70, 50, 30 and 10 rb, Rm: rarlyses use only conventions1 data in a Cresnan type successive approximtion analysis.

The NU-5 Vertical Tmprature Profile Radiometer (VTPR) and the TIROS N Stratospheric Sounding Unit (SSO) are ludir vieving IR sounders which provided data for NHC maps above 10 mb. Before 23 February. rpirical regression coefficients were used to derive tmperature and thiclrress from the outputs of the two VTPR chmnels with the highest altitude weighting functions.

The SSU is a pressure modulated IR radiometer. For the winter of 1979, radiances were available for retrieval only from ch.nnels peaking at 15 and 5 mb; information from an additional. higher, lwel is avail- able from later instrwieets. Mter 25 February, readings from the SSU channels were uoed with calculated regression coefficients to give t-perature and thickness. In 1979 neither set of coefficients was stratified by latitude or season.

The British lleteorological Office. which furnished the SSU, also determined the thickness betwem 100 ob and rveral higher lwels by regressing them on the radiance. The regression coefficients also did not vary vith latitude or season for the period in question; this modification was introduced in June 1979.

The LI?S is a limb scanning IR radicmeter, which flew on Nimbus 7 and provided temperatures from 100 to 0.05 mb. Radiation emitted by the 15 um bands of C02 ia measured in 2 spectral channels, from which the tmperature was inferred as a function of pressure, using an iterative retrieval scheme. The vertical field of view (FOV) is 2 km, leading to high vertical reeolution. The thickness between standard pressure lwelc vaa calculated, and added to the NEK: 50 mb height to give height fields. The analysis uoed a Kalaan-filter on data around latitude circler. Thin is being further refined. The ulm of detectors cooled by a solid cryogen limited itr life to 7 montha.

SIUCS is another IR limb scanning radimeter on Nimbus 7. Tempera- ture is derived as a furction of presmure from measurements of 15 um radiance. along the orbital track using a recurrive estimation approach to determine 10 eigenfurctionr. The vertical FOV is 10 km. The taperatures and derived thiche8~sare Fourier-analyzed around latitude circler each day. Height8 vere built up from the SSU 20 mb height8 (aee below).

TmEATUXE COHPARISONS

(a) W-SSU Cqmrisons

There is general agrement betvem SSU radiances and simulated radiance8 derived from SAl6 taperature prof ilea. Where the difference^ are greater than 1 K in brightness temperature, they can be explained qualitatively by: time evolution of the field; data voids; and tides. It is expected that proper treatment of these three areas will reduce differences to less than 1 K everyvhere.

Caparisons of thicknesses from 100 mb show the same general features. The agreement in undisturbed regions is better than expected in view of the lack of information from both instruments between 100 mb and 20 mb.

(b) W-LIK Comparison

Further detailed numerical comparisons are required in this area, and vill be carried out in the near future. Qualitatively agreement is good, but differences are larger than SAUS-SSU. Differences may be consirtent vith the lower vertical resolution of Sm. Amplitudes of vaves are slightly maller from SAMS, but the locations of warm and cold areas agree well. In the zonal mean, LIK temperatures appear to be . slightly higher at the stratopause. A feature of mplitude 10 Y.which slopes steeply eastward is visible in LIB 26 January at 20N above 2 mb vhich is not apparent in Smdata. It may be of narrow vertical extent.

(c) SAIIS-LIP6 - Berlin Comparisons

In undisturbed regions where there is adequate radiosonde data, there is general agreement to within 3 or 4 K. In disturbed regions, agreement is better on 26 January than on 2 January or 26 February. This appears to be due to the systems sloping on the latter two days, vhile the phase of the wave is almost independent of height on 26 January. It seems likely that the retrieval or analysis methods are causing the wave to be shifted in height or in latitude. Both SAW and LIM have the warm center a few degrees further north than the Berlin analysis on 2 January. The problem may be one of vertical and/or horizontal resolution in the retrieval and/or analysis.

Quantitative comparisons are complicated by the chanle by NllC from the NOAA 5 VTPR to the TIROS N SSU in February 1979. Initial cow parisons show LIS agreeing in the mean with NMC to 1.22' from 100 to sl mb. Map features are in generally good agreement. Ac 10 mb, where the NMC analysis uses only radiosondes. large differences occur over the oceans.

HEIGHT ANALYSIS

The agreement between analyses was found to be generally very good, only the very demanding situation of 26 February showing large differ ences, vith those limited mainly to the upper stratosphere. Maxim and minima usually agreed to within 10-20 decameters. The representation of gradients has yet to be evaluated quantitatively. Charts appeared generally similar, though thare were signs that the extent of smoothing used in satellite analysis may benefit from further study. Sane very localized errors were found to be associated with gaps in data coverage, which could lead to incorrect features in the flow.

Even in the worst case, February 26, the serious differences were limited to the region of intense warming.

The range of 1 mb heights in the warn pool was rather large, the highest being the SSU analysis and the lowest NHC, with SAW and LIH close together in between. The high SSU value is largely a consequence of the lack of channel 17 data in the upper levels so that the high temperature below is extrapolated upwards. The values were in order of the depth of their weighting functions. This explanation is consistent also with the observed sharp drop in the intensity of the temperature maximum with height in the upper stratosphere and lower mesosphere. The reason for the iarge difference between the NMC and SSU analysis is not clear, since they both use SSU observations (but with very different retrieval and analysis procedures).

COMPARISON OF DAILY ZONAL WINDS

For January 2, the zonally averaged zonal wind (Ti) derived from SAMS, SSU, LIMS and NMC data generally agree well over most regions except at the top level around 0.4 mb and 26'N where the LIM results are apparently greater than those from SAMS and SSU (but in agreement with nearby rocket measuranent winds).

On January 26. ii derived from SAYS and SSU generally agree within 5m/sec although larger differences are present in the region of the jet core. The values of ii calculated using SNS, SSU, NllC and LIltS data are reasonably cloee in the middle latitude regions, but differ in polar and subtropical regions. The stratospheric jet in the NHC data spreads over a wider area than in the LIP6 results.

Again on February 26, in the middle latitude regions agreement mong SAUS, SSU, and LIHS was reasonably good, but there were differences in ii in high and low latitudes. The LIE and SSU analyse~ tend to yield somewhat different positions for the zero wind line and region of easterlies in the tropics.

WAVE WLITUDE AND PWE FOR TEMPERATURE AND GEOPOTENTIAL HEIGHT

A comparison of the clmplitude and phase distributions of planetary waves 1 and 2 in the Northern Hemisphere stratosphere was carried out for the 3 days. No distributions of the wave mplitudes and phases were available from the SAM data. The comparison was thus primarily limited to the LIltS and SSU data. Sane conventional information was also avail- able for the 50 and 30 mb levels from the Berlin group.

The comparison of the wave I and 2 ampli~udedistributions from the LIWS and SSU data showed good agreement with regard to the height of the amximum wave mplitude. The latitudinal position of the maximum wave 1 amplitude also agreed quite well. The LIWS an3 SSU wave amplitude and phase distribution were similar for the days in question, except that the LIES maximum wave 2 amplitude was situated somewhat farther north. The sensitivity of heat and momentum transports to the phase and &iplitude structure is such that detailed quantitative comparisons are necessary to get meaningful results.

On 26 January, a difference of 300 gpm was present between the maximum wave 1 amplitude values for the LIW acd SSU data while a difference of 50 gpm was present in the same type of comparison for wave 2. In each case, the LIWS wave clmplitudes were larger than the SSU amplitudes, possibly resulting from its higher vertical resolution. These differences amounted to only 1C-15% of the wave mplitudei.

ELIAS SEN-PALM FLUXES, HEAT AND HOMENTUM TRANSPORTS

Comparison of the Eliassen-Palm (EP) f luxds were made for two days during the period of the minor warming of January 1979. At the height of the warming of January 26, SSU and LINS data were in good agreement regarding the direction of the fluxes, both showing upward directed fluxes from the troposphere, strongly curved equatorward in the middle stratosphere, presumably due to the effect of the zero wind line. On January 22, the direction of the fluxes were also in qualitative agree- ment, showing strong upward propagation to the upper stratosphere. In comparison, however, there were noticeable differences in the magnitudes of the divergences of the EP flux. Differences were apparent between two independent analyses of the LIMS data for January 22, one showing a region of divergence around 60N extending from I mb down to 10 mb which was observed neither in the second LIP6 analysis nor in the SSU data. The differences between the two LIP6 results appear to be associated with the data editing and analysis procedures, and resulted in different high latitude momentum fluxes, rather than significantly different heat fluxes.

On February 26, there wae also an appreciable difference in high latitude momentum fluxes between LIMS and SSU data in the l,,*.er strato- sphere, again apparently associated with the LIMS analysis. In this instance the Berlin analysis agreed well with the SSU values, both showing negative momentum fla:xes in high latitudes. In view of the large geopotential amplitudes associated with warnings, only small phase grsdients were necessary to explain the observed fluxes.

In conclusion, it was felt that these diagnostics have highlighted c!;sracteristics of the different analyses which may need further at tention. Additional work should improve the particularly sensitive f ratures of such analyses.

CitNCLUS IONS

The quality of the data from all these sources is generally good. especially when one notes that the disturbed and difficult conditions that were chosen severei; test the observing systems. The basic fields of taperacure and height, based on these comparisons, are believed to be correct for the most part. Problem areas have been noted. Improve- ments are possible in a number of cases. For the derived quantities, it is necessary to be especially careful when taking derivatives of quantities in these basic f ields, especially derivatives higher than the f irst.

The participants agreed that this workshop had been useful in identifying problems, and areas of concern. Preliminary plans were made to resolve problems which were identified here, and understand those differences among them. It was felt that this workshop had served as a beginning, not as an end to the data comparison. In order to complete a more quantitative comparison of the agreed upon data, plans were made to hold a second workshop in the spring of 1983, probably in Oxford. As part of the i-eparations for siach a meeting, the data producers agreed on additional days to intercomparc, hnd to a complete exchange of c~mparisondata, on magnetic tape, before that time. At the second meeting, greater emphasis will be placed on understanding the meaning of th~data, and understanding the physics of the stratoepheric winter disturbances. Preli~inaryplans were formulated for Q final meeting, to be held in Hamburg at a time close to the IUGG meeting, to complete the data comparison, but to focus much more strongly on the understanding of stratospheric winter phenomena. APPENDIX 1

W3R!!SHOP ON COWARISOH OF DATA Ah'D DERIVED DYNAKICAL QUM'TITIES DL'RING NORTHERN HEMISPtl'iRE WINTERS (PIIP-1 WINTERS)

11-16 Aay 1982 Boulder, Colorado

U.-L. Cb.iin France

S. A. Clough United Kingdom

F. G. Finger USA

R. R. Garcia ISA

K. A. Gel la ' USA

Y. L. Grose USA

D. L. Bartrrann USA

A. Hauchecorne France

I. Brrota Japa

J. R. Eolton USA

W. J. Fohri USA

R. Labitzke FRG

R. Madden USA

J. D. Ilahlman CSA

T. Xatsuno Japan

T. N. Palmer USA

K. Petzoldt FRG

C. D. Rodgers United Xingdm

H.-F. Wu USA APPELDIX 2

PROPOSED AGMM

UOkKSHCP ON DATA COZfPARISaR AND DERIVED DYNAUICAL QUUrrITIES WRING NORTHEW KEUISPtlLRE UIh;TEBS (1978-1982)

South Doon Roaa ! -tiom1 Center for Atmospheric Research Boulder, Colorado USA 11-14 my 1982

Tuesday. 11 My

Topic Lead Discuaunt

An Introductory Ruiarks Cille Goals of the Workshop hbitzle. Gillc Data Requirauents for Observation Studies Itadden Conventioual Data Petzoldt FWand TIROS X Satelliter Finger

??! Description and Evaluation of the Data Types and kulyws

LIS (Limb Infrared Hmitor of the Stra:osphere) Gille SAM (Stratospheric and Mesospheric Sounder) Rodgerr SSU (Stratcspheric Sounding Unit Clough Lidar Sounding of the Aaosphere Hauchecorne Data Requirement- for Theoretical Studies Eol t on

Wednesday. 12 Hay

AH and PK Tmperature and Height Field Cmparisons Wave 1 and 2 Amplitude and Phaee, for Temperature and Eeigat

Thursday. 13 llry

An Wenturn Trtnsports

PU Heat Transports

Friday. 14 I(ry

A EP Fluxes and Other Derived Quantities

PU Concluding Discuesionr Whsr has been learned. What ate the courses for future action. WMKSEOP 011 EQUAl'oRIbC MIDDLE A'I1IDSPE€EE WUPEEU'ZS ME MIDDLE LRlDSPBePE EAMBS

The Yorbhop was held to effect a clor interaction rong theorias, rodellerr, LsT- md Sf-radar scientists and other erperi- muter. working on the uddle aCI.osphere. The Workshop determined the required obrrratioas, baoed on recent progress in middle atrospbere research. llST and ST radars now cmder constroction, or in design and planni- stages, were described. Thpresent report presents the vori- shop pgrr, a mqof each rssion, ad edited versions of two purcl discussions.

The convenors acbovledge the excellart arrangaents of the meeting by Local Arrangements co-chumen, Drr. 1. E. Vdandt and B. B. bl sley, IWMb, Boulder. Tbe convenors' thanks are duc to variouo co-sponsoring organizations including SCO-EP, COSPAR, IAGA, W and UBSI. Session 1. DYNAMICS: TaEOPIES MDI(DDEL!i

Chairun -3 Reporter, first half-wssicn: I. Birota, Kyoto University. Kyoto Chi- odReportc . rcond half-session: J. M. Forbes, Boston College. Cbestmt Bill

J. If. Forks end 9. S. Lindzm, Waves in the equrtori.1 rsosphere: Theories and obwxvftio~lneeds (invited review).

Contributions by, inter alios: P. S. Lindzm and J. H. Forbes, &sospheric turhrlcnce. 1. J. hmkertm, Gravity waves .nd ilcrtial inntability. M. L. Salby, krul features wer the equator: prospects far observations and idcntifiucion. L. Coy. A slwly varying model of gravity vavw.n flaw inter action in a colpressible atrocpberc. I. E. VmZmdt, A univerul spectrum of buoyancy waves in the lover riddle abosphere.

Session 2. OBSERVATIONAL ILESULTS I

Chirun, first half-session (A): ?I.A. Geller Reporter: L. Coy, University of Wasliington, Seattle Chairun. second half-session (0): J. K. Cho Reporter: J. Eovtger, IIu Plmck Institute, Lindau

P. L. Bailey md 3. C. Gille, Satellite data reduction .nd the obsercation of middle atmosphere waves (invited review).

Contributions by, inter alios: R'.. L. Salby, D. Iiutunn. P. L. Bailey, and J. C. Gille. Evidence for quatorial Kelvin modes in limbus-7 LIlS. K. S. Gage, Obse~edvariability of the tropical tropopause. If.-L. Chnin. Lidar results in middle atsmosphere dynamics at middle Latitudes. M. Petitdidier md R. Woodun. A Cree's function simulation of a stratospheric 30qinute period wave packet. P. Czechowsky. R. Rottger, R. Buster and G. Schmidt, Implications for middle atmosphere research deduced from YtlF radar ~bse~ationsat tbe Arecibo Observatory. R. A. Vincent, The use of multibem Doppler radars to study gravity wave monentum fluxes. Tuesday, 11 1I.y 1982

Session 3, OBSERVATIOIAL BFSULT- I?

Chirun, first hlf-raaioo: J. Bottger Ctuiraaa, second half-=scion: k-L. Chnin Reporter: B. B. Balsley. IIIM, boulder

8. B. lklsley, Ovexvieu of PST obsen8tionrl capabilities (iavited reviev)

Cmtr itutions by, inter alios: R. If. Wad, P. Kr Rastogi, B. J. Yatkins. and G. B. 'Loriot, Radar evidence for #in turbulent structures in tropo-ctratospkre at Hillstoot Bill. U. K. Hocking, t?n the extraction of turbulence parmeterr Era power spectra wascred by radar. J. Buat md F. Bertin, In situ mersurcrtnts in stratospheric turb~lentlayers. K. S. Gage. HST radar detectioa of tropopauee height. 3. Rottger, KSi radar investigations applying spaced anteno. techniques (invited revicv). J. Rottger .od C. E, Meek, A detailed arulysis of wind velocity data deduced vith the spaced antatm drift method.

Panel Discussion: Is there aced for a middle atmosphere radar facility in equacori.1 latitudes? Wabers: S. Kato (Chaixun), B. 1. 'Ialeley. J. H. Forbes. K. S. Gage aad I. Birota

Session 4. ST BAMRS, PWtED OR mFDEP WNSTRUCTIQI

Chiman: B. B. Balsley Reporter: S. Fukao, Kyoto University, Kyoto

S. Xato, ?be Hu Radar under construction at Shigaraki, lapan (invited review) S. Fukm and S. Kato, radar system: and its antenna design [invited review) R. A. Vincent, The Adelaide ST radar (invited review) S. A. Bouhill, A proposed large HST radar for middle latitudes (invited review) A. P. Fitra, Tbe Indian PST radar (invited reviev) J. Brosnrhau, Thr Chmg Li radar in Taiwan Session 5. SAUR IEtlUllQUES

Cbtirun, first half-seasion: R. A. Viaccn~ Cluiw, second half-ration: R. F. Uoodvn Reporter: E. T. Farlcy. Cornell University. Ithau

D. T. Farlcy, Revieu of ST radar probing techniques (invited revieu) it. F. Woodun. On-line sigarl processing for ST radars (inoited reviev)

Cmtribations by, inter alios: S. A. Bowhill, A fast integrating preprocessor for a cohercot- scatter radar qsta. S. A. Bowhill, Interactive microcomputer systss for radar control ad data acquisition using the FOPM language. G. 1). brio+, and it. 8. Wand, frplsentation of phasecoding for ST obse~etionsat Millaome Hi11. K. Uakasugi, H, Hatsw. S. FuLso and S. &to, A amplscntary code equence for lLST radar observations. U. P. Sulzer ad P. Uoo&n, Optirkrtion of rsospkric obsexvations through llcv coding techniques. N. P. Sulzer ad R. Woodun, Quasi-uaplscntary coder: A ncv rct of phase codes for uratospkric radar P. K. hstogi and C. B. loriot, Practical spctral maeat estirtion for 1-elevation ST experimmts at Hillstone Bill. C. E. Ilcck, A real-tir iomspheric drift syste. C. Cornish, B. I, mlrley. D. T. Fuley and R. Voobn. Evidence for echoes fram the gap region.

Sersion 6. SU-Y

Cisaiman: S. A. -hill Reporter: 1. G. Roper, Georgia Iostitute of Technology, Atlanta

P. C. Roper. 98F radarr as meteor vind radarr .nd the SCOSTEP GLOBaT (Globs1 Hetcor Observations) (invited rcricv).

Pmel Discussion: The Future of Middle Amospbere Radar hbtrs: S. A. Bowhill (Chairman), D. T. Fatlcy, K. S. Gage, J. Rottger. R. A. Vioceat .nd R. F. Wwdrrn SESSION REPORTS

SESSION I. DYNAMICS: THEORIES AKD tQDELS

WAVES IN TEE EQUATORIAL M5SOSPtiERE: THEGRIES M'D OBSERVATIONAL YEEDS

J. H. Forbes and R. S. Lindzen

S-rr. Current knwledge of mesospheric gravit )--type saves at equatorial latitudes is revieved with a viev towards evaluating the possible contrib~tionsof an equatorial WK radar. Based on theoretical considerations. diurnal series of rocket launchings. and radar measursents, diurnal propagating tides and especially the gravest svtric (1.1) rode vith 28 h vertical vavelength, are antiripated to be especully prominent in the equatorial mtsosphere. SEMAT oersuramts of coluon H20 densities suggest the posscbility of noaxmigrating as well as asy~lctricdiunul propagating modes being excited, +ith vertiul vavelmgths in the 20 km to 60 Iis range. Recently, geograptiully mtricradars at Kyoto (35.N) and Adelaide (35's) have delineated strongly asyrmtric tidal behavicr about che equator in both diurrul and semidiurnal components, betveen 80 and 100 h altitude. For eigtnsolutions of Laplace's tidal equation (vhich may be distorted uuder actual conditions due to background vinds .zld meridiorul t-perature gradie~ts).asytnmtric tides are characterized by nonzero !i-S velccities and zero E-U velocities at the equator, whereas the reverse is true for smtric components. An equatorial IcST radar could, theref ore, contribute signif iuntly to the dewnvolut ion of tidal structures in the eiddle atmosphere.

On theoretical grounds it is expected that the (1.1) mode is upable of producing signifrunt turbulence via nonlinear cascade or convective instability mctunins, and a rean easterly equatorial jet (= 50 1 sec-1) peaking near 105 h aue to mcmentum deposition in the region vhere the tid+ is dissipated. An equatorial radar would, therefore, also provide the opportunity to observe the important middle atlospbcre pracesses of vave-mean flow interaction and wave/turhlence colrpling for a known wave forcing. As these phencmena primarily occur above 75 ks, it is imperative that measurements extend as far into the lwer themosphere as possible, preferably to 105 bp. Consequently, placement of such a radar must avoid possible interference by the equatorial electrojet.

Required system constraints including altitude and local time coverage, time and heiubt resolutions, etc. are outlined. It is also emphasized that placement of the radar must consider the availability of pcsospheric sounders at other latitudes vithin the same longitude sector. Discussion

R. Wooban: (Ref. to measurements of tides at Natal and iiourou as compared to theory! There appear to be large phase discrepancies, as much as 180.. betr-ren the node1 and data at the lwer heights (30-60 'k).

J. Forbes: Yes. Bwever, these phases correspond to very aall ~plitudesand are not really of any consequence.

S. Bowhill: One can see the mpiitudes are belw the noise level, and the phase doesn't mean anythicg at those altitudes. Ubt limitation is involved in obtai~inga diurnal tide from 12 burs of data?

J. Forbes: One cacnot extract a diurnal ~idefrw 12 hours of real data.

S. Bouhill: Tvelve hours is typical for ai HST radar.

J. Forbes: Using meteor radar observations, one could possibly obtait 24 hours of data vithin the 80 to 100 Im hcight region.

S. Bouhill: If i~desin that height region are of interesr, then a meteor radar vould be satisfactory.

R. Roper: I object to the practice of plotting turbulence intensities less than local diffusion values.

J. Forbes: My co-nts vith regard to this topic pertain to the mesospheric region vhere turbulence values are greater.

D. Farley: Jiclaarca is not shorn on the map of mesospheric tidal observation stations.

J. Forbes: I umitted Jicearca since the radar observes only 12 hours of the day in the ~esosphericregion. The other sites are mainly meteor radars or partial reflection drift radars.

Sunmary. It is generally recognized that as internal gravity vaves reach aplitudes for vhich they are unstable, they vill break down, generating turbulence sufficient to inhibit further grovth. This has been hypothesized to be a major Murce of vsospheric turbulence. The possibility that cuch waves right gcocrate turbulence at smaller rplitudes, via a cascade of energy fram stable waves to waves of aaller uale vhich eventually go mstable, is investigated here. An iterative technique is utilized whereb a converged intenully consistcot solution is obtained for a wave vhich fed. upon itaelf. Porrulas are derived for the breaking scale md result~ngeddy diffusion coefficient, and urple siulationa presented for the (1.1) diurnal propagating tide. In addition, tw characteristiu of this uchania are noted which may be menable to obwrvations: (1) Internal waves are cbxacterizr~bv horizontal scales wh;ch are ruch larger than vertical scales, wbcr. or convective instabilities horizontal and vertiul scales are r ~ble. Thus, as one obsenes amller and auller vertical cca ne should begin to rea breakdown in horizontal coherence as the unstable uale is approached. (2) Similarly, convective elhents are generally asmciated with shorter tir scales thm are internal waves. Presuubly a tir-vertical spce spectral analyais could reveal such a transition.

Discussion

B. Base: Concerning the cascading of a wave, hw are different frequencies generated?

J. Forbes: It is hypothesized that the cascade occurs via some type of nonlinear interaction.

S. hhill: Hw is it different from the classical KelvirHelmholtz instability?

J. Forbes: First of all, it is assumed the prhry wave rmains stable. A cascade down to higher wave numbers is allowed and despite the reduced amplitudes (as specified by some power law), unstable tsperature gradieotr might be generated, and hence convective instability. In the Kelvin-Helmholtz case, there is a limiting wind shear beyond which instability and presumably turhlence is generated.

H. Tanaka: I believe the Kelvin-Helmholtz instability will occur before the convective instability.

T. VacZacdt: In the presence of a mean shear, perhaps.

S. Bowhill: Can this cascade occur in the absence of a shear?

J. Forbes: Yes. We don't consider the presence of s mean vind shear. D. Parley: These vaves are linear, yet saw nonlinearity -st exist to hea cascade.

J. Farbe.: Yes. The nonlinear uacade does not preclude the p~imq vave, feeding energy at scme lw vave number, ft-m being linear md stable.

S. Bwhill: Is it fair to characterize the model as beginning with a tidal structure vith certain A,, vhich gives rise to a shear vhich un then induce ao instability?

5. Forbes: !to. In our del the prhry wave can generate turbulence wen at stable aplitudes via the cascade process.

R. Woodun: Steepening of a vave is one vay of generating higher harmonics vithout instabil ilty.

S. Bouhill: Do these higher haxnonics that are generated have the effect of steepening a vave, or do they have the ef feet of being a random component that represents turbulence? I think there is a real difference between a high frequency vhich is coherent vith the origiual spatial frequency and one vhich is not.

J. Forbes: It is mot incoherent mtil the unstable scale (in the rave number spectrum) is reached.

S. Bowhill: It is in fact a steepening of a vave that we are wn- sidering, and not the generation of turbulence per se.

J. Forbes: In principle a finite mount of turbulence vill always be generated (in our model) at scme critical scale vhere 8 transition occurs betveeo coherence and noncoherence (turbulence). Whether this turbulence vill mount to anything depends on the prirary vave smplitude and scale, the background teaperature gradient, and on the assumed pover law.

T. VanZandt: Are these vertical vave numbzrs represented in the cascade pover law?

J. Forbes: Yes.

S. Bowhill: The pover Iav for steepening is not know.

3. Forbes: Yes. We errr~inedthe effect af varying the pover law as shown in the figure. S. Bowhill: Does the (1.1) tide generate miforr turbulence through- out this region?

J. Forbee: Only at the zeroth iteration in our model. The eddy diffusion coefficient is proportional to some 4wer of the wave temptrature gradient divided by the static stability.

S. Bowhill: This is normally not what is observed. The turbulence tends to concentrate in the regions of greatest st eepenirtg.

R. Woodman: Bawd on your model, vould you expect the turbulence to occur in thin layers or to be more homogeneously distributed?

J. Forbes: The viev in this particular calculation is that the distribution wmld be more kmogenecus. On the other hand, we have not attanpted to account for critical levels or diurnal variations.

S. Bwhill: This model provides one possible explanation for the 6-11 background turbulence which occurs in this region in addition to the very strong turbulence (a thousand times as strong) which occurs in very thin layers. It's very difficult to understand how shear can sustain turbulence throughout an entire volume.

Unidentified : In 1967 Lindzen suggested that breaking of the diurnal tide in the tropics is the primary mechanism for creating turbulence there. What's your view of the relative importance of this mechanism?

J. Forbes : This is an alternative view. In the present conf igur- ation it is not necessary for the tide to go lmstable in order to generate turbulence.

GRAVITY WAVES AND INERTIAL INSTABILITY

T. Dunkerton

Sununarr. Gravity waves (including Kelvin waves and tides) and their unstable breakdown is a topic closely intenwen with the inertial stability of the equatorial middle atmosphere. The enhanced diffusion associated with breaking waves would presumably stabilize the observed cross-equator ial mean wind shear. Without this enhanced dif i~sio.-.,one expects the atmosphere, as an essentially inviscid system, to exhibit inertial instability in the tropical winter mesosphere. Recent theoretical progress suggests that this instability may not necessarily be zomlly syumetric, and that it may be closely related to the Kelvin wave instability found by Boyd (1982, Jki).

At the same time, gravity WWe6 (including-Kelvin waves and tides) appear to provi& a plausible explanation of the t?sopause lleaknnual oscillation. The underlying concept is selective transmission, whereby vertically propagating waves are able to generate mean wind reversals at upper levels. In this case, the phase reversal in the total seniannual oscillation is explained by this concept. Considerably more obsema- tional vork will be required to assess this theory.

Fiuelly, there is new interest in the saturation mechanisms under- lying the unstable breakdown of equatorial Rossby-gravity vaves. It is plausible to invoke as many as three distinct candidates as possible sources of instability; the order of preference is inertial, barntropic. and static instability. By looking for regions of unstable breakdown in the observed Rossby-gravity wave in the lower stratosphere, it is con- ceivable that the mmer to this difficult question might be partly provided by radar observations.

Discussion

H. Salby: Uhat is the speed of the Kelvin wave which deposits westerly menturn in the mesopause region?

T. Dunkerton: Tte phase speed estimated from Dr. Hirota's paper is about 50 m scc-1.

B. Baloley: What is the altitude range where the inertial in- stability might occur?

T. Dtmkerton: The theoretical model has no vertical shear or vertical dependence. The greatest ehear occurs in the winter mesosphere.

Unidentified: What is a typical vertical scale?

T. Dunkerton: That's arbitrary and related to the viscosity. For typical shears, the scale is 1-2 km.

Unidentified: What latitude baud does the inertial instability span?

T. Dunkerton: It is confined to the tropical vinter mesosphere within 10" of the equator.

S. Bowhill: Do the westerlies and easterlies provide the forcing?

T. Drmkerton: The coriolis interaction auees a northerly flow to generate easterlies which then lead to more northerly motion.

S. Bowhill: If they are produced by the instabiliir, what is the source of energy?

T. Dunkerton: It's kinetic energy conversion from an initial linear shear to a cross-equatoxial sh~arleqding to the instability similar to Taylor's concentr ic cylinders.

R. Woodman: Are the east-west winds needcd to start the whole system?

S. Bovhill: Perhaps they are a corsequence of the instability. T. Dunkerton: It's a matter of semant, . One is the coneequence of the other. Cross-equatori. 1 advection may be thought of as the "first cause" by creating a cross-equatorial mean wind shear.

J. Mahlman: In my numerical modeling work I have not observed the inertial instability found by Hunt.

T. Dunkerton: Hunt's model shears were about twice as strong as the observed shears.

NOWFEATURES OVER THE EQUATOR: PROSPECTS FOR OSSERVATION AND IDENTIFICATION

M. L. Salby

Smry. Several planetary normal modes are expected to achieve large wind signals in the middle atmosphere wer the equator. Rossby- gravity mode amplitudes of wave numbers 1-3 increase rapidly in the upper stratosphare and mesosphere. A many-fold increase at mesospheric altitudes over surface values is predicted by linear calculations. The wind oscillations are predominantly rneridional over the tropics, maximizing near the equator. Propagation of these modes is westward at periods near 1.2, 1.6, and 2.1 days, respectively. Spatial and temporal characteristic8 of the latter are not inconsistent with features of the "2-day wave", (Rodgers acd Prata, 1981, JGR, 86, 9661).

In addition to the Rossby-gravity modes, the wave number 1 Kelvin normal mode also exhibits appreciable vertical growth in the presence of realistic winds. Propagation ir eastward at a period near 1.4 days, the wind perturbation being predominantly zonal and maximizing over the equator. Hotsuno (198G, JMSJ, 58, 281) has tentatively (eenrifi?' this mode in surface pressure fluctuations. Because these modes (1) propagate fast enough to grow vertically in the presence of realistic winds, (2) are quasi-free oecillaticnr, ar~d (3) are suf ficienrly removed in frequency from the "red" end of the spectruw, they have the potential for achieving 3tatirtically, significant signals in the middle atmosphere -- e:en if toLally masked by noise at the surface.

"Conventional" means of retrieving syno~ticfields from asynoptic satellite data cannot faithfully recqver ieaturos of s~chshort period. This leavea ground-based radar techniques as one of the few oceans cf obseming the phenomena. Simu1:aneous measureaents, however, will be vital in i4entifying these featurea. --Discussion A. Stanford: Plcnse comment further on the statement that present satellite observations cannot resolve 1-day period waves. Bow do you retrieve synoptic f eatures from asynoptic data?

H. Salby: Conventionally it has been done by some form of space- time correlation; and an aggregate of methods has been used, some of them statistical. There has beca uncertainty as to what frequencies and wave ntmbers are determinable. The majority of these methods usea to estimate synoptic fields strongly attenuate or filter the shorter periods or smaller scales. Basically, the short period waves cannot be recovered synoptically because they evolve (propagate) appreciably during the time (one day) it takes the satellite to encircle the globe.

A SLOdLY-VARYING HIEEL OF GRAVITY WAVE-MEAN =OW INTERACTION IN A COMPRESSIBLE ARK)SPHERE

L. Coy

Summary. The vertical propagation of an equatorial Kelvin wave is investigated by considering the init. 1 switch-on at a lower boundary of a two-dimensional internal gravity wave. Modulation equations have beeu developed for a single zonal harmonic which predict wave action, wave phase speed, and the mean zonal wind as functions of height and ti-. These equations are integrated numerically. The results show that the waves are capable of generating mean flows greater than the pt.sse speed of the wave forcing. Tile wave phase speed increases in the interior of the domain due to the accelerating mean flow. At present such accelerated waves have not yet been obssrved but may be relevant to theories of the quasi-biennial and semiannual oscillations. Discussion

Unidentified: Y&t is the phase sped of these Kelvin wmes?

I. Coy: M m we-1.

I. Birota: It is difficult to rmderstaud the physical rmbg of a switch-on dlin equatairl mcraa flw inter- action. In the equatorial region, there is a quasi- equilibriu. Yht is your interpretation?

L. Coy: If there is no sudden mitch-on, it makes it difficult to interpret this silple experhat in a physical way. I do think the rplitudes chage uuubt, so aae of these results uybe memingEul.

U. Schoekrl: Would - t mrize the rjor differences ktvte your model rd lhmkerton' s?

L. Coy: In his model the flw above is a descending ohear zooc which is liritd by the phue rpcd of the forcing wave. In ry model they can be larger.

J. Stanford: Vht is the tiw scale?

L. Coy: One unit is the tir to travel oiw vertical rule height at the linear group velocity. ¶'his is about 10 days far the Kelvin wme.

Surrr. Although power spectra of :he resosule fluctustions of vind and temperature in the troposphere md lower stratosphere Luve been available for uny years, there is no generally accepted dymmical explanation for them. In this work the power spectra of mS0S~8le fluctuations of the kritontal vind in the rmgc of frequencies from the inertial frequency (1 to 2 x cyclec/a in riddle latit~des)to the buoyancy frequency (4 x cis in the stratosphere) and in correrponding rrrges of horizontal and vertiul wme numbers are con- sidered. It is shown, first, that they exhibit a considerable 3egree of univermlity; that is, both the shape and the rplitude of the spectra tend to be independent of geographical location md season. It is then sham that the spectra cur bt described in ferns of a spectrum of gravity (or buoyuncy) waves, vhich is a slight modification of the universal spectrum introduced by Garrett md Hunk (1972, 1975) to describe the msoscale spectra in the ocean. The dynamical processes that right mintain a ~nirernlshap adrplitude are discusrd. Tbt irpliutions of * univerui spctru famiddle atrospkre dyaaics are explored.

Unidentified: In the oc-m the temporal spctru wuld be referred to intrinsic frequency. la the amspkre this couldn't possiL1) be since the wid sped is usually greater th.n or equal to the vme sped.

1. V8nZandt: It is puzzliog why the Garrett and ?hmk spectrum, which is applicable to the ocea where the doppler shift is ull, wrks r vell fathe a-spkere where the Qppler shifts are large.

Enidcntified: I lure reservations about applying consistency relations (rarios of spctra) to verify spcctral 1~s.10 cor paring intertul gravity raves. for instance, one right expect an equipsrtition of K.E. and P.E.. vkreas for geostrophic t~rbulcoceoac might erpct a ratio of 2 or 3. The observations may differ from both of these. In any case. I dcn'c- think they would k suf ficicntly differcnt to be conclusive.

T. Vdandt: kpariug asry spectstm or consistency relation is mot enough. One must evaluate all information avail- able, and take into acoomc the mnbcr of adjustabie par-etess and experiwatal errors.

Unidentified: Bued on the observations, ubt are the space ad tir scales for vhich this relation breaks &vo?

T. V.nf.ndt: In the horizontal vave number spectra thc largest scale to be dominated by gravity waves is 1000 h. spctra end before the smaller scales are reached. For the vertical rcales the buoy~cyvme model fits fra 4 h to 100 r vhtre the data end ana the model still fits very well tberc.

R. Wooban: Ctmcerniog the cut off at the Brunt-Vaisala frequency. it does not &a plausible if one considers the relatively large doppler s!-ifz occurring in the atmosphere.

R. Bottger: You mmtioncd that ve observed this peak in the spctrw when the vind velocities are low. I ude some inter- ferometer Peasureents vhich I will discuss taorrov, and found the horizontal phase speed of these vmes conpared to tke viod speed. Tb phw oped is much larger, r, ooe can dicregard the &oppler shift.

T. V.nZ.ndt: Vbt uas the pb.H sped?

I. Bottger: A facta of 5 or so larger.

I. VPZ.ndt: Ye Qn't Ls~lthe phUC relocity of tke vucs an- trihting to these coatirors spectra. l'& mes that are studied obserratiaully anros~ly dicrete vres vhicb are a nubclass of the camtin of vaes. my my not be typical.

1. tottger: It is my impression that the phase velocity of r me vbicb is very close to the Bnmt-Funla freqmcy is statiomq. It just stays there M a L md do# motion.

S. hubill: It is possible the cutoff that's okned is .ot due to the sitmstion there, kt at tbc point vbcre thc vsves vere first geaerated. At this point the wind relocity my bebeem quite a bit less. (kce the freqnency of the vsve is deteained, it propagate imto wias where the viwl velocity is greater ad it vill retain the .re taporal frequency. Iberefore, its relation- ship to the Brunt-Vunla freq-cy will rcruin the o# reyrdless of the doppler &if t.

Unidentified: It uy help to look for breaks in the 81- o; the spectrrr, uy at the Brmt-Vuula frequency or at the byocy scale length.

1. V.nZ.odt: In the vertical relocity spectra that I sbdthere isn't a break in slope bpt a snddea drop in acrm density by .n order of mgnitubc.

Y. Eckluud: Ue heeuined a number of vertical spctra in the stratosphere at Platteville .nd Alaska, ad befd the occurrence of a sharp break at the buoy-cy frequency to be the exception (about 12 of the uses) rather than the rule. The rest of the tir there is nc apprat trmrition. P. L. Bailey and J. C. Cille

P. L. Bailey described .ac of the characteristics of utellite btr- Surllite data hestable 8yreutic errors and a character- izable precision. Tie eorer.te is nearly global, includes both day and nht obrezvations, ad is capable of good vertical resolution- Tk taporal. 2-1 and vertical resolution of satellite data has appliutions in the study of atmospkric umes and such data have bea~ hirtaiully an irportmt roorce faploctary vnre studies.

hro vieuiq wthob beken a-dm mdir ad lid. Th ndir viesing gives better global coverage tban the limb vicviag hrt the limb view* has mncb better rertiul resolution. Bigh vertiul resolution is necesury for a#riq .or kportmt qrwstions about the riddle a*-oqbere, including or- trmsport.

fbc processing of utellite data was considered as a rries of steps: data collection, data rpping, calibratioa of the orbiting inurmemt, retr kval of geophysical parreters, object ire analysis. .nd the ulculation of derived quantities.

An iqortat part of the processiag of the Pirbus 7 Lbb Infrared lbaita of tbe Stratosphere (1116) inar~mtis the use of the th fiita sequential estirtion techuique. This technique represents the data field by 6 uwl baonics at each latitude of interest and gives prediction equations for the wave coefficients and the crmr of each coefficient. fhc coefficients sad their errors are updated each time a neu data point ia obtained. For a given data set the filter is applied both farvard and backward in tir and the tuo estirtes are cabined. Vbcn the filter was tested on nmnufactured data it was foplld to give very acaarate results falarge rpiitude statiomry waves but the aplitude was attesaated for vrres with high phrc speds.

Pcsults from LU6 -re illustrated in a latitude height section shoving v-• 1 rplitude and phue. and in component tir series sbouimg tagoral wave rplitude variations and ua~ephase propagation.

What vollld be a ck.racterimtic value of the US error in the taprature profiles? About 3-6. in the tropics and 5-6. in the polar latitudes. Can the vertiul resolution be increased at higher altitudes? Instrumeat noir limits the LIl6 on Xirbus 7. Interpretation of uuuraents at high latitudes becomes lare difficult due to the breakdoup of LTE.

ubt is the horizontal resolutien of LIS? The borizoatrl ueishting fuactioa is about 280 b.

H. L. Salby, 0. Eartuna, P. L- kiley and J. C. Gille

Kelvin waves are Immm to be m hport-t source of westerly -tor in the qoasi-himnial oscillation ad are believed to be irportot ia the who-1 oscillation. Two &ta umples trem the Ekks 7 LMvere euhdfa kirin wres. fbc first tir priod revealed on cutward raria wae 2 in the taprature field vith a period of about 7 days. Tbc rcod tir priod was 1- enough (60 bys) to all- a cjrplete spectral .nrlysis. fht data slmwed wave 1 vita periods of 6.7-8.6. aud 3.5-4.0 days and vae 2 with periods of b.0-7.5 aud 3.3-4.3 days. All unes were eastward propaetiq. Tbe rplitude structure of the differcat wave desvere .bpM as fuactioas of bright .od latitude. Thc vertical melengths wen estimted to be 10-32 and 41 h for the wave 1 rodcs .nd 7-13 and 10-32 h for the wne 2 rodc~. Tk fuc of lLST radar bta in the fllture would be belpful for detecti- shorter wavelemgth mades (if they exist) and in forriag a better synoptic picture.

Urge variations in the tropopaur bcig!bt are seen at ~idlatitudcs. Mort of the obsened vrrutions can be erplaimed by ridlatitude vesther systss and the amal cycle. Tbc -ma1 bight variations in the brtbem Baispkre ad Southern Bemisphere are mt of phase. Tropical ruin.onde &u were urd to obaerre the aumul cycle of the Pacific tropiul tropopauae. Tbe annual cycle vas f oaad to be ic phase tirough- out the tropics vith m rplitudc variation of about 1 h and vitb the mimiam beights occurring during the lorthem Baispbcre sr.

Results were shovn from a rodel calculation of the mnul cycle of the tropical tropopauw bcight wbich agreed well with the observations. Tb model related cb.lrges in tk bight of the tropopauw to changes in incoming aolar radiation. Tbe tropopauw bight would increase vith iacreaaed comectioa resulting fra high sea surface temperatures. An important part of the IIIU.~cycle in tbe Me1 ames from the anmu1 variatioo io the Sem-Iuth distaoce.

Intermma? variability of the tropiul tropopaur height vas shun fra 1953-1%9 alag the Zurich saspot mmkr. The twcarves appeared to be vell correlated.

Saw results vae vbich illustrated the potatial of the Lidar technique to study rbort-texm variations in the atmolpbcre. Ik techoiqw ruored luer bcbcrtter fra vhich tapramre profiles cao be constracted io tbc 3065 h region,

A11 the tapratare profiles .krta short-tar variations frol 30 umces to 2 boars. Spctral ulysis gave vertical melagths fra 3 to 9 h vie aly the 1-r 6 to 9 h wavelegths appuiog in s-r. Other thm tbe tides, vhich dorrcd up at 12- mmd 24-r periods wst of the pver vas from periods of 2.54 bars.

10 ttis paper art-period grrity wue events obsened vith the 43- radar at Arecibo uere described md rodcl ulculatiop. vere preseoted to explaio the obsenatiors. I'k characteristics of the mat vere a quasi-siaasoid.1 ocillatioo 0,' the zomI viod of aht 20 mio period aod 34ms-l rplitude io the altitude regioo ktwcm 12 aod 15 h. fbc kginaiog of the event vas ehrabaized by ao hpulrlike trmsitay variatxon; in the altitudes lacr th.n 11 h the period of oscillatioo was abaat 30 uoates,

fbc classic equatioo of ynit-• propa~.tionio the preseoce of a source was mlved to determiOC the Creeo's frmctioo. The height variation of this fmctioo abwe the source vas ulculated aod it vas shcm that the event c~ k rcparated ioto a tr-sitay aod ao oscillatiog prt. mreu the trmsitory part vu very similar md occarriog exactly at the .m tir at each altitude, the gravity-vme oscil?atioos rfta a vhile chmged io different altitudes md vere oot obwnable at the laver btifits. Hot only ti- variatioos bat also spatial variations of the source (e.8. ~~rscloud activity) sere included in the model. It was .boM that aoc uonot observe .ny variatiaas after the tr-sitay part if the equivalmt baoy~cyfrr quency wc = wg.zlR (z = altitude above the source, oad P = distance from the wro to the obaerration region) is aat of the range of the oource apctrm.

The capaations vere urried out for m isotherul atmosphere ad no background vind vhicb my aca~untfor minor differeuces betveen obrrwatioml and cap\tatioml results. It was pointed out that this vthod to amme the atmosphere nsponr to o hpulrrlike source may be less problematic lad rore realistic than the approach applying the dispersion relation to a single wave event. This type of vat, cam- bining rabr observations witb Ddel calculationa, can be regarded as a w.t valuable approach to rmderstoading source rcbirsof gravity waves .

IWLICATIOIS OF HIDDIE mSPSERE lFSLIUCB DEDUCED FPOH VBF RAMB OSEXVATIOIIS AT TBE ARLILECIBO OBSERVATORY

This paper reported preliminary results from se~eralexperirntal upaignz urried out in 1980 and 1981 at the Arecibo Observatory *re a transportable 30+Y/120-kY VHP radar of the X.x-Plauck-Institut fur kronaie was operated vith the large Ancibo dish antenm. Using a best bight resolution of 300 r, it was possible to investigete in detail mesospheric turhrleuce itructures. It is evident that different layer types occur in the lwer md the upper rsosphere. Ybcreas the layers at altitudes lwer than 75-8U h are stratified (deduced from a considerable aspect sensitivity), thin and lri~ted,the layers above 80 h are several kilawters thick and appear "cloud-like*. Tbe lwer layers bea mrmv spectrum, and the upper layers a very vide specttu, i.e.. strongly fluctuating velocities. It appeared that the layers on the average are separated by 12-15 h in height and eloping davnvard during the day, suggesting a connection with the dim1tide. This is supported by the observation that the strongest layers oftar occurred in regions of highest shear of the me- wind vhich was ~easured siultaneously vith the radar. Superimposed on the lean wind vere often gr.rity-v.ve oscillations of about 10-min periods, and it was suggested that the mesospheric layers below 80 h are uused by wave-induced turbulence. Houwer, one also has to consider the variation of D-region electron-density profiles which influence the VHF radar detection of rsospheric turbulence. The upper rsospheric layers witb strongly turbulent velocities could be generated by hydrostatic instability since the Richardson number could get negative due to the diurnal tide near tbc equator (as pointed out in ao earlier paper by Lindzen). It rains presently unsolved if this still holds for the latitude of 19' where Arecibo is located. Although the intermittent aature of usospbtric turbulence limited in some ynlvr the continuity of VBP radar ruuraents of winds in the mesosphere, merage vind prof iles could be deduced over 8 longer period of almost 40 days from Deccober 1980 to January 1982. The ruuraents taken around the noon bours again indicated the presence of the dim1 tide; however, considerabit day-to-day variability was observed. One ryasnu that this variability is due to plmctary vmes. A signifi- cant peak-to-peak rplitudt of 6 1s-I was found in the tom1 vind at a period of 6 days, but not in the meridioml wind. It was consequently asnud that this was duc to 8 Kelvin wave. Since these tropical me disturbmces can supply westerly -ntum to the roar1 ra flw in the mesosphere, the continuous observation of vind profiles by radars will be 8 valuable contribution for glob81 circulation dels. A brief exrple of a Kelvin-Helmholtz instability observed in a strong jet belw the tropcpauw was f imlly prewnted, vhich again proved the tmique applicability of high-resolution radars to investigate atmospheric dyrua ics.

TEE USE Of WLTIBW DOPPLER EADARS TO STUDY GRAVITY WAVE IOMENTUU FlUXLS

R. A. Vincent

This presentation described a new and unique appplication of radar measurements. He stressed the possible importance of this technique to estimate horizontal waveleogtlis and momentum fluxes of gravity waves which recentlv turned out to be required input parreters for man-flw nodels. The experirental layout of this technique involves antenna bers at equal off-set from the vertical and the measurerent of Doppler velocities in these directions. Assuing that the velocity statistics .resimilar at the bea positions, Vincent shoved that the correlation u'w' between the horizontal and vertical velocity fluctuations is the difference of the mean square velocities, calculated over suitable tine intervals =d divided by a geaetrlul factor. This correlation is directly proportional to the momentum flux. Ry means of a cross- spectrrrm analysis the horizon~alwavelength and phase velocities of gravity waves and from the mean Doopler velocities the prevailing winds can be deduced.

R. A. Vincent showed experi~entalresults obtained with the buckland Park 1.98 nBz radsr applying the described technique. He used two becms at zenith angles of 11.8' corresponding to 35 km horizontal separation in mesospheric altitudes (72-94 km) and confined the analysis to velocity variations betveen 8 min and 8 h period. The Menturn flux in the mesosphere changed from westward towards eastward in the higher altitudes. Vincent argued thrt the estiwted body force of acceleration of 15-20 ms-'/day could help to explain the off-set of wind velocities in the mesosphere deduced by theory and experiment. The estimted horizontal roml wavelength of gravity wnes with periods less thm 60 rin wag 40 to 80 h on the merye, which is similar to values deduced from noctiluccnt cloud observations. The roam1 phaoe velocity dis- tribution had an umtry in the lovcr heights 80-86 h with dominating westward propagation, whereas in the upper height a s~actriul distribution was obwnrcd. An enaaaion of this experirot, using different be- directions, is pi--d. After a leer ad detailed discussion it was generally agreed that this is a perfectly correct md very suitable wthod to deteah gmity-wme parreters in the middle atmosphere.

PROPAGATIOI OF PLABETMY WAVES AS Slim BY LIMR WPIBG IUE Vm

This report presented evidence for the upability of this method to wuure temperatures in the riddle atrampbere behreaa M aad 80 h. Be shoved sat euples of the propagation of planetary waves through the mesosphere and stratosphere, uoifestad by the doward descent of cooling or waning events. By comparing these ruuraentm with global oboemations of the prevailing wind it was possible to 8h0~that these events are signatures of planetary vrres. It was pointed out that this is a rjor technique to study stratospheric warring events. &ever, clear skies are obviously needed to allw these tmperature acasuraents a8 well as supplaentary radiosonde ascents to cover the altitudes belw 30 b. SESSION 3. OBSERVATIONAL BESULT?3 XI

k number of papers were presented describing observations of both turbulent and stable atmospheric structures. All but one of the papers involved radar observations at frequencies ranging between a few MHz and 1295 Hz; the remaining paper presented in situ observations of turbulent structure obtained using a zero-pressure balloon technique.

An invited review paper describing the 0bSe~atiolulcapabilities of !ST (&sospheres Stratosphere, Troposphere) radar systesas (Balsley shoved that the HST technique holds a great deal of promise in the near f nture for examining many ;spects of a&aospheric dy&mic processes including turbulence, gravity waves and atmospheric stability.

The thiclmess of turbulent layers observed by the Millstone radar appears to be of the order of a few tens of meters (Wand, Rastogi, Watkins and ~oriot). It appears to be possible to estinste the thickness of turbulent layers by measuring the magnitude of the shear rezion. Such estimates indicate maxirum turbulent layer thicknesses of 1C ., - 100 m in the troposphere and 50 m - 500 m in the stratosphere. Esilrates of the turbulence dissipation rate in the mesosphere can be obtained from radar echo spectral width under certain conditions. Hocking reports E values raoging betwaes 0.02 w/lrgm - 1.0 w/kgm, with typical values lying betveen 0.02 v/km - 0.1 v/kgm.

VHF radar techniques can also be used to measure the height of the tropopause with an accuracy better tban the radar pulse width (Gage). The technique makes use of the fact that VEF radar returns from stable stratospheric structures are much gtronger when observed at vertical incidence.

Although most of this session was concerned with observations using the Doppler radar technique, the tvo final papers (Rottger; and Rottger and Ueek) discussed the technique of uring spaced antennas to obtain comparable atmospheric results. This technique also makes use of the enhanced echoes observed at vertical .incidence. At least two of the ST radar systems currently uoder construction will make use of both techniques in order to establish their relative advantages and dis- advantages.

Finally, zero-pressure balloon results (Barat and Bertin) show striking evidence of many thin (10 m - 240 m) turbulent layers in the stratosphere (25 km - 276.5 km) in regions of large vertical shear. Richardson numbers between 0.08 and 0.25 were measured in these regions. Concurrent estimates of vertical heat flux range between 10 - 10 . PANEL DISCUSSION

IS TEERE NEED FOR A WDDLE ATHOSPIIERE RADAR FACILITY IN EQUATORIAL LATITUDES ?

S. Kato

The panel consisted of five members: Drs. I. Hirota, W. A. Geller, J. U. Forbes, B. 8. Balsley and R. A. Vincent and was chaired by the present reporter. It was found that a middle atmosphere radar facility ir needed in equatorial latitudes, the present facilities at Jicamarca and Arecibo being located not close enough to the equator for investi- gating precise structures of equatorial waves. Uore than one facility ir required to learn the longitudinal structure of the waves, etc. Specified requirements for the observation of atmospheric waves, i-e., tides. Kelvin waves, G.V. md infrasonic waves were discussed as reported belw. Final;y, it was suggested that an equatorial observatory equipped with llST radars and other useful facilities as lidars be established and operated under international cooperation. For this purpose a vorking group should be set up and vork on the planning.

CONTRIBUTIONS Of AN EQUATORIAL MIDDLE ATWOSPHERE RADAR TO THE STUDY OF ATMOSPHERIC TIDES

J. M. Forbes

Scientific obiectives. Atmospheric tides, oscillations in meteorological fields at subhaxmonics of a solar nd lunar day, comprise an important component of middle atmosphere dynamics. Tidal oscillations in the middle atmosphere can to first order be viewed as the.superposition of several "quasi-modes" each witn somewhat dis- tinguishable and identifiable horizontal structures and vertical wave- lengths. The specific mixture of these structures, which might be comprised of migrating and non-migrating, vertically propagating and evanescent, and sylmaetric and aiymmetric components, determines the global spatial variability of the tidal oscil lations. Recently, geo- graphically syametric radars at Kyoto (?5'N) and Adelaide (35's) have delineated strongly asymmetric tidal behavior about the equator in both diurnal and semidiurnal components, between 80 and 100 km altitude. For "true" modes (that is, eigenfmctions of Laplace's tidal equation), asymmetric tides are characteri-ed by nonzero N-S velocities and zero E-W velocities at the equator, whereas the reverse is true for symmetric components. A properly placed equatorial radar could, therefore, contribute significantly to the deconvolution of tidal structures in the middle atmosphere. However, it must be emphasized that an equatorial radar will yield most fruitful results if utilized simultaneously in conjunction with at least two other similar radars within the same longitude sector (A Q '30').

The gravest sy-tric diurnal propagating (1,l) mode is thought to be capable of producing significant turbulence via nonlinear cascade or conv ctive instability mechaniems, and a mean easterly jet (z 50 m sec-'1 peaking near 105 km due to momentum deposition in the region where the tide is dissipated. An equatorial radar would, therefore, also provide the opportunity co observe the important middle atmosphere processes of wave-mean f lov interaction and wave/turbulence coupling for a knouu wave forcing. Hwwer, these phenomena vill prhrily occur above 75 km, so that it is imperative that measureaents extead as far into the lover thermosphere as possible, preferably to 105 km. Therefore, placement of the radar must avoid possible interference by the equatorial electrojet.

Radar svstem constraints/reauir~nts.

desired altitude range: 15-105 km local tie coverage: 24 hours At: 60 minutes dl: %2-4hn h>60km z1-2km h(60km

accuracy: Q, 2 msec-1 h > 60 km 2 .5 msec-l h < 60 km

Desired coordinated measurements.

(1) Simultaneous 24 hour local time mesospheric soundings at 2 other latitudes witbin 30" longitude of the equatorial radar, ?ref erably geographically conjugate, and preferably within +30° latitude.

(2) Simultaneous lidar measurements from which tidal temperature variations caa be obtained. Besides providing compieaentary in- formation on tides, such measurements would delineate tne occurrence of statically unstable conditions as a function of hcight and time, which car1 be compared with the spatial/temporal distribution of turbulence.

SCIENTIFIC REQUIREMENTS FOR THE NEW MST RADAR IN THE EQUATORIAL REGION

Subiect. Observation of equatorial waves in the mesosphere.

Backnround. During tt - Yre-HAP period (1978-1981) there has been significant progress in observational and theoretical rtudier of large-scale wave dynamics in the equatorial middle atmosphere, in connection with the quasi-biennial orciliation in the tropical strato- ophere and the semiannual oscillations at the stratopause and mesopause levels.

In regard to equatorial waves, the vertical propagation of Kelvin waves into the mesosphere with a characterirtic time scale of several days has been observed by satellites (Hirota, 1979; Salby et al., 19821, and the interaction of this wave with the mean flw is considered to be a mechanism for the generation of the semiannual zonal wind oscillation at the stratopause level (Dunkerton, 1979). A recent theoretical study by Dunkerton (1982) shows that the penetration of Kelvin waves into the upper mesosphere, as well ae that of short-period gravity waves, is likely to he responsible for the generation of the mesopause semiannus1 cycle. This result suggests the need for further observations of equatorial waves in the mesosphere.

Reauiremente.

(1) Location: In order to detect equatorially trapped wave modes it is desirable that the new obsentation station is located near the equator, i.e., within f5" latitude. (2) Height range: Up to the lower thermosphere (2100 km). (3) Quantities to be observed: Three components of wind velocities. (4) Resolution: Less than one kilmeter (vertical) Less tha~one hour [time) (5) Additionel remarks: In order to separate the wind variations due to planetary scale waves, tides and gravity waves, it is necessary to carry out continuous measurements throughout the daytime. It is also required to cover the various phase of long-term variations such as biennial, annual anc' semiannual cycles.

GRAVITY WAVES, TURBULENCE AND =AN now

6. B. Balsley

The establishment of a lorlatitude MST radar wmld provide a unique end valuable opportunity to determine the imprtence of both turbulence and gravity wave processes in the equatorial middle atmosphere. At present very little is known about either of these processes or about their effects on weather and climate or higher latitudes. Similarly, little is known af the general circulation patterns of equatorial latitudes, particularly in the stratosphere and mesosphere.

In order to mount a reasonable experimenal progrm to study gravity waves, turbulence and the general circulation at equatorial latitudes, the data should be obtained e~sentiallycontinuously for a number of ]ears. This proceSS allws studies of both annual and interannual variability. Time resolutions of the data bace rhould be about three minutes . order to resolve fluctuations down to buoyancy vave periods. Accuracies of the velocity mersuremrnt should be at least +2 m/s (horizontal) and fl cm/s (vertical). A height resolution of 500 m would be desirable.

INFRASONIC WAVES

S. Kato

Infrasonic vaves are those atmospheric waves whose periods range between a few seconds and a few minutes. The vaves behave as sonic pressure waves with some dispersion with increasing periods. The atmospheric temperature and wind distribution with height is effective on the propagation of infrasonic vwes. It is well known that the stratosphere and mesosphere make up various waveguides for the waves. Besides unusual conditions under which the waves are excited a6 AIW (auroral infrasonic vaves) atd those by volcanic eruption, we have constant generators of the pressure waves as ocean vaves. It seaas interesting to investigate the role such infrasonic vaves may play in dynamical and thermal structure of the middle and upper atmospber ; ihe pressure waves tend to be mplified in the course of upard propagation due to the decreasing ambient air density and coui be detected with fairly intense waves in the middle atmosphere. Because of :' -'--short period of a fw ten's of seconds at most, we need a good time resolution, much better than that for gravity waves. What tollows show requirements for detecting infrasonic waves:

time resolution: > lo2 sec height resolution: a few hundred meters height range to be investigated: 10 - 100 km velocity resolution: < 1 cm/s in the stratosphere and < 10 cm/s in the mesosphere.

UPPER TROPOSPHERIC CIRCULATION AND CONVECTION UPPER TROPOSPHERE-STRATOSPHERE INTERACTION

K. Gage and A. Grossman

An equatorial ST or FIST radar vwld yield valuable inform~tionon convection and Ytpper tropospnerir circulatiol in the tropics. The tropics are kllcwn to play a vital role in global climete but are still only pooriy observed. An equatorial ST or PET radar wwid enable improved mesoscale observation and at the same time pro~idea nearly continuous long-running data base which should prove most valuable for climate studies.

ST and IST radars have the ability to ruure the three- dlensioml vind vector as well as indicate tropopaur height with a ampling rate rsnging from the synoptic @ tvicc/&y) to reso-scale (a If5 min). Furthemore. the ST/BST system can be routed around the zenith (VAD rcms) to provide -80-wale estirtcr of divergarce and vertiul mtion on tie scaler of the ader of 10-15 minutes as vell as larger area ertirtes of borizontal vind vector ;compared to vertiul pointing rode). These capabilitier of the SI/lsr radar could be used both in single md network roes to provide ocv inrights concerning the description md nature of troposphcric/strato.pberic motion fields in :he tropics. &ng the nay topice upon which ST/= radars could shed light are: convective cloud and cloud clumter interaction with trow ~pheric/stratosphericwind field and tropopauw dynnics; gravity vwes on stable layers in the tropospbere/stratorpbcrc; turbulent motions at very h'4h altitudes and their relationship to vteorologiul phtnaae~ such as tropical cyclortes; and mountain/flw interactious in the tropics. Cmpared io conventioml radar wind apparatus the ST/ST radar has the r3tential of costiag less per unit of inforution and operating rasotely from areas which arc difficult to supply. This upabiiity has the potential of providing vell defined t-opiul wind networt. over a long time period vhich would aid in cur understanding of planetary scale phenmeu such 8s the Southern Oscillation, roamon md Salter circulations, snd dynamiul events associated vith El Wino. SESSION 4. EX MMRS: PLANtED OR UNDER colDSIMlCTION

Five IcST radar systss curremtly pl-d or under construction were revi~wedin this rssion. Firstly, the ~cneraldesign concept of the KJ radar cmder mnstruction in Jaw vas .bOVIL by S. Kato, Kyoto University, and then S. Fubo of the .rrt University described the details of the design of the array and elsents of the WI radar antmmm. Secondly, the Spaced &ten= radar being conuruaed in South katralia was reviewed by 9. A. Vincent. University of Adelaide. S. A. -hill of the University of Illinois described the upgrad* of the Urbmu Radar to ooe of the most sensitive radars in middle latitudes. It was announced by A. P. Kitra, Ilatiotml Physical Laboratory of India, that m PST radar systs was heing plmrwd in Indi., although ~w details. including the location md the operatiom1 frequency uerc not yet decided. Fi-115, J. Brosahp of ITCBD Technolog Iac., explained the dual rode (Doppler and Spaced Anten-) radar, the construction of which was scheduled to start this Sepcclber in Chtmg-Li. Taivan. All raj.rs except the Indian one are expected to start operation (fully or partially) in a coupie of years.

Table 1 lists the location of these lsT radar facilities, md thcir parreters are presented in Table 2. In what follws we describe in greater detail the individual radar systss.

The radar nw being constructed in Ja~mis named Mlll or KJ radar after the riddle and upper atmosphere that will k principally investi- gated with this systa. Th system is a pulr-modulated monostatic radar, operating at 46.5 Wz. lk configuration is quite different fra the existing )IST radars. A circular array with m aperture of 8330 m2 ir compowd of 475 crorrd Yagi mtcn~s,each of which is prmided with a lorpower solid-state rplifier (rP module). A peak output power of rore than 1 Hi is gmerated when the whole ryrta is coherently activated. In this oyrte, phase rhifting is performed at a lwpover level blr electroniufly controlled phae shiftera, which enable rapid and continuous scanning of the .atam. The whole rpstea is monitored and controlled by a network of ucroprocessorr.

The antenna array designed by numerical computation is a circular array with the equilateral triangular grid with spacing of 0.7 i (A: warelength). In this e:aent arrmgaent, the mtcn- bea can be tilted up to 30. from tte zenith, and the ridelobes at mgles of elevation lover thm 20' are rore than 40 dB down fra the rinlok for the whole scan range. TABLE 1 WTIdS OF llFT BAN& FACILITIES IMNED OX UUDEP CGHSZWCTIOW

10 radar Kyoto Stigaraki 34.85'3 / 136.1OeE University Japan

Adelude radar University of Buckland Park 34.63's j 138.48E Adelaide Australia

Urbradar University of Urb 60.17'N 1 88.17.V Illinoia Illiaoir

Indim radar Uuiorl Piisical Bot yet - / - Laboratory decided

The three-subelsent Yagi mtenna was Ccsigred to optimize its performance for ut inf bite array. The Yagi mtcnna tus an elaaent gain of 7.2 dB that is the higbcst gain expected for the present elaent spacing. Imped.nce utching to tbe feed lime is also excellent. These properties show little deterioration wrr the whole scan rage and over the frequency blodvidth of 2 t&. The edge effect to be included in the finite array is found to be -11 except for the outeraost array elarents.

A receiver on hrdJap8oese uteilite EICEC (tc be launched in 1984) vill be used to test the antenna directivity. Om tenth of the rotranas and TR modules are scbtduled to be constructed by March 1933, starting the preliminary observation of the troposphere ad the lover stratcsphere. The vhole syste will bc completed in srrr?r 1984.

3. A. Vincent

The syste~is designed as the Space hte~uaradar. The trans- sitting array vith a square aperture of 88.6 x 87.7 t- consists of 32 north-mth rows of 48 halflr#elngtf: Cipoies of :he coaxial callinerr type. Each row of dipoles bas its m coaxial feed-line to the trloaitter louted at tne center of the array. The arrhy be= is directed verticslly for the Spaced Antc~lyde.

fbe receiving antenna consists of three spaced arrays, each con- sisting of 4 x 4 five-subelement Yagi =tmnas. They are located vest of the trmsmitti~garray, the center of each array being on the vertices of m equilateral triangle having sides of length 10 ,. Sign8ls from rbe three receiving arrays are premplifizd near the arrays and then fed to the main builaing at the east end of the radar site.

Pulse repetition frequency is variable frm 64 to 1024 Bz. lill~ber of -2les and height range to bc obse~vedare also programable.

Due tc the comparably low poueraperture product of the present sj~tm,the height range to be covered will be restricted to belw 3C km. It is plmned that the peak output pover is increased to GO-500 Irk at tbc text constructior! stage io 1983. It is also =visaged that the Doppler mode of operation will be used for the trmscitting array by installing the TR svitch. Hwever, the be= steering will be li~itea only in the Eli plane due to the arrangmtent of the dipcles.

It should be noted that this radar will be situated adjacent to the existing 2 #It partial-ref lection radar and very near the con jugate point of the I&' radar of Japan. This radar vill be the first WI r~dar in the Southern timisphere whm coapieted late this year. The S'rbau radar operating at 40.92 lllz is scheduled to be upgraded soom. The upgrading will apply to all aspects of the present syjta. Pirely, the mtcam of th? square array is to be enlarged to 10' rn: -- almost tea tirs the present aperture. The array is umporcd of 12 x 12 modules, ach consirtiag of 4 x 4 dipole elements. Although the anfama be- of the present systm is fixed to appoxirtely 1.5. southeast of the zmith, a limited kr steerability vill be afforded for the upgraded systs, phasing each element of the lodular array by 90. steps.

Secondly, the peak output power of the traaitter will be increased to 6 HU with the mximm duty ratio of near 12. Tbc bandwidth of the tran~itterwill be enlarged to allost 1 mz, which improves tbe bcight reso:ution from the present value of 3 b to near 150 r. Tbe 1 rcgatuud phase witching will also be irplemented. The drive circuit of the trmmitter as well 8s the =-itch wiil be iraproved.

Tbe receiver bandwidth will be utched to the trrmmit pulse width. A sophisticated integrating preprocesscr vill be installed.

Finally, the curratly used computer. a PDP-15 with a paper tape I/Q device, will be replaced a floating-point processor (7 IIFLOPS).

It is expected that this sysca will be the mst sensitive ?ST ra&r in middle latitudes when colcpleted, conparable to the Jic-arca and Poker Flat radars in lov and high latitudes, respectively.

The Indian Pa7 radar currently planned by National Physical Laboratory has basically a similar coafiguration to the Poker Flat rrdar in Alaska. Tte radar vill operate in the 50 IRz band, but the exact operational frequency will depend oa the frequency cleirmce by the Indian government.

The transmitter vill be composed of 24 modular transmitters alcng with the total peak output power of 2.5 HU and an average pover of 60 kU. Each wdcle has a peak output pover of 100 kU vith the maximum duty ratio of 2.5%. These modules operate vith pulse length from 1 ;s to 32 ..s (1 ,s steps) with pulse repetition frequency frm 256 Rz to 8 kHz (binrry steps). The antenna consists of two superirposed arrays, with the dipoles of each array arraged at right angles to each other. One array is uud for one linear polarization. The array with an aperture of 128 x 168 m2 is composed of 48 row. of four separate coaxial collinear antennas. Each anteaus is constructed of 16 tulfir.*eleagth dipoles. Eight mch adjacent antennas are fed f ra a cmnwdular trutritter. Tbe two arrays will be switched to the tranritters and phased to point in five directions; zenith and ?Mafra the zenith in the Eli md IIS planes.

The data aquisition, calculation of spectra, .ad initial uulysis will be done on-line by a miniunputer, .ad the whole systa will be controlled either by the same minicomputer or by a network of micro- processors.

The 53 lllz radar i3 Taiwan is designed to be operated in both the Doppler oode and the Spaced Antenna rode. Tbe switching between the two modes will be done on a tin scale of seconds. This capability will enable direct comparison betwee the two lodes that has not yet been made before.

Three separate subarrays which are required for the Spaced Antenna mode are each provided with identical trlnritters and receivers. The subarrays are initially composed of 32 Yagi mtenms with PI aperture of near 1500 m2, but easily expandable to 8 x 8-element arrays in the future. The elaent spacing and the number of subeleents have not yet been detezmined.

By using 0, 90, 180. and 270' delay lines, a fairly simple ber steering is realized. The mmber of be- positions is five; zenith and off-zenith in four azimuths. The be- steering systa alw allows the alternate elements to be fed out of phase to provide tn, orthogonal twin lobe patterns providing a null at the zenith. Them twin lobe patterns provide Doppler data vith both positive .ad negative components, the difference between the two lobes giving data on maentum transport. The three subarrays can be operated independently or together in a11 combinations of these reven be= patterns.

The minicomputer wil; initially be utilized only to write inte- grated data onto the magnetic tape and provide a minimum of real time display.

The sensitivity of this radar will be 6 dB down from the SOUSY radar in the Spaced Antenna mode of operation. The construction will start this September, and be completed in late 1983. SESSION 5. BADAB TECHNIQUES

UST radar probing techniques were reviewed by D. 1. Farley. The points discussed include: (1) antenna nearfield effects (the Arecibo antemum, for euplt, is actually too big for optimum MST work). (2) range and frequency alia;ing, (3) coherent vs. incoherent integration, (4) various forms of pulse compression, and (5) the dependence nf the signal-to-noir ratio (SNR) md signal detectability on pulse length (range resolution). The backscattered signal strength is actually proportiowl to the inverse of the antenum area in the mar field (unless the a~tenluis focurcd). Arecibo is the only observatorv vhere thir effect is currently a significant probla. It was pointed out that coherent integration is simply a form of digital larpass filtering. With optimm processing the effective SNR or detectability of the received signal is usually proportiom1 to (average trmtmitter paver) x (pulse length) x (integration time)l/2. High average paver can be achieved by pulre compression (at the expenee of added ground clutter) or by using a high pulse repetition frequency (at the expenr of possible range rbiguity problas). Tbe pulse length dependence disappears for very thin scattering layers. A suggested increased dependence for 'coherent' layers was mentioned and was discussed at some length in session 7 (met discusrnts believed that horizontal coherent had no effect on pulse length dependence).

8. F. Woodman reviewed the hardvrre implementations of on-line digital sigual processing at rveral BT radars, especially kecibo (at both 430 EUz and S-band) md SOUSY. Be emphasized the convenience of interchanging coherent integration and pulse decoding; the decoding of phase-coded (compressed) pulses after integration rather than before greatly reduced the number of digital operations required, especially for VBP radars, for vhich the signal Doppler shifts are very mall. Arecibo is fortunate in having available several extremely high-speed special-purpow digital devices designed for radar astronomy obrenations. The speed of these devices exceeds most HST requirements and has made porsible wrc etratospheric obsenrations at S-band vith a resolution of 30 m. Woodran and his collaborators have developed an algorithm which very effectively rawer moat of the ground clutter. etc. from Arecibo data.

S. A. Bowhill described the data preprocessing syetes planned for tbe upgraded Urbana Radar. Since it is designed for a specific system and does not need much flexibility, it is quite simple md inexpensive, but nevertheless it cm eample 600 altitudes at I50 m intervals vith 8 2.5 ms interpulse period. In a wcond talk, Bowhill described what can be done vith a very siarple system using an Apple computer and only floppy disk storage. A single disk can accommodate an hour's data from 20 altitudes. The FORTH computer language is particularly comrenient for such a aysta. G. P. Loriot md R. H. Wand described the phase coding and data processing schemes ueed at the Hillstone Hill Observatory. Data are transferred directly into an Array Processor, permitting very fast processing. The primary limiting factor is the size of the AP iemory (large nenories are very expensive). With their present system the available on-line options rmge from a 4096 point FFT at only one altitude in real time to 32 point F'FTs at 270 altitudes. Coherent integration is not as useful for UHF radars as for VIIF, as mentioned earlier, and so the processing requiraents are lore severe, There was some brief discussion of various ways to achieve unbiassed phase codes (equal time at both phases).

K. Wakasugi discussed detailed ulculations of his (with U. htsuo, S. Fukao, md S. Kato) of the full rbiguity function of various complementary code sequences md showed how the range sidelobes behave for targets giving various Doppler shif to. It was pointed out in the ensuing discussion that, for wst llST applications, the Doppler shifts actually encountered are not large enough to cause difficulties.

U. P. Sulzer and R. F. Woodman next described sae intriguing work carried out at the Arecibo Observatory. They developed sets of pseudo- random codes designed to operate well in the 'real vorld', in vhich the radar transmitter doesn't generate exactly the phase-coded pulses intended. Because of such tranmitter imperfections, the range sidelobes near the central peak are not zero, as they should be theoretically, for complementary code pairs. They are still small (about -20 dB typically at Lrecibo), but reducing them further is desirable for some measursents. One scheme described to achieve a reduction for mesospheric observations involve tranmitting a sequence of 256 different 52-baud codes, each of which must be decoded separately. The 256 'best' codes were chosen out of about 10' possibilities by a computer search iavolving sme 10 hours (!) of Array Processor tire. A similar scheme for the stratosphere uses 48 32-baud sequences grouped in quasi-wmplaeatsry quadruples. The search for the optimum quadruples required more than 300 hours (I I) of AP time -- not a route for the fainthearted. The use of such schemea requires special purpose hardware since no data reduction via coherent integration is possible. The codes adopted give near-in range sidelobes about 30 dB lwer than the main peak (roughly 10 dB better than that actually achieved by the supposedly corplmentary codes).

P. K. Rastogi and G. B. Loriot discused Some of the procedures currently used in ST erperienl-8 at Uillstone ail1 to reduce the effects of ground clutter and power line interference. Mter determining the nature of the interfering signsls, digital notch filters were applied to the data.

C. E. Ueek then gave a description of the systeP used in Saskatoon to study drifts using the partial-reflectioa technique. The system is controlled by an Apple computer and runs mattmded. Ueful data are obtained in the range 75-125 h with 3 h resolution vith A trmritter having only 10 Y of average pover (but 50 kW peak pover). The obsenrations were in good agreerent with rocket data.

Finally, C. Cornish shoved same data from vertical incidence radar mearureents at Jiuarca. Echoes were obtained from the entire lCrr range, including the difficult 40-50 h region. The range rerolution was 2.5 km, the peak tranaitter power war about 3 MU, and the average power was about 170 kW. R. C. Roper

While the ability of MST radars to measure winds from 1 Irm to 100 ka altitude is theoretically feasible, .at limitationr do exist. In particular, the diurnal variation in D-region ionization makes continuous recording (necerury for the delineation of tidal winds) virtually imporsible, except for high latitude stations ia summer. Eor ever, by using the radar as a meteor wind radar, continuous wind mearuremcnts un be made over the 80 to 100 km height range (as has been daonstrated by Susan Avery in rerults prerented at the IAMF' Weeting, Euburg, August 1981).

The lover powered and less expensive ST radars also have the potartid for uae ar meteor wind radars, and thir possibility should be taken into account in the design of these facilities.

The GLOBBET (Global Radio Meteor Observations) progr-, currently in the planning stager, ir designed to further not only the wind measuremato currently being performed rsder the UGA Global Radio Meteor Wind Studies Project and the UBSIIXAGA Coordinated Tidal Obwr~ationrProgra, but also the better mearurment on a global scale of rteor rates, velocities and orbits, and the underrtanding of the physics of meteors and their interaction with the earth's atmosphere.

The author briefly mentioned his recent visit to Moscow, to work on the GLOBIET Plmning Document (to be presented at the COSPAR meeting in Ottava later this month), and also to Dushanbe, Tajicstan, for a tour of the Astrophysical Observatory, which is unique in its application of optical, N imaging and radio techniques to the observation of comets and meteors. It appears that the 50 km altitude "hole" in WT radars will probably require the uee of the lidar technique currently being used by the French, and reported by Ihrie-Liw Chanin earlier in the meeting. R. Woodman shoved a vievgraph of echoes from Arecibo, obtained using the 5 mz heating facility as an MST radar. Close scrutiny shoved that echo strength decreased rapidly below 6Q h, and that the plotted ground clutter vas many times stronger than 50 km echoes.

Panel Discuruion: Th Future of Uiddle Atnoephere Radars

Panel members were: S. A. aowhill (Chairman), D. T. Farley, K. S. Gage, J. Rottger, R. A. Vincent, and R. F. Woodman J. Rottger: We should not overlook the possibility of using medium frequency or low BF to take advantage of the higher re- f lection caef f icient in the partial reflection mode, plus the fact that orrn-made noise tends to be a minimum in the neighbor'mod of 2 IMz in the daytime.

R. Vincent: Use of the Buckland Park array on 2 to 3 EQlz has revealed a clutter problem, and various methods of integrating out the clutter are being investigated. In addition to the clutter problem, another question should be addressed: What is the scientific merit of using a radio method to f ill in the '%ole", when it can be done more easily by other means (c.f. paper preceding this discussion)?

S. Bowhill: Clutter can be a real problem on 60 Miz. Its occurrence is seasonal. In general, itc effects can be minimized by varying the interpulse period.

K. Gage: Our ability to discriminate against clutter (or any non- atmospheric and therefore undesired signal) depends on hw well we understand the desired signal reflection process. We have developed a model based on a ''volume filling" reflector which indicates a 2 dB/km falloff in returned pover in the stratosphere at all latitudes (the height of the tropopause deternines the behavior at lower altitudes, and provides a tool for monitoring tropopause height). Atmospheric stability and density are of prime importance in this model.

S. Bovhill: One strategy which can be applied is to integrate returns coherently for, say, the first second, then integrate the real and imaginary parts of the complex correlation function (if the vertical velocity is constant, chis is equivalent to coherent integration). If ground clutter in serious, perhaps one should look off-vertical, and 1 :grate for an hour to find the horizontal velocity, thereby integrating out the ground clutter (end, of course, the shorter t zriod gravity waves). . Farley: We need to be aware that simply changing acquisition, reduction, or analysi~schemes will not defeat the funda- mental concepts of information theory. Since spectra are transforms of correlations, the inherent limitations of one appear in the other. With regard to the use of lower frequencies, bandwidth limitations result in a drastic loss of height resolution.

S. Bowhill: It does appear that one needs to use medium frequencies in order to see int3 the gap. R. Uoobn: Propouls can be made to the Arecibo Observatory by anyone who wishes to use the heater facilitv there.

J. Rottger: Becauw of the long pule widths at lover frequencies, one needs to look at low elevation angler in order to Ite returns from the rtratospbere, and off-vertical antenna gains fall rapidly. There are plans to ur the Tromso heating facility to investigate the stratosphere, but off- vertical antenna gain may limit its ueefulness at there altitudes.

S. Bwhill: Returning to clutter rejections, coherent integration is essential.

P. Rastogi: Higher signal-tcmoise ratios in the "hole" region should surely arisc during PCA events at high latitudes. Coherent integration will be required.

R. Vincent: Yes. The effects of such events have :eea sea at least as lov as 50 km at Kavson, Antarctica using a coherent integration partial-ref lection drifts system.

S. Bwhill: Partial reflection drift systems have traditionally not used coherent integration.

C. Meek: Coherent integrators are being installed in the Saskatchewan partial reflection drifts system.

S. Bwhill: In addition to PCA events, it might be prof itable to look during solar flares.

8. Woodman: Where bandwidth allws, coding techniques can be helpful in improving signal-to-noise radio and clutter rejection.

J. Green: A simple two bit 180° phase code helps, particularly against man-made interference.

S. Bowhill: The standard clutter rejection is a notch at zero frequency. However, this will not help with F-region backscatter. Sea clutter usually appears as +ve and -ve drifters around zero. Can other frequencies be produced by the ocean?

R. Woodman: Ships can be a problem.

S. Bwhill: Because Illinois is so flat, we have never seen clutter from surf ace features appearing in the stratosphere or mesosphere. R. Vincent: There is clutter at 50 km at Adelaide due to hi1 1s. It appears to move very slowly, probably due to changes in refractive index with time over the clutter path.

W. Bocking: Yagi antennas are sometimes used to identify ground clutter, but this can be difficult in that different propagation paths are involved.

J. Rottger: We have a clutter problem at 55 km which is due to a TV tower. We are investigatinq possible changes in clutter siprntures with tranamitted frequency, as compared to actual atmospheric echoes, and also comparisons with radiosondes to "calibrate out" the clutter.

B. Balsley: We have no detectable clutter at Poker Flat.

R. Woodman: It is certainly easier to discriminate clutter at 51) Mlz than it is at 430 MTz; there is considerably more fading at the higher frequency. The intrinsic width of clutter is less than that of atmospheric echoes. For further comwnts eee Sato and Wocdmrn in the preprint volume of the American Meteorological Society Radar Meteorological Conference No. 19 (1980).

P. Rastogi: It is possible to remove clutter by a deconvolution in the frequency domain.

S. Bowhill: Concerning the topic of D-region incoherent scatter, it is observed at 430 MHz. Has it been observed at 50 Mlz?

R. Woodman: Possibly, but it was not recognized! The question has yet to be resolved and we are planning to search for it at Jicamarca.

D. Parley: The best indicator is the time constant. For incoherent scatter, the molecular diffusion time constant is appropriate. For coherent scatter, the eddy diffusion time constant. TurbJlent echoes will be wider than rn- coherent scatttr echoes.

P. Rastogi: The variat'on of the turbulence microscale with height, with a large microerale at greater heights, is an observable phenomenon. One must always be careful in distinguishing turbulence f ram incoherent scatter.

B. Balsley: At 50 MHz the top of the echoing region is 85 km because of the increase of the tlrrbulence microecale with height. Perhaps we should easily o'Ds2rve incoherent matter at 50 MHz above 85 km. S. Ilovhill: Fkn one observes essentially no coherent echoes belw 175 kn is the time to rarch for lncoherear scatter echoes at those altitudes. Uuch more inforution can be obtained from mesospheric spectra than ve have obtained thus far.

1. VmZandt: ReEerence has been made to long-lived sheets of turbilence in the atmosphere in the ure terms as those vhich exist in the ocean. Fossile turbulence refers to the tapra- ture f luctuations (cT2)left over aiter velocity fl~ctuations(cV2) have ceased. The decay of velocity is controlled by kl~euticviscosity; the d-cay of tepera- ture by thermal diffu~;vit)-;and the deuy of concentra- tion by wlecular diffusivity. In the ocean, these go as 100:lU:l. Velocity f luctutions dcuy 10 tirs faster than temperature fluctuations. In the atmosphere, these nar-eters arc roughly equal and all f luctution fields ueuy at tLe merate.

8. Roper: It is simply a question of Prandtl number.

T. VanZandt: There is, in fact, no need for "fossil turhlcnce* t~ explain long-lived sheets of turbul-nce in the atmosphere. They are associated vith long-lasting vind shears. There is a real need to correlate turbulent sheets with wind shear at ull scales. Current correlations are less thau unity probably because, at the limit of height resolution for wind metsursent, the shears are not large enough to drive the Richardson mmber belw critical, whereas, at still culler scales, they are.

J. Rottger: * .dars can be subdivided at this stage of dcvelopent into two classes: (1) B-s! svinging (VAD or velocity azirmth display; or pointing in three directions), and (2) Spaced antmilr. Can we settle cm a preci- noaenclature for these classes?

(Considerable discussion follwed, resulting mostly from the fact that techniques nov in the process of development, ~chas interfero- meters, sc6ed not to be easily classified at this tir.

It vas finally resolved that the technique using spaced antarnas should be called the SPACED AKTMRA technrque, and that, since all other *echn5ques at present in use measure line-af-sight dopplers, the so- called "bem svi*zingw techniques varld best be referred to rnrder the collective heading of DOPPLER techniques.

S. Bwhill: Let us nov consider the problem of backscattered si-1 strengths and range resolution. W. Hccking: If there are several "reflectors" within a layer, do the povers reflected by each add (incoherent scatter process. 'r dependence) or do tbe voltages add (coherent scatter processes, <:r dependence )? For a sxngle tranritted f requenry , the dependence is on (:r 12. However. a f bite ~uluis not a single frequency. and the smaller of the pulse length or the imdividaul wreflector" thickness is renponsible for the reflected pover. On the average the povers will add, rather th.n the voltages. %t is, more than one scale is responsible for the scattering,

8. ha: In verifying tbis bypothesir, ooe beds to be certain that both signal-tenoir ratio and receiver bmduidth are appropriate to the task. A :r dependence will resalt if the receiver bmduidth is narnnter than the pulse.

D. Farlq: I s,pport the tr dependence md kliwe we are dealing with random sc,tterers.

K. Cage: fbc rdiuhs mycomponents in the Fourier Win. The question is: Is a cokerent scattering process possible? In the book "Sbrt Wave Radio Propagation" (edited by D. E. Kerr) there is m appendix by Seibert md Goldstein which discusses incoherent vs. cohercnt scztterers. Sp8tially varying structures are coherent. Structures fluctuating in tir are incoherent. The arywnt can be wttlcd by a properly designed experhat. Tbe age model, which ass-s a (drI2 dependence, appears to de- scribe the &ta well. By oherring vertically (uxiuring the spcular) and off vertically (maxiruing the turbulent) a caparison of rmge resolution dependence could !te ude.

J. Green: We hre rhe data (from spcular md oblique soundings) .nd should k able to resolve the problm.

J. Pottger: With 150 resolution md observing a single, ~11-&fined layer, it appears that neither s Lr nor a (~r)'dependence suffices. For this use mother theory is required.

S. Douhill: The fiml topic for discussion is the appropriateness of dimtributed vs. single tr.oritter for I(ST radars.

S. FoL.0: The Kl (middle md uppr aaospkre) radar rt Shigara, Jawumes a distributed trsnmitter. Imeatigators imolved vitb the design are particularly interested in -11-scale motions, vith a hi6h priority king placed on rapid kr swinging. With distributed tranritte s the array CAU be lore easily segented and inexpensiv~ stable phuc shifters can be made using PII diodes at low pouer levels. Sidelok accuracy should be greater. This is eccesnry to minimize interfereuce in Japan.

1. blsley: Tbc ratiomle fathe Poker Plat radar (64 traritters) catered on reliability for continnous and cnuttcnded operation, for which it is obviously eeccsury to rinilise catastrophes1 If one a two f hlrplifiers faii, the qrta still record. uaeful data. The Poker Flat llST rabr hs beem "ao the urn contimvusly since Febrrury, 1979.

S. hubill: At Illinois, we already hes big tranoitter. Uhile there is 8 #itching pmbim associated vith modulariring the ateam at high powr levels, we believe ve can solve it with a large ce~ric%.fern witch. Rqid witching is not contaplattd. Tbcre is at leut ooc bcllcfit of a "single compo~~~nt"tran~aitter - bmdvidths are more easily widened.

I. Woodm: A capletely solid-state tranrltting qsta, such as the WI r8d.r. is mecostly than one using vacw tube?

S. FoLo: Ve believe that qata reliability will be better md the solid-state 9sta will be less expensive in the long run.

S. Bowhill: I wish to thmk the Worksbop convenors, Rofesrors Kato md Hirota, for aganizing an outst.ndimg and very tirly weting, and alao the cooittee rmder Dr.. Balsley and Vmtmdt for the local arrmgacnts. Ute*. Iff iliatiom

Paul Br~ley Hatiom1 Ggter fa^ Atmospheric Research

John Brommh.n

Sidney A. Bwhill University of Illinois

hrtin I.

David A. Cuter Natioml Otc.nic aud Ahaspkric Ahhistration

G. S. Chndrawkturo Bhsrat Electronics Ltd.

hie-Liw Chin

Jih bin Cho Nations1 Central hiversity

Wallace L. Clark Natioml Occmic .nd dtmospheric Ahhistration

Charles Cornish Cornell University

Lvrence Coy University of Washhgtaa

Peter Czechowsky tlu-Plmck-Iwtitut fur Aeroncie

Timothy hrnkerton Rationsl imter for Atmospheric Rzsearch

Warner L. Ecklmd Rations1 Oceanic and Atmospheric Actrinistration

Donald T. Farley Cor~;ellUniversity

Jeffrey M. Forbes Boston Col iege

David C. Fritts

Shoichiro Pukao Kyoto University -in A. Ccller

Xicbcl Glus

Uillir E. -don

John L. Creep

Kyoto Bnirermity

Zbc Uoirersity of Adelaide

Kyoto Unirersity

%tiom1 Center for Ataospberic Research

George B. Lorioc tkrtbeast Radio Observatory Corp.

D8rm Lu Uatioml Occoic md Atro8pheric Administration

University of Saslirtcbcu8~

Uat ioal Physical l.boratay

Bhrat Electronics Ltd.

northeast Radio Observatory Corp. George C. Reid Natio~lOcemic .nd Atmospheric Administration

Anthony C. Riddle Natio~lOceaic 8nd Atmospheric Administration

Robert G. Roper Georgia Tech

Jurgcn Rot tger EXSCAT Scientific Association

K8thrp J. Ruth Natiolul Ocemic adAtmospheric Administration

Nationsi Clnter for Atmospheric Research

Rava: Research Laboratory

Nation1 Center tor Atmospheric Research

University of Saskatchcu8a

lava State Unirersity

National Oceaic and Atroxpheric Achinistration itobert A. Vincent University of Adelaide

Koichiro Ysksugi Kyoto Institute of Iechnolog

Jacs & Wunock Iatioml Oceanic and Atmospheric Adrinistration

University of Alaska

Ration81 Oceanic and Atmospheric Administration

Ratioml Science Foundation

Institute Geofisico del Peru GROUND-BASED STUDIES OF TEE XDDLE ARlOSWERE

Schverin. German Dsocratic Republic organized by the Auday of Sciences of the Gerun Democratic Republic, Central Institute of SolarTerrestri.1 Physics (Heinrich llertz Institute), together vith the National Camzittee on Geodesy and Geophysics. co-sponsored by the ICSU Scientific Canittee on Solar-Terrestrial Physics (SCOSTEP)

The Symposira is intended to focus upon those studies of the middle atmosphere for which ground-based methods, with their abilities of continuous monitoring of both long-ten md event- like processes. are particularly suitable. It should discuss results and methodical quertionc of ground-based observations as well as their complaentary relations to space techniques and other theoretical and aerontmiul studies relevant to the projects of the internatio~lKiddle Atmosphere Progrm.

The progra is to consist of invited and contributed papers on the f ollwing topics :

- Diagnostics of the middle atmosphere by D region observations - Seasonal and interannual variations - Troposphere-stratorpher~sospbere coupling - Winds and waves, and their tracking bv radar and radio sounding rethods

- The nsopause, and links to the theaosphere (NU, Airglw, Ra Libr, Sporadic-E)

- Solar-terrestrial influences on the middle ataosphere

Convener: Prof. Dr. J. Taubenheim Zentralinstitut fur Solar-Terrestrische Physik (Heinrich-Hertz-Inntitut) DDR-1199 Berlin, Gernun Democratic Republic Date: Early s-r, 1981

Venue: Kyoto (Kyoto City Ha11 near Heian Shrine)

Sponsor: Radio Atmospheric Science Center. Kyoto University

Co-sponsors : bin Nation81 and Interuatioual Bodies supporting W (under conrideration)

Nmber of attendents expected: 150-200

Subjects for discussion: All subjects in UAP are covered, but "interaction mong dynamics, chemistry and radiation" may be a stimulating subject. Joint WIUGASymposium on Middle Amsphere Sciences (MAS), XVIII Assembly of IUGG, Haburg, FRG, 15-27 August 1983.

R4S is being joint15 organized by the International Association of llcttorology and Ahospheric Physics (I.)and by the International Association of Geomagnetia and Aeronaay (IAGA). It is cosponsored hy SCOSTEP and COSPAR. IWgroups involved are the Interrutioual Caissions on the Ueteorology of the Upper Atmosphere (ICIRIA, leading), Atmospheric Chemistry and Global Pollution (ICACGP). Atmospheric Electricity (ICAE), Dyamiic Ueteorology (ICDn), Ozone (IOC), and Radiation (IRC). The mphasis of the progrm will be on the dynamics, energetics and cbaistry of the middle atmosphere (about 10 to 120 km height). Special problems included are the electrodyaamics of the riddle atmosphere and the physics and chemistry of ions, aerosols and noctilucsstt clouds. th~tualinteractions of the llriddle atmosphere regions and coupling with the troposphere and upper mesosphere will be discussed. Cantributed papers on significant observational. theoretical, and cxperirental results are solicited.

The Middle Atmosphere Sciences Symposium is irm~ediatelypreceded by a spec~alIUCG Symposium with review papers on the Middle Atmosphere Pronram. 11 half-day sessions starting on August 20 are planned for the Uiddle Atmosphere Sciences.

' Uodeling of the middle atmosphere, including radiation budget ' Coupling between the stratosphere, mesosphere, and thermosphere ' ~liLtoiogyof the middle at;osph;re Gravity waves and turbulence. and parsnetrization of related transport in middle atmosphere models Dynaics, including troposphere coupling ' Remote sensing W flux, photochemical processes and related chemistry ' The electrody~micsof the middle atmosphere ' Trace species in the middle atmosphere ' Noctilucent clouds ' Physics and chemistry of ions and aerosols in the middle atmosphere

Deadline for the submission of abstracts is 1 Harch 1983. The origiual should be sent to the Secretary General of IAUAP, Mr. S. Ruttenberg, NCAR, P. 0. Box 3000, Boulder, CO 80307, USA, and a copy to each of the conveners Dr. A. Ebel (IAUAP), Institute for Geophysics and Ueteorology, University of Cologne, D-5000 Cologne 41, Federal Republic of Germany, and Dr. P. C. Simon (IAGA). Institute dlAeronmie Spatiale. 3 Ave. Circulaire, B-1180 Bruxelles, Belgium. Detailed instructions about the abstract format are included in the Second Circular of the IAMP General Assembly (available from the IAPIAP Secretary General, Mr. S. Ruttenberg) or the Third Circular cf the XVIII IUGG General Assembly (available from the Chairman of the Local Organizing Committee, Dr. W. Zahel, Institute fur Ueereskunde der Universitat Hamburg, Heimhuderstrasse 71, 2000 Hmburg 13, FRG). Figurer 1 and 2 belw were inadvertently omitted in the Nationml Report of the United Kingdom, publirhed in Volume 4 of the 8mdbook for )UP. The editor regret6 any inconvenience caused by this airrion.

Fip1. Photochemical processes influencing the concentrations of neutral and ionized sodium conttitumts. The numben rnsofirtcd with the different processes are those referred to m the text.

Figure 2. Location of existing and proposed experimental facilities in the U.K. for the study of motions in the middle atmosphere. Hatched circles represent the common volumes sounded by meteor wind radan to be operated at Sheffield and Aberdeen.