Institute of Spaceand

AtmosphericStudies

20002000200020002000

Institute of Space andAtmospheric Studies

Institute of Space and Atmospheric Studies, University of Saskatchewan116 Science Place, Saskatoon, Saskatchewan, S7N 5E2, Canada

Phone: (306) 966-6401 Facsimile: (306) 966-6428Electronic mail: isas@dansas.usask.ca

Web site: http://www.usask.ca/physics/isas

Annual Report2000

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Table of Contents

ISAS Facilities

An Eventful Year in the Department andthe InstituteCanadian Space Agency (CSA)ProgramsThe Natural Science and EngineeringResearch Council (NSERC)Outreach: Technology TransferOutreach: Media and GeneralFunding, Staff and Programs

Department of Physics andEngineering Physics Faculty MembersISAS StaffISAS Graduate Students

Observatory FacilitiesField SitesComputing FacilitiesOptical and Electronic Laboratory FacilitiesParticle Calibration FacilityElectronics and Mechanical Stores Facility

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Chair�s Report

Members of the Institute667

Advisory Committee 5

Research ProgramsPlanetary AstronomyAtmospheric DynamicsMagnetosphere/Ionosphere InteractionsIonospheric PhysicsAeronomy Research

G.R. DavisA.H. Manson

G.J. Sofko, A.V. KoustovA.V. Koustov, G.C. Hussey

E.J. Llewellyn, D.A. Degenstein

Appendices PublicationsGraduate Student ThesesPresentations (Talks, Papers, Posters)Visitors to ISASAttendance at Meetings or Other VisitsServices and DistinctionsVision Statement

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51535457585960

University of SaskatchewanGovernmentIndustry

ISAS 2000

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Mr. Peter MacKinnonDr. Michael Atkinson

Dr. Mark EveredDr. Michael CorcoranDr. Gary Kachanoski

Dr. Tom Wishart/ Dr. Dick NealDr. Franco Berruti

Dr. Akira Hirose

Dr. Alan Manson

Advisory Committee

GovernmentPresident, Communications Research CentreVice President, Radio Science Branch,Industry Canada, OttawaHead, Geomagnetic LaboratoryGeological Survey of Canada, OttawaChief of Experimental Studies, MeteorologicalService of Canada, Environment Canada,Downsview, ONActing Director of Program DevelopmentSpace Science Program, Canadian Space AgencyOttawaDirector General, Defence Research EstablishmentOttawa (DREO), National Defence, OttawaPresident and CEO, Saskatchewan ResearchCouncil, SaskatoonActing Chief Operations Officer (SRC designate)

IndustryDirector, Corporate Planning and CommunicationsSED Systems - a division of Calian Ltd., SaskatoonPresident, Scientific Instrumentation Ltd., SaskatoonPresident; Kipp & Zonen Inc., SaskatoonV-P of Finance (Kipp & Zonen Inc. designate)President, PAKWA Engineering Ltd, Saskatoon

Dr. Gerry TurcotteDr. William Sawchuk

Dr. Richard Coles

Dr. David Wardle

Dr. David Kendall

Dr. Prakash Bhartia

Mr. Dan McFadyen

Mr. Bryan Schreiner

Mr. Don Epp

Mr. Larry CooperMr. Ben Dieterink

Mr. David CortensMr. Dennis Johnson

PresidentVice President (Academic)(Academic V-P designate)Vice President (Research)Dean, College of Graduate StudiesActing Deans, College of Arts and ScienceDean, College of EngineeringHead, Department of Physics and EngineeringPhysicsChair, Institute of Space and Atmospheric Studies

University of Saskatchewan

ISAS 2000

Members of the Institute

Department of Physics and Engineering PhysicsFaculty Members

ISAS ExecutiveG.R. Davis

D.A. Degenstein

G.C. Hussey

A.V. Koustov

E.J. Llewellyn

G.J. Sofko

B.Sc. (McMaster), M.Sc. (Toronto), D.Phil. (Oxon.)ProfessorB.Sc., B.E., Ph.D. (Saskatchewan)Assistant ProfessorB.E., M.Sc., Ph.D. (Saskatchewan)Associate ProfessorM.Sc. (Leningrad State), Ph.D. (Moscow Instituteof Earth Physics), Associate ProfessorB.Sc., Ph.D. (Exeter), D.Sc. (Saskatchewan)F.R.S.C., P.Eng., ProfessorB.A.Sc. (British Columbia), Ph.D. (Saskatchewan)P.Eng., Professor

B.Sc., Ph.D. (Canterbury, N.Z.), ProfessorA.H. MansonISAS Chair

Adjunct Professors

B.Sc., M.Sc., Ph.D. (Saskatchewan)B.Sc. (Hebrew, Israel), M.Sc. (New Mexico, USA),Ph.D. (Tel-Aviv) (until July, 2000)B.A.Sc., M.A.Sc., Ph.D. (British Columbia)B.Sc., M.Sc., Ph.D. (Saskatchewan)(until July, 2000)

R.L. GattingerI. Oznovich

D.R. McDiarmidD.P. Steele

Institute of Space and Atmospheric Studies StaffProfessional Research Associates

D.A. André

C.-S. Huang

I.K. KhabibrakhmanovN.D. LloydC.E. Meek

B.Sc. (Erlangen-Nurnberg), Ph.D. (Georg-August,Germany), P.Eng.B.Sc. (Huazhong, China), M.Sc., Ph.D. (Hefei, China)(until September, 2000)M.S. (Hons.), Ph.D. (Moscow) (until July, 2000)B.Sc. (Hons.), Ph.D. (London)B.A. (Queen’s), M.Sc., Ph.D. (Saskatchewan)

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Research Assistants

T.R. FultonW.R. McMurray

J.K. Taylor

B.E. (Saskatchewan)B.Sc., B.Ed. (Manitoba), Data Assistant/ArchivistB.E., M.Sc. (Saskatchewan)

Research Engineer M.J. McKibben B.Eng., M.Sc. (Saskatchewan), P.Eng.

ISAS SecretaryB.Sc. (Hons.) (Saskatchewan), ISAS TechnicianISAS Assistant

D.M. JaroslawskyW.L. Marshall

S.F. Pfeil

Technical and Support Staff

Graduate StudentsPost-Doctoral Fellows (Supervisor)

S. Petelina (Llewellyn)

M.Sc. Students (Supervisor)

T. Chshyolkova (Manson)

B. Hesman (Davis)

M.M. (White) Hunt (Llewellyn)

E. Ivanov (Llewellyn)

K. Toews (Sofko/McDiarmid)

B. Wilcox (Llewellyn)

Influences of Airglow upon the dynamics of the MLTregion

Ground-based Planetary Spectroscopy - James ClerkMaxwell Telescope (JCMT) project (since March 2000)

Odin-Stratosphere and lower mesosphere aeronomy(until August, 2000)

A sensitivity analysis of the OSIRIS system perform-ance to misalignments that might occur during launch(until May, 2000)

SAPPHIRE studies of Ps6, (pulsations), PMSEs,sporadic E (polar mesospheric summer echoes)(until August, 2000)

Odin Ground-based Validation

7ISAS 2000

Odin Aerosol Studies

Summer Students (Supervisor)

A. Bourassa (Llewellyn)T. Lengyel (Llewellyn)

P. Marttala, (Hussey) T. Roschuk (Llewellyn)T. Wiensz (Hussey)

Ionospheric conductance effects in high-latitudephenomenaPlasma processes in the high-latitude ionosphere asseen by coherent radarsStudies of F-region echoes and field-aligned currentsusing SuperDARNInfluences of planetary waves upon the dynamics ofthe MLT regionTheoretical and experimental studies of E-region plasmawavesSuperDARN-derived plasma convection: Comparisonwith other measurements and application to field-aligned current studies

Ph.D. Students (Supervisor)

L. Benkevitch (Koustov)

D.W. Danskin (Koustov)

J. Liang (Sofko)

Y. Luo (Manson)

R. Makarevitch (Koustov)

L. Xu (Koustov)

Chair�s Report

ISAS is one of 4 research units or groupswithin the Department of Physics and EngineeringPhysics (PEP); the others are the Plasma PhysicsLaboratory, Material Sciences (associated with theCLS), and Sub-Atomic Physics. ISAS is the largestUnit. Our professors are appointed to PEP, andassociated with that have significant teaching andadministrative tasks (including College andUniversity). For our research, we use ISAS as a focusfor facilities, administrative services, the teaching ofSolar Terrestrial Physics (STP) graduate courses, andcollegial interactions. However, the health and viabilityof PEP must be strong if ISAS and the othe r researchunits are to be successful.

Professor Akira Hirose (Plasma LaboratoryDirector) continued as Head of the Department, andis now in his second year of a three-year term. Weare fortunate to have such an effective and diligentperson in that position, and one who has givenvaluable support to ISAS. The Chair’s 3 year termwas completed on June 30th, and so considerationwas given in May to the Report prepared by the chairfor 1997-2000, and his views on the future. Followingcareful discussion the Executive asked ProfessorManson to continue for another term, providing thathe did not continue to serve on the Department’sManagement Committee. There was concern thatthis additional activity could lead to conflicts of interest

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The three themes of the Terrestrial“Atmospheric Environment” (0-100 km), theTerrestrial “Space Environment” (ionosphere,thermosphere, magnetosphere) and of “PlanetaryAtmospheres”, continue to be the focus of researchwithin the Institute of Space and Atmospheric Studies(ISAS). The work has prospered, due to the energeticleadership of our seven Professors, who also act asthe Executive and as Principle Investigators (PIs) forthe main programs of ISAS. The research activitiesare based upon a strong and diverse set of

observational systems, including ground-basedradars and optical systems; and optical systems onaircraft, rockets and space vehicles. The analysis ofthe data from these systems leads to complementarytheoretical and modelling activities, and strongnational and global collaborations. This report givesan overview of ISAS research progress for thecalendar year 2000. This Chair’s Report summarizessignificant events and links them to the researchprograms of our community.

An Eventful Year in the Department and the Institute

in the future. Alan Manson, who had agreed to serveanother term (but who had remarked that this wasvery likely his last term), welcomed the reduction inAdministrative duties and agreed to the request. TheDeans and Senior Administration Funding, Staff andPrograms were so informed of our recommendation,and agreement followed.

‘Priority Areas’ were developed at theUniversity in 1998/9, to optimize the effectiveness ofsome research units and groups, and to develop newareas. Because scientific modeling has become suchan essential part of Solar Terrestrial Physics, and ofISAS programs, the chair promoted this notion, whichwas enthusiastically supported by others. ACommittee representing PEP, and most other sciencedepartments in the College, eventually prepared aproposal for an “Institute of Scientific Modeling” (ISM)in 1998 and 1999; it was finally submitted in 2000 asan “Institute of Complex Systems”. The selectioncommittee thanked us for the Proposal, naming it asone of those which would have been supported withextra monetary resources. The loss was verydisappointing, as it would have represented the largestmulti-disciplinary Institute in the College of Arts andScience, and have been the first of its type in Canadawhere a program of teaching and research camebefore the acquisition of a large computer.

9ISAS 2000

As this Report is being written (May 2001),we have welcomed our new Dean of the College ofArts and Science, Ken Coates, and the new AssociateDean (Science Faculty), Keith Taylor. Both havealready visited ISAS, and have listened to our SciencePresentations and toured the Facilities. The new‘Divisions’ in the College mean that the Sciences willhave more independence and responsibility. We havewaited since 1997 for a ‘permanent’ Dean and thisnew structure, and we look forward to working withboth of these gentlemen and our colleagues in theother Science Departments.

Canadian Research Chairs

There was considerable activity involving theChair, the ISAS Executive, and the UniversityAdministration on the theme of what was originallycalled the “21st Century Chairs for ResearchExcellence”, but became the “Canadian ResearchChairs” Program. We advertised globally throughout2000, to alert prospective candidates to the expectedopportunities. The Executive met in June, a sub-committee brought forward recommendations to aSeptember meeting, and our top two candidates wereinvited to ISAS/PEP in the Autumn. There were 20candidates, many of excellent quality, but the twochosen were truly outstanding and represented the

Canadian Space Agency (CSA) Programs2000 Developments

The CSA continues to have major influencesupon Atmospheric and Solar Terrestrial Physics inCanada and upon ISAS. The Chair representedSaskatchewan and Manitoba, and in particular ISASand associated high technology companies, on theSolar Terrestrial Relations Advisory Committee(STRAC), which was renamed the “Space andAtmospheric Environments Advisory Committee”(SAEAC) for the year 2000. Before and at the firstSAEAC meeting at Ottawa in May there was muchdiscussion about the perceived need for each of thetwo Environments to have more independence, focusand budgetary responsibility. After hours ofconstructive debate it was agreed that SAEACrecommend there be a continuing SAEAC, but withsub-committees and Chairs for each of the

areas of Space and Atmospheric Environmentsrespectively. The University had been working inparallel, and provided the “Strategic Research Planfor the CRC Program” on August 31st. This includedsix ‘thrusts’, including “Environmental Sciences”,which contained a “focus” of “Conservation andClimate Change”. Acting Dean Dick Neal played apivotal role at these early stages, and input to himand to V-P (Academic) Michael Atkinson led to ISASbeing mentioned specifically in the “Plan”. It is hopedthat the “Space Environment” will also be included insubsequent revisions of this “Plan”.

The University chose to put major emphasisfor the first year’s (2000) CRC Program “decisionpoints” upon in-house candidates, and thenominations from the University in the Autumn weretherefore submitted without a ISAS candidate.However we were encouraged by the Head and theActing-Dean to continue to promote a candidate.During 2001 “Theme Committees” will be active foreach of the six “thrusts” of the Strategic Plan, andwith Departmental approval of the ISAS nominee (whowas chosen from our two top candidates) occurringin Jan 2001, we will work towards having that nomineeselected by the Theme Committee for the 2001University nominations for a CRC in AtmosphericEnvironmental research.

two Environments. There would be SAEAC meetingsover two days, with Agenda-time for meetings of thetwo groups, as well as for plenary sessions. Themembers of the CSA “Space Science Program”(SSP), particularly David Kendall (A/Director ofProgram Development), Rejean Michaud and WilliamLiu (Scientific Secretaries for the Atmospheric andSpace Environments) worked throughout 2000developing this new structure, and in working withthe Meteorological Service of Canada to ensure thisother major stakeholder was fully involved with theAtmospheric Environment sub-committee. There willbe an ISAS person for both of the new sub-committeesof SAEAC. The first meeting will be during the springof 2001, when we will enjoy beginning to work withinthis new committee. At the May meeting of 2000

Plans for the activities of the two Environments werealso presented and discussed; these offer manyopportunities for ISAS Scientists. There was alsodiscussion of the proposal for the “CSA-SpaceScience Fellowship Program”, which offersopportunities for young scientists to establish goodcareer paths within the Universities. This could be ofvalue to ISAS as we look toward the retirement of 3of our senior professors within 5-7 years. TheInstitute’s research on Planetary Atmospheres isassociated with the “Space Astronomy” Program“within the CSA, and the JSSA (Joint Sub-committeeon Space Astronomy) is the Advisory committee. It ishoped that the Planetary Astronomy members of thisCommittee, and also of the “Space ExplorationAdvisory Committee” which is involved with space-craft which fly to Mars, will meet on occasion withSAEAC, since many of the community it representsare interested or already involved with PlanetaryScience.

Ongoing Collaborations with the CSA

During 2000 the developments of the existingsatellite programs continued strongly: Odin (withCanadian systems OSIRIS; Ted Llewellyn, PI) andMOPITT (Gary Davis, Science Team). DougDegenstein has now become involved with theairborne version, MOPITT-A, as Gary Davis placesmore emphasis upon his Planetary Sciencesresearch. These systems are discussed in somedetail in the Scientific Programs section. Odin focusesupon middle atmosphere aeronomy, and MOPITTupon tropospheric pollution. We must mention thatat the time of writing in Spring 2001, Odin has beensuccessfully launched and is acquiring superb data.The Odin CSA-contracts and an NSERC-CSP areproviding for considerable technology transfer,opportunities for training and education, and for SolarTerrestrial Physics (STP) science. A MOPITTNSERC-Strategic Projects grant is also providing asignificant impetus for atmospheric science activity.There have also been two successful new initiativesin Planetary Astronomy (Atmospheres) for which GaryDavis is the P-I: the SPIRE (Spectral and PhotometricImaging Receiver) program for the European SpaceAgency’s FIRST observatory (Far Infrared andSubmillimetre Telescope) has been approved; and a

The SAEAC committee is the CanadianNational Committee for COSPAR, the InternationalCommittee On Space Research. As part of thisresponsibility the CSA-SSP staff produced amagnificent Canadian Report (1998-9) for the 33rd

COSPAR Scientific Assembly in Warsaw (July, 2000).The chair was delighted to contribute a significantsection on ISAS Research.

The remaining CSA-related activity for theChair was the further development of ‘CUISAE’, the‘Canadian Universities Institute for Space andAtmospheric Environments’, which had its genesis in1998. The web-site for CUISAE is within that of theInstitute’s. Two review lectures were presented atthe DASP-2000 meeting in Toronto (March), andCUISAE activity was incorporated into an InternationalSymposium (PSMOS–see below) held in Torontoduring May. Posters were sent out to all Physics andEngineering Physics Departments this year.

Concept Study MU (Measurements of the UnresolvedSpectrum of the Earth). These bring $250K to ISASover two years.

The CANOPUS program, which is the majorCanadian ground-based auroral network, continuedto involve ISAS scientists in national and internationalcollaborations. There are effective collaborationsbetween CANOPUS and the ISAS radar systems, e.g.SuperDARN, MF radars (see the Scientific Programssection). The various new Space EnvironmentDocuments (see the CSA-Space Science web-site)provide more opportunities for linkages between suchground-based systems (almost exclusively NSERCfunded) and CSA programs such as CANOPUS. Dr.Dieter Andre continued as the local system managerfor the new (CANOPUS) Alphaserver 1000/233 MHzand Mike McKibben takes responsibility for relatedAlphaserver/ISAS community linkages. Theyprovided assistance to local users as well as workingon the analysis of data. The Alpha-system, which isthe basis for much of the ISAS computing system,has now been “donated” to ISAS, which is nowresponsible for its maintenance and operation.

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The Natural Science and Engineering Research Council(NSERC)

ISAS 2000

Grants from NSERC provide the foundationfor ISAS research. There were several significantgrants awarded this year. George Sofko (with SashaKoustov and Glenn Hussey) were awarded aCollaborative Research Opportunity Grant for theCanadian SuperDARN work ($850K over 5 years);and Alan Manson was awarded a Research Grantfor “Dynamics of the Middle Atmosphere, using theSaskatoon MF Radar and Collaborations with SatelliteSystems and Networks” ($360K over 4 years).

The ISAS professors continue to provide‘User Fees’ for the support of ISAS services from their

The support and promotion of our Research,through the Office of Research Services, has beenvaluable during 2000. The Vice President (Research)is Dr. Michael Corcoran; the Director of ResearchServices is Julia Taylor; and the CommunicationsOfficer, Kathryn Warden. They have been helpful withregard to the promotion of ISAS programs. TwoSaskatoon companies, SIL (with Larry Cooper,President) and Kipp and Zonen Inc.(with BenDieterink, Research Scientist) worked with us thisyear. SIL provided research projects for the EP425course Engineering Physics Systems which was

research grants, in lieu of the now obsoleteInfrastructure Grants. These funds are additional tothe ongoing budget from the College of Arts andScience. This University of Saskatchewan seed-money is invaluable, and now includes some revenuesfrom ISAS contract-overheads. The College budgetencourages NSERC to provide these ‘user fees’, andthen allows for ISAS administrative services whichcannot be funded from any other NSERC-CSA-MSCsource. This ISAS Infrastructure budget is close to$80,000, while total revenues to ISAS PIs are $1.85million for use this year, with approximately$1.3 million remaining in ISAS.

Outreach: Technology Transfer

ISAS is well positioned in this regard. Wehave an effective and regularly upgraded web site(http://www.usask.ca/physics/isas/) which is linkedwith the CSA’s web site (http://www.space.gc.ca). Weare listed in SOURCES (for Editors, Reporters,Researchers), which has a hardcopy book, and alsoa web site. ISAS also has an entry in the CanadianTechnology Network (CTN), which is sponsored bythe NRC and Industry Canada, and providesCanadian business with links to technology (http://ctn.nrc.ca/).

Posters and other ISAS materials areregularly posted to all Canadian Physics andEngineering Physics Departments and to 3rd and 4thyear students to encourage more graduate students

convened by the Chair. Both students and industrialpartners enjoyed and benefited from this activity. SILare also involved with the development of the CADIradar (Canadian Advanced Digital Ionosonde:Professor John MacDougall, UWO). One of John’ssystems is now operating at the ISAS Park Site. AnIndustrial NSERC Scholarship between SCI-TEC(now Kipp & Zonen) and the University ofSaskatchewan, and involving Dr. Llewellyn and theOdin project, has been completed this year. Thegraduate of that program, Meg Hunt, is now workingat Kipp & Zonen in Saskatoon.

Outreach: Media and General to join our community. Materials developed by MarciaMain (ISAS Secretary) and the Chair during 1998/1999 were used. A redesign of these by our newSecretary Debbie Jaroslawsky (May 2000) was begunduring 2000. Copies of these are also readily availableupon request.

These new materials were also used by thePhysics students who attended CUPC (CanadianUndergraduate Physics Conference) at the Universityof Laval in Quebec City during November, for theirGraduate Studies promotional event. Graduatestudents interested in working in ISAS can completedegrees in the disciplines of Physics, EngineeringPhysics or Environmental Engineering.

Funding, Staff and Programs

The diversity of research programs supportedby ISAS means that funds from NSERC and the CSAhave been sought and secured. This has allowedthe programs of ISAS to flourish despite some difficultyears earlier in this decade. The economic recoveryof Canada has already had significant effects uponthe CSA and NSERC, and we have felt the results ofthis already.

The research and core staff have compriseda total of approximately 30-35 persons during the lastfew years, figures closer to that of ISAS in the pre-CNSR years (1989; 30 persons). Our numbers havegrown recently due to strong CSA programs andSuperDARN. There are (2000 average) 7 PIs(Professors), 2 Adjunct Professors, 5 Post DoctoralFellows/Research Associates, 4 Engineers/ResearchAssistants, 3 Staff-persons (Technician, Assistant-stores and finances, Secretary) and 11 graduatestudents. Several other Graduate students (circa 5)will join us in 2001.

The ISAS staff form an effective andproductive group, with strong national and globalcollaborations due to the diversity of our programs.Graduate students, Research Scientists andEngineers learn the skills of developing state-of-the-art experimental systems, of analyzing data usingsophisticated software and powerful computingsystems, and of preparing research reports and

There were two major Research activities oncampus during the year at which ISAS participated:the Research Committee of Council organized“Building Research Success at the University ofSaskatchewan” in January, where we had a largeposter; and “Experience US” in February, whenstudents, teachers and parents from around theprovince attended. Our professors have writtenseveral articles for, and have been interviewed by,staff from the local newspaper, the StarPhoenix; andhave had articles in the University’s Campus New.

Finally, the video-conferencing systemoperated during 2000 from the ISAS ConferenceRoom. The MOPITT team (Jim Drummond,University of Toronto, PI) has provided this systemsince regular team meetings are considered essential,and ISAS is providing operating costs. The systemis available for ISAS and PEP staff. The potential forthis system is very considerable, and will be a verypowerful outreach mechanism.

papers. The research environment for our Professor-PIs is extremely competitive, as they are alsocommitted university professors, with normal teachingand administrative duties; our competitors in theUnited States and Europe are often full-timeresearchers.

We have 7 professors, 5 of whom areProfessional Engineers (Drs. Llewellyn, Sofko,Koustov, Hussey and Degenstein), with a desirableblend of youth and experience. Those five form astrong leadership unit for the Engineering Physicsprogram in the Department. Our active AdjunctProfessors are a very active and valuable resource:Drs. Dick Gattinger (Odin, Ted Llewellyn); and DonMcDiarmid (SuperDARN, George Sofko).

The seven PIs provide a very well balancedcoverage of the STP area. In the “AtmosphericEnvironment”, we study the chemistry and aeronomyof the lower atmosphere (troposphere 0-20 km); thechemistry, thermal structure, and dynamics of themiddle atmosphere (30-100 km); the coupling betweendynamical processes, atmospheric waves, andthermal and chemical ‘structures’; and the compositionand structure of planetary atmospheres (ProfessorsLlewellyn, Manson, Davis and Degenstein). Thesetopics relate to “Global Climate Change”, and includethe effects of solar variability and of changingconcentrations of Ozone and Green-House Gases

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(GHG) upon the Atmospheric Environment. In the“Space Environment”, we study the plasmainstabilities of the E- and F-regions of the ionosphere;the convection patterns of the ionosphere/thermosphere as they respond to the disturbed sunand magnetosphere; the response of themagnetosphere and geospace-plasma to solaractivity; the drifts of meteor trails in the D- and E-regions; and the effects of atmospheric waves uponthe thermosphere (Professors Hussey, Koustov andSofko). The coupling between the “Space” and“Atmospheric” Environments is also studied byDrs. Hussey and Manson. These topics relate to“Space Weather”, “Space Climate” themes, theireffects upon space vehicles and energy-distributionsystems on planet Earth, and have as a goal thedevelopment of a prediction capability.

ISAS 2000

Within Canada’s “Space Science”community, the two major themes are also “SpaceEnvironment” and “Atmospheric Environment”, soISAS contributes fully to the national agenda. Theprinciple influences upon our PIs are already evidentfrom the preceding sections of this report and areelaborated upon in the Scientific Programs Section;MOPITT, ISO and FIRST satellites, plus the JamesClerk Maxwell telescope, for Gary Davis; the Odin-OSIRIS satellite for Ted Llewellyn and DougDegenstein; WINDII and TIMED satellite missions,MF Radars, along with new SCOSTEP and CEDARinternational studies and projects for Alan Manson;and SuperDARN, CANOPUS and relatedmagnetospheric satellite missions for George Sofko,Sasha Koustov and Glenn Hussey. Details of ourwork are provided in the Scientific Programs Section.

ISAS Facilities

The majority of the optical and radar systemssupporting the programs of the Institute are at thefield sites described below. There are a number ofadditional systems which have been developed orpurchased with Institute funds, or are operated forcolleagues by ISAS staff. These include the following:

Three-component Magnetometer and ULFSystem

The fire at Park Site on July 13, 1999 destroyedthe 3-component magnetometer and ULF system,which was operated for the University of Tokyo.

T.V. All-Sky CameraThis has the following features: 2 filters and

shutter to allow observations of specific wavelengths;PC control for automatic field use; a photo-sensor forcomputer failure. This all-sky camera was returnedto ISAS and is awaiting deployment to another fieldsite.

Observatory FacilitiesMeridian Scanning Photometer (multi-wavelength) MSP

Five single-channel photometers areincorporated into this (Iwan Goza for Dr. McEwen,during 1992/93). It is PC (IBM-compatible personalcomputer) controlled. This MSP has been located atboth La Ronge and Rabbit Lake, for Dr. McEwen’sCNSR/STEP research; it is now at Rabbit Lake (sincethe Spring of 1995).

Spectral Airglow Temperature Imager(SATI-2)

In December 2000 a SATI-2 Imager beganoperating in the penthouse observatory on the roof ofthe Physics Building. The equipment is on loan fromthe Institute for Space and Terrestrial Science YorkUniversity. The instrument measures perturbationsof the rotational temperatures and vertical columnemission rate of the O2 Atmospheric nightglow layerat 94 km and the OH Meinel layer at 86 km.

Rabbit Lake (58°20' N, 103°70' W)This site was extensively used from 1985-1990

as part of the HILAT and VIKING satellite activities.A new trailer, obtained with CNSR funds, was locatedat Rabbit Lake during 1992 with a TV all-sky camera.The system was upgraded to a digital recordingcapability in the Fall of 1993, and operated until Springof 1996 with visible, red and green filters. The sitealso supports a CADI phase-coherent ionosondesystem from the University of Western Ontario and amagnetometer (for collaborations with JapaneseColleagues).

Park Site (52°12' N, 107°7' W)The field site near Asquith continues to be used

by the Atmospheric Dynamics Group with their large

Field Sites

MF (2.2 MHz) radar system. This has extensivetransmitting and receiving antenna systems forspaced antenna and interferometry studies of themesosphere and lower thermosphere (60-110 km).Turbulent scatter and meteor trails are used to providewinds, atmospheric waves and turbulence data aswell as ionospheric data from D-, E- and F-regions.This internationally recognized system is fullyautomated and requires only occasional maintenance;this is normally provided by weekly visits. Data aremade available to collaborators in International (e.g.STEP, MLTCS) and National (e.g. CNSR) programs.

The 160-acre site is leased from a local farmer,Mr. Charles Chappell, on a long term rentalagreement. On July 13, 1999, a fire caused bylightning destoyed two of the three bays of the mainreceiver building. The other wing, the MF Radar wing,

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suffered extensive smoke and water damage. Thetwo fires damaged wings were demolished and theother wing was cleaned and restored. The MF Radartransmitter and receiver systems both had to undergoextensive cleaning before being returned to the field.A new building was completed in April 2000. It wasattached to the existing MF Radar Wing. The newbuilding has a 600 sq. ft. cold storage area and a 600sq. ft. working area. The new working area alsocontains the optical dome.

Bakker�s Farm (52°15' N, 106°27' W)In May 1997, SAPPHIRE operations were

terminated at the Bakker Farm site. The associatedSAPPHIRE transmitter sites at La Crete, Alberta andGilliam, Manitoba were decommissioned inSeptember 1997. The 6- and 2-meter antennasystems have been left standing to be used on acampaign basis. The building, complete with opticaldome, remains ready to be used with either the radaror optical experiments.

Kernen Farm (52°9' N, 106°32' W)The Kernen Farm is the site of the Saskatoon

SuperDARN system. The site is comprised of twoantenna arrays:1. The main array: 16 log-periodic antennas mountedon 15 meter towers. Each connected to a 600Wpulsed transmitter.2. The vertical interferometer array: 4 log-periodicantennas mounted on 15 meter towers connected toan independent receiver to allow angle of arrivalcalculation.

Prince George (53°59' N, 122°35' W)A new SuperDARN radar was built in 1999 on

a site 15 km east of Prince George, British Columbia.The radar system is identical to the SuperDARN radaroperating in Saskatoon. The radar has two antennaarrays: a main transmitting array and a verticalinterferometer array. The radar point 5° west of northand is paired with a U.S. run radar on Kodiak Island,Alaska.

Recent changes to the computing facilities atISAS include an upgrade of the ISAS node ofCANOPUS (Canadian Space Agency) by theinstallation of an Alphaserver 1000/233 MHz(managed by D. André and M. McKibben), and theacquisition for the SuperDARN analysis of an HP9000/715 (managed by D. André).

The recent additions of computer equipmentcomplement the present systems available. TheUniversity provides a wide variety of services, throughits Computing Services department, at quitereasonable costs; the system is primarily VAX/VMSbased. Also, there is an IBM RS6000/340 workstationwhich was supervised by Dr. N. Lloyd. The Physicsand Engineering Physics Department provides a LANmanager-based file server for PC-based programsand data storage.

The scientists, engineers, graduate studentsand core staff all have PC 486/586/686 systems whichare connected by Ethernet to the major computers:University network, CANOPUS microVAX andALPHA, IBM RS6000/340, and HP 9000/715. Manyof the PC’s are running Windows for Workgroupssoftware which enables the sharing of printers anddisk space amongst PC users. Some of the PC’s arerunning LINUX, a unix type operating system for PC’s.Electronic-mail (e-mail) services are provided by eachof the major computer systems. These include theSPAN e-mail access, provided by CANOPUSmicroVAX and ALPHA, to the majority of the CanadianSolar Terrestrial Physics Community who are involvedwith CANOPUS. The 8 mm tape copying facilityenable the production of SuperDARN data tapes fordistribution to national and international colleagues.

Finally, most of the Institute’s observationalsystems have the capability of real-time analysis ofdata by dedicated PC systems, which has minimizedthe need for major main-frame computers or evenwork stations. The MF radar at Saskatoon(Atmospheric Dynamics Section, Dr. Manson), theVHF radar transmitter/receiver system known asSAPPHIRE, the SuperDARN MF radar at the KernenFarm, and the Rabbit Lake/Rankin Inlet All-skyCamera, are each computer controlled and generateprocessed data. These are then ready for detailedanalysis. In addition, the engineers within ISAScontinue to demonstrate leadership by the use oftransputer technology.

Computing Facilities

ISAS 2000

An Institute with such extensive observationalsystems, and data analysis programs, requiresconsiderable computing facilities. A wide range ofcomputer systems is available to ISAS scientists andgraduate students.

Optical And Electronic Laboratory Facilities

Particle Calibration Facility Electronics and MechanicalStores Facility

Comprehensive electronic and mechanicalstores were maintained for ISAS researchers through2000 by Shirley Pfeil (Dept. Assistant), who wassupported from ISAS funds (100%). Shirley’s hoursremain at .80 FTE. Materials and components areprovided at cost and this has been of significantpractical assistance in research programs. Turn-overof parts and purchase of equipment, and other relatedexpenses in the year 2000 lead to in excess of a halfmillion dollars in activity.

ISAS accounting is handled by Shirley. Sheprovides in-house monthly and annual budgetsummaries for all ISAS accounts, which aresupervised by herself and the ISAS Chair.

The Optical Laboratory is under the directionof Bill Marshall and continues to provide generalsupport for the research programs within the Institute.There are optical calibration standards for visible, UVand IR (200-900 nm). Low brightness sources (LBS)in the UV and IR were developed during the CNSRfor medical research (ozone) and stratosphericmeasurements. In particular, calibrated detectorswere obtained for the UV-A and B regions, and therewas testing of sources and detectors over the 200 to400 nm range.

The Electronic Laboratory has network andspectrum analyzers, signal generators and testequipment to allow development of state of the artVHF/HF/MF radars. Marshall also maintains thiselectronic test equipment and develops new systems/sub-systems for the optical and radar facilities of ISAS.Marshall is supported by ISAS funds (50%), NSERCfunds from the MF radar group and the HF/VHF radargroup.

Projects of particular note include the following:• SuperDARN system support• Park Site MF radar system maintenance and

development, and• General support for the electronic/mechanical

needs of 32-35 ISAS personnel• SATI-2 system management

The basis of this facility is the Canadian SpaceAgency electron calibration system (1-400 eV), witha cryogenically pumped vacuum chamber and cleanroom which was developed for FREJA-CPA, but hasalso been used for various rocket systems. Thisfacility is within the Optics Lab. It will allow calibrationsfor electron energies of up to 25 keV, which are ofvalue for satellite and rocket systems sampling auroralelectron populations.

16

17

Research Programs

Planetary Astronomy

Atmospheric Dynamics

Magnetosphere/Ionosphere Interactions

Ionospheric Physics

Aeronomy Research

ISAS 2000

19

G.R. Davis

Planetary Astronomy

Team MembersResearch Assistants: T.R. Fulton (LWS project)

J.K. Taylor (MOPITT and SPIRE projects)Graduate Student: B.E. Hesman (JCMT project, from March 2000)

ISAS 2000

Introduction

The recent detection of planetary companionsaround other stars raises some fundamental scientificquestions. Are planetary systems common in theuniverse, for example, or is the existence of our ownunusual? Is the Solar System a good template forother systems, or is it an exception, as discoveriesso far seem to indicate? Finally, and perhaps mostimportantly, might the environmental conditions forthe development of life be prevalent elsewhere?Recent technological advances have made it possibleto investigate these challenging questions, and thequest is likely to become a major scientific theme ofthe 21st century.

The study of our own planetary system is avital component of this line of inquiry. Not only is it theonly system we can observe at relatively close range,but to the extent that it serves as a template forplanetary systems in general (which is yet to beestablished), it can be used to constrain theoreticalmodels of planetary formation and evolution. Theindividual members of the system furnish importantclues to its formation, and demonstrate the range ofpossible evolutionary pathways (e.g., runawaygreenhouse effect on Venus, atmospheric escape onMars).

The best tracers of planetary formation andevolutionary processes are the relative abundancesof the elements and isotopes which make up theplanets, and the technique of choice for measuringthese abundance ratios is infrared molecularspectroscopy. The projects described below are alldirected towards this goal.

Long Wavelength Spectrometer (LWS)

The LWS was was launched in November 1995on the Infrared Space Observatory (ISO), an ESAcornerstone mission for infrared astronomy, andoperated successfully until the on-board cryogen(liquid helium) was exhausted in April 1998. It used agrating and a Fabry-Perot interferometer to providespectroscopic capability over the spectral range 45-180µm. Since these wavelengths are completelyinaccessible from the ground due to absorption in theterrestrial atmosphere, this mission provided anunprecedented opportunity for the spectroscopicdetection of many important planetary constituents.The LWS consortium comprises scientific researchinstitutions in the U.K., France, Italy, the U.S.A. andCanada; I am the only Canadian Co-Investigator. TheLWS Solar System team, which I lead, comprisesmembers in Canada, the U.K., Spain, the U.S.A. andFrance.

Last year I reported that the primary scientificobjective of the LWS planetary programme is tomeasure the D/H ratio in the atmospheres of the giantplanets. This number is cosmologically importantbecause, for Jupiter and Saturn, it should berepresentative of the D/H ratio in the primordial solarnebula from which the solar system formed.Deuterium was produced in the big bang, is destroyedin fusion processes in stellar interiors, and is notregenerated by any known mechanism. The D/H ratioshould therefore decrease with time over the age ofthe universe, and its value at the time of solar systemformation is a critical parameter with which to constraincosmological and galactic evolutionary models. The

Figure 1. Emission line of water vapour in the stratosphere of Jupiter, detected with the LWS in its high-resolutionmode.

LWS is uniquely suited to determine this quantitybecause it can measure the first two rotational linesof HD (an isotope of molecular hydrogen, which isthe primary constituent in giant planet atmospheres)at 56 and 112 µm; these lines are not accessible usingany other technique. The R(0) line was measured inUranus and Neptune in the LWS grating mode andthe R(0) and R(1) lines were measured in Jupiter andSaturn in the LWS high-resolution mode. Analysis ofthese data has proved very challenging because of anumber of instrumental factors which must be takeninto account; this was our highest priority in 2000 andwork is continuing on both sets of HD measurements.

A second area of analysis was the unexpecteddiscovery of H2O emission lines in the upperatmospheres of Jupiter and Saturn. An example isshown in fig. 1. The existence of water vapour in thestratospheres of these planets (also discovered in

Uranus, Neptune and Titan using SWS, anotherinstrument on ISO) indicates a flux of oxygen ontothese planets and potentially onto all bodies in theSolar System; potential sources are comets andinterplanetary dust. These observations wereanalysed in 2000 and are being combined with theSWS observations in collaboration with colleagues inFrance.

Finally, LWS observations of Neptune wereanalysed during 2000 and are shown in fig. 2. Althoughthe infrared spectrum of Neptune is dominated bymolecular hydrogen, it is slightly sensitive to the heliumabundance at 30 µm and 50 µm. Using data acquiredfrom space (using SWS and LWS) and from theground throughout the infrared, the temperature profilewas adequately constrained and global averagehelium abundance was determined to be 16±6%(Burgdorf et al., 2000).

20

21

Figure 2. The infrared spectrum of Neptune. The diamonds are from ground-based observations; the squares arefrom ISO/SWS; the closed circles are from ISO/LWS; and the open circles are also from ISO/LWS, but are less reliablefor technical reasons. The spectrum is dominated by molecular hydrogen but is slightly sensitive to the presence ofhelium.

ISAS 2000

Ground-based Planetary Spectroscopy

This complementary project consists of anongoing series of measurements of planetaryemission spectra at submillimetre and millimetrewavelengths (300 µm—1.1 mm) using the 15 mJames Clerk Maxwell Telescope (JCMT) on MaunaKea, Hawaii. Broad-band, incoherent spectroscopyfills an important niche since tropospheric absorptionlines in planetary spectra are pressure-broadenedto widths well in excess of coherent receiverbandwidths. A polarising Fourier transformspectrometer (FTS) was designed and built for thesemeasurements by a collaborator at the University ofLethbridge, Dr. D.A. Naylor, and is used inconjunction with a dual-polarisation 3He bolometricdetector system.

Last year I reported the first detection of then=20—19 Rydberg line of neutral hydrogen in the Sunat 29.622cm-1, the highest n-value of hydrogen everdetected. The obvious next step was to search forthe n=22—21 line at 22.096 cm-1, which occurs in

the 450 µm atmospheric window and should beobservable from Mauna Kea under good atmosphericconditions. Using an identical observing strategy asfor the earlier line, we recorded a set of solar spectraas part of an observing run in December 1999. Thesedata were analysed in 2000 and the line was detectedas excess emission at the solar limb relative to thecentre of the Sun. This represents the first detectionof this line and is, again, the highest n-value ofhydrogen ever detected in the Sun. This discoverywas reported by Clark et al. (2000).

Our next observing run on the JCMT was inDecember 2000. The scientific objectives of this runwere (a) to refute a claimed detection of HCl in theatmosphere of Saturn, and (b) to carry out a spectralsurvey of the Orion A molecular cloud with the FTSand a heterodyne receiver. Although the weather waspoor during our three nights on the telescope, werecorded a full data set which will be analysed during2001.

Measurements of the Unresolved Spectrumof the Earth (MUSE)

In response to a CSA Announcement ofOpportunity for Concept Studies in Space Astronomy,I submitted a proposal for MUSE in February 2000.The concept is to place a spectrometer on amicrosatellite into a high, polar orbit around the Earthin order to measure the spatially-integrated infraredspectrum of the planet and its dependence ongeography, season and phase. This is essentialprecursor information to future missions, currentlybeing planned, to measure the infrared spectra ofextrasolar planets. The objective of these futuremissions is to search for evidence of life elsewhere inthe universe through biological modification ofatmospheric composition. MUSE was selected forstudy, and the work will commence in January 2001.

Spectrometric and Photometric ImagingReceiver (SPIRE)

Like LWS, SPIRE is a general-purpose space-borne instrument for astronomical spectroscopy.SPIRE will provide imaging photometry and imagingspectroscopy (resolving power up to 1000) over thesubmillimetre spectral range 200—670 µm. This is akey spectral region for studying stars in the earlieststages of formation, when they are still coupled to theinterstellar medium; for studying galaxies in the earlyuniverse, which emit the majority of their energy inthe submillimetre due to the combined effects of highredshift and reprocessing of stellar ultraviolet by colddust; and for studying the formation and evolution ofSolar System objects. SPIRE is being designed andbuilt by a consortium of scientific institutions in 7countries (Canada, France, Italy, Spain, Sweden, theUK and the USA), and is scheduled for launch onESA’s Herschel Space Observatory (HSO) in 2007.I am the PI for Canada’s participation in this project:our contributions will be a cryogenic shutter for theinstrument and personnel for the Instrument ControlCentre. The project is financially supported by theCanadian Space Agency.

The cryogenic shutter is required becausethere will be a 2.5-year interval between spacecraftintegration and launch, during which the flightconfiguration will not be simulated. Since the SPIREdetectors will be optimised for the flight situation, theywould not operate correctly in the pre-launchenvironment and instrument tests during this periodwould not be possible. The solution to this problem isto put a shutter in the instrument which will close forground-based instrument tests and open permanentlybefore launch.

Most of the effort during 2000 was directedtowards initiating the shutter design. Joe Taylor and Ivisited several collaborating groups in Europe andestablished an initial set of requirements. These wereused as the basis for a design study contract to be letby the CSA in early 2001.

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23

Atmospheric Dynamics

A.H. Manson

Team MembersResearch Associate: Dr. C.E. MeekResearch Assistant: R.A. McMurrayTechnician: B. MarshallGraduate Students: Y. Luo, T. Chshyolkova

Introduction

The Atmospheric Dynamics Group is stronglyinvolved with ISAS, Canadian, and Internationalprograms. The region studied, the upper MiddleAtmosphere or Mesosphere Lower Thermosphere(MLT, 60-150 km), is strongly affected by not onlysolar and auroral disturbances but also weather-related tropospheric/stratospheric disturbances frombelow. National and International programs such asCEDAR (Coupling, Energetics, and Dynamics ofAtmospheric Regions - U.S. sponsored), andSCOSTEP (Scientific Committee on Solar TerrestrialPhysics) with its new programs (below), demonstratethe importance of the MLT region and the relevanceof the ISAS work. Indeed Canada has become aleading nation in Middle Atmosphere research, withsponsorship by NSERC, the Meteorological Serviceof Canada (MSC) and the Canadian Space Agency(CSA).

The basis for our MLT research is theSaskatoon medium frequency radar (MFR, 2.2 MHz),operating in spaced antenna and interferometrymodes at the Park Observatory. It provides profilesof the horizontal and vertical wind, and of atmosphericwaves, in real time and continuously. The samplingrate for profiles is 5 minutes, with 3 km samples from60/75 - 100/110 km (day/night). This main radar

ISAS 2000

facility was refurbished in 1997, using funds from anNSERC equipment grant. The system is now readyfor another decade of operation. The second of ourMF radars has been located at Platteville 40°N (theBoulder Aeronomy Research site) since December1999. Our colleagues, Drs. Susan Avery and DeniseThorsen (University of Colorado) have an NSF grantto support the operation of the system. We now have10 months of excellent data. The third MF radar atTromsø involves three Universities: the University ofSaskatchewan, the University of Tromsø (AuroralObservatory) and the University of Nagoya. Data maybe seen at this web-site: http://atmos.phys.uit.no. Ourprinciple colleague from Tromsø is Dr. Chris Hall. Hehas effectively monitored the operation of the MFR,and lead the research for several innovative studies.The members of the ISAS group are Drs. Alan Mansonand Chris Meek, principle scientists; Yi Luo, Ph.D.graduate student and research assistant who isstudying planetary waves in the middle atmosphere;Tatyana Chshyolkova, M.Sc. graduate student, whois studying dynamic influences on the airglow, usingthe SATI-imager on loan from our colleague Dr.Gordon Shepherd (York University); and RonMcMurray and Bill Marshall, research assistant(archiving; data analysis) and technician respectively.

International Programs

The new SCOSTEP programs, (1998-2002),have been very active in 2000. The first of these isS-RAMP (STEP Results, Applications and ModellingPhase). It has two major themes, which are tocomplete studies based upon observations duringSTEP (1990-1997) and to select observing intervalsfor new campaigns. These will be called “spaceweather” campaigns and will emphasize coupling inthe solar-terrestrial system from the Sun, through themagnetosphere, and down into the middleatmosphere and troposphere (Alan Manson is on theSteering Committee). Three of the Projects below usedata acquired during STEP. Some of these resultswere prepared for the COSPAR Assembly at Warsaw(July 2000), and the S-RAMP Conference at Sapporo,Japan (October 2000).

There has also been vigorous activity withinthe two other SCOSTEP programs in the post-STEPera (1998-2002): Planetary Scale MesopauseObserving System (PSMOS - Gordon Shepherd andMaura Hagan (NCAR - Boulder) PIs); and EquatorialProcesses Including Coupling (EPIC - ShoichiroFukao (Kyoto), PI). The MLT radars and opticals ofSTEP (MLT) have transferred their networkingallegiance to S-RAMP, PSMOS and EPIC to ensurethere is continued attention to vital matters of MAdynamics, aeronomy and coupling. The ISAS MFRsystems are playing strong roles in all of theseprograms. We led one paper on ‘airglow variability’(see below), and Alan Manson, Chris Meek and YiLuo provided strong support to papers on ‘Tidalstructure and variability’ led by Dora Pancheva(University College of Wales). We will report on thesepapers next year.

1 . Gravity Waves (GW)

In a paper from last year we studied windsand GW using six MF radars located from the Arcticto the Equator (Tromsø 70°N, Saskatoon 52°N,London 43°N, Urbana 40°N, Yamagawa 32°N, Hawaii22°N, Christmas Island 2°N), [Manson et al., EarthPlanets Space, pp 543.1999]. Frequency spectra andspectral variances (10-100 min, 2-6 hr bands) for theheight layer 76-88 km during 1993/4 were utilized.Differing doppler-shifting processes weredemonstrated at high and low latitudes. The result ofthis is that the winds effectively control the intensitiesof GW fluxes, and the latitudinal variations showstrong Semi-Annual Oscillations (SAO) at the higherlatitudes, and quite weak variations below 32°N.

Such relationships should also be evident inrealistic Global Circulation Models (GCMs), providingthey are run at temporal and spatial resolutionsappropriate to the GW fluxes and mechanisms. Thesemodels typically contain orographically-forced wavesof zero phase speed, waves resulting from non-linearand tropospheric processes (which are limited by theModel’s resolution), and parameterized GWs for theunresolved scales. The GCMs must contain theselatter GW fluxes if they are to reproduce thetemperature and dynamical fields and waves of thereal atmosphere. Unfortunately the results obtainedwith different parameterizations are not unique, andsomewhat similar results can be obtained withdifferent theoretical assumptions. We now show theAbstract for this new paper, which is submitted forpublication:

Scientific Projects

We will present brief summaries and figuresfrom the major studies of 2000. The phenomenadescribed will begin with Gravity Waves and thenproceed to longer time and spatial scales, and airglowstudies. The format chosen is to provide Abstractsfrom the papers, which are accepted, or submitted tojournals.

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Gravity Wave Activity and Dynamical Effects in the Middle Atmosphere (60-90 km): Observations from an MF/MLT Radar Network, and results from

the Canadian Middle Atmosphere Model (CMAM)

A.H. Manson a,*, C.E. Meek a, J. Koshyk b, S. Franke c, D.C. Fritts d, D. Riggin d , C.M. Hall e,W.K Hocking f, J. MacDougall f, K. Igarashi g, R.A. Vincent h

aInstitute of Space and Atmospheric Studies, University of Saskatchewan, Canada, bDepartment of Physics,University of Toronto, Canada, cSpace Science and Remote Sensing Laboratory, University of Illinois,U.S.A., dColorado Research Associates, Boulders, U.S.A., eAuroral Observatory, University of Tromsø,Tromsø, Norway, fDepartment of Physics and Astronomy, University of Western Ontario, Canada, gUpperAtmosphere Section, Communications Research Laboratory, Tokyo, Japan, hDepartment of Physics andMathematical Physics, University of Adelaide, Australia

Abstract

It has become increasingly clear that Gravity Waves (GW) have an essential and often dominant rolein the dynamics of the Middle Atmosphere. This leads to them having strong impacts upon thethermal structure and the distribution of atmospheric constituents. However, the observations ofGW have been limited in their latitudinal extent, so that climatologies of important characteristicsare arguably inadequate. With regard to models, the inclusion of GW-drag effects has been problematic.Usually no seasonal or latitudinal variation in the subgrid-scale GW-drag parameterization schemeis included, and varieties of parameterization schemes have been used. Although these often makeconflicting assumptions, they generally produce similarly acceptable end-products eg zonal-meanzonal wind fields. In this paper we report upon the beginnings of a substantial program, usingobservations from a network of MF radars (North America, Pacific and Europe), and data from theCanadian Middle Atmosphere Model (CMAM). This model allows the GW and tidal wave fields tobe assessed, characteristics and climatologies of which are well known from the MF Radars. Thereare useful similarities in the observed and modeled background wind and wave fields, and strongindications that the two non-orographic GW-drag parameterization schemes (Hines (H); Medvedev-Klaassen (MK)) have significant and differing effects upon the dynamics of the modeled atmosphere.

ISAS 2000

We include in figure 1 the hemispheric phase of the semi-diurnal tide for the two parameterizations.There are significant differences between the two. The MK is preferred and is shown in the paper to beremarkably similar to the MF radar observations.

Figure 1. T

he 12-hr tidal phase-contours from the C

MA

M experim

ent (H and M

K param

eterizations). The latitude num

bers range from 1(20°

N) to 7(70°

N); the local-

times are in hours on the contours.

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Seasonal Variations of the Semi-Diurnal and Diurnal Tides in the MLT:Multi-Year MF Radar Observations from 2-70 N, Modelled Tides

(GSWM, CMAM)

Alan Manson et al (The other authors were co-authors of the previous abstract. Maura Hagan(NCAR, Boulder, USA) was a new principle author, since she is the PI for the GSWM tides.)

Abstract

In an earlier paper (Manson et al. JASTP p809, 1999) tidal data (1990-97) from six Medium FrequencyRadars (MFR) were compared with the Global Scale Wave Model (GSWM, original 1995 version).The radars are located between the equator and high northern latitudes: Christmas Island (2N),Hawaii (22N), Urbana (40N), London (43N), Saskatoon (52N) and Tromso (70N). Commonharmonic analysis was applied, to ensure consistency of amplitudes and phases in the 75-95 kmheight range. For the diurnal Tide seasonal agreements between observations and model wereexcellent, while for the semi-diurnal Tide the seasonal transitions between clear solstitial states wereless well captured by the model.

Here the data set is increased by the addition of two locations in the Pacific-North American sector:Yamagawa 31N, and Wakkanai 45N. The GSWM model has also been further developed (2000) toinclude an improved gravity wave (GW) stress parameterization, background winds from UARSsystems, and monthly tidal outputs for better characterization of seasonal change. The other model,the Canadian Middle Atmosphere Model (CMAM) which is a General Circulation Model, providesinternally generated forcing (due to ozone and water vapour) for the tides. The two GSWM versionsshow distinct differences with the 2000 version being alternately closer to, or further away from,observations; overall the 1995 version is still to be preferred. CMAM provides results dependentupon the GW parameterization scheme inserted, but the best scheme provides very useful tides,especially for the semi-diurnal component.

ISAS 2000

2. Tidal Oscillations (2°-70°N)

Tides are particularly important in the lowerand middle atmospheres. Their forcing depends uponglobal ozone and water vapour distributions, whiletheir propagation, dissipation and the developmentof higher order ‘Hough modes’ (3D harmonics)depends upon global mean winds, temperatures andGW-related turbulence. In the MLT region (60-150km) these waves are usually dominant in terms ofamplitude, and they accelerate the mean winds, createturbulence, and modify the distributions of trace-gasconstituents. Observations are essential to helpquantify these effects. Modelling is very important; itis also a severe test of a model, as so many physicalprocesses are involved in the final tidal states at theMLT heights (circa 90 km).

The observational portion of the new studyfor 2000 used the six MF radars from the GW study(2°-70°N). The objectives were to document themonthly and seasonal variabilities of the 12-, 24-hrtides for radars in this North American-Pacific sector,over several years (1990-1997), and to compare withthe Global Scale Wave Models (GSWM1995,GSWM2000; Maura Hagan, NCAR, Boulder) andagain with the tides from the CMAM. It must bestressed that the differences between the GSWMversions are purely due to different assimilated-background data. If there are flaws in these new data,the tidal results of the new version may be inferior tothose of the original. The abstract follows, for thisnow submitted paper:

Figure 2. T

he 12-hr tidal profiles from the M

F radars (thin lines) and from

GS

WM

1995 (dashed lines) and the CM

AM

experiment (M

K param

eterization).

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The 16-day Wave in the Mesosphere and Lower Thermosphere: SimultaneousObservations at Saskatoon (52N, 107W) and London (43N, 81W), Canada

Y. Luo1, A. Manson1, C. Meek1, T. Thayaparan2, J. MacDougall3, W. Hocking3

1Institute of Space and Atmospheric Studies, University of Saskatchewan, Canada, 2Defence ResearchEstablishment Ottawa, Canada, 3Department of Physics and Astronomy, University of Western Ontario,Canada

Abstract

Winds from MF radar observations (60-110 km) at Saskatoon (52N, 107W) and London (43N, 81W),Canada, are processed to investigate the quasi 16-day (12-20 days) waves. The waves at both sitesbecome prominent from late autumn to early spring (October-April) when the zonal backgroundwinds are eastward. Throughout the mesosphere they have amplitudes of 5-15 m/s, with the zonalcomponent being stronger than the meridional on average. And they exist over a large range ofaltitudes, generally decreasing with height up to 105 and 95 km for Saskatoon and London, respectively.The summer wave activity, however, is weak and limited to a thin layer around the zonal zero-windline (85 km). The local periods at lower altitudes are longer than that at higher ones, and periods atthe two locations at the same time are usually not equal. Although in some situations the phases atLondon lead those at Saskatoon by tens of degrees, the general phase differences do not appear tohave a simple pattern. The lack of coherence or correlation between the two locations for the waveamplitudes, heights of occurrence, and even periods are probably due to the longitudinal and latitudinaldifferences or localized wave activity.The vertical propagation characteristics for the 16-day wave show a standing wave structure fromwhich the vertical wavelength of ~40-50 km can be derived. This could be caused by interference ofthe incident wave from the lower atmosphere with the downward reflected wave from near themesopause. When combining the zonal and meridional components, they demonstrate a quasipolarization mode of either linear or elliptical characteristic. The possible reasons for these wavecharacteristics, such as the effect of the background wind, interaction with the gravity waves, andincluding dissipation and modulation processes, are discussed.

3. Planetary Waves PW: 16-d

After the tides, the 16-d PW is the mostconsistently significant dynamical wave feature in theMLT. These waves also modify the dynamical,thermal and chemical structure of the region. Thewave intensities and phases have been obtained fromthe MF Radars for heights from 58-105 km, andcontinuously from 1980 to 1996. (Luo et al., p 2125 J.

ISAS 2000

G. R. 2000). The occurrence is strongest in winter-centred months and covers the whole height range,with intensity maxima near 60 km. However insummer, the wave is much weaker and confined to~85 km. The abstract for a study completed in 2000is now given:

We show one figure for the profiles of the semi-diurnal tide at the eight stations, with the GSWM1995and the CMAM experimental outputs also shown (Figure 2). Both models are very similar to the MF Radarresults, with the CMAM being statistically preferred.

Figure 3. (a) T

he band-pass (12-20 day) filtered 16-day waves at three altitude layers from

1994 to 1996 at Saskatoon. T

he solid and dashed oscillatingcurves represent the zonal and m

eridional components, respectively. T

he envelope-like curves indicate the statistical 95% confidence levels for the oscillating

amplitudes; (b) T

he same as (a) but for London.

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Springtime Transitions in Mesopause Airglow and Dynamics: Photometerand MF Radar observations in the Scandinavian and Canadian sectors

A.H. Manson a,*, C.E. Meek a, J. Stegman b, P.J. Espy c, R.G. Roble d, C.M. Hall e,P. Hoffmannf,Ch. Jacobi g

aInstitute of Space and Atmospheric Studies, University of Saskatchewan, 116 Science Place, Saskatoon,SK, S7N 5E2, Canada, bStockholm University, Sweden, cBritish Antarctic Survey, UK, dNCAR, Boulder,CO, USA, eAuroral Observatory, University of Tromsø, Tromsø, Norway, fLeibniz Institute, Instituteof Atmospheric Physics, 18225 Kühlungsborn, Germany, gInstitute of Meteorology, University ofLeipzig, Stephanstr. 3, D-04103 Leipzig

Abstract

Observations from 2 optical ground stations and 3 MF radars at high and mid-latitudes have beencombined to describe �springtime transitions� in atomic oxygen and the mesopause wind fields andwaves for eight years (1991-1998). The typical signature in the Stockholm (60N, 20E) OI 558nm�green-line� emission involves a rapid (circa) 2 day rise in the night-time value by factors of 2 or so,with a subsequent decrease by factors of 3 to 10. There is considerable inter-annual variability inthese green-line emissions, and also the hydroxyl airglow (intensities and temperatures) at Bear LakeObservatory (Utah, 42N, 115W), but the 6-8 year means do show a characteristic airglow �springtimetransition� (AST) near the end of March. MF radars from Tromsø (70N, 19E), Juliusruh (55N, 13E)and Saskatoon (52N, 107W) demonstrate springtime reversals in the mean (daily) zonal winds at 85-95 km, both annually and in 8 year means, at times near the airglow �transitions�. The �tongue� ofeasterlies (near March 30) is a long-established feature of mesopause dynamics, and clear indicationsof associated changes in tides and gravity wave fluxes are also presented. The TIME-GCM is alsoused to investigate the characteristics of the airglow and winds during the interval associated withthe AST events. Useful similarities with the observed variations are demonstrated.

Conclusion

Several projects are underway as this reportis being written. They include variations of the windand wave-fields with latitude (MF radars at Saskatoonand Platteville); the modulation of GW fluxes byPlanetary waves ( 2-,16-days); the 16-day PW

The PSMOS Program includes a project for the study of “Day-to-day variations in the airglowemissions in relation to global dynamical processes”. The following abstract is from an accepted paper:

ISAS 2000

4. Relations between Airglow and Dynamics

variabilities between 2 and 70N; and airglow –dynamics relationships using the SATI-imager. Weare also preparing for collaborations with colleaguesleading the Odin-OSIRIS (GW and ozone), andTIMED (winds in the MLT) satellite systems.

We show one figure for the band-pass filtered 16 d PW at Saskatoon (a) and London (b) (Figure 3)

G.J. Sofko

A. The Canadian SuperDARN FACILITY (G.J. Sofko, Principal Investigator)

The Canadian SuperDARN Radar Facility

The year 2000 marked an important increasein the number of northern hemisphere radars in theSuperDARN network. The University of Sask-atchewan engineering/technical team of MikeMcKibben, Head Engineer, and Bill Marshall,Technician, played critical roles in the construction ofthe Prince George, BC, radar, which began operationson March 1, 2001, and the Kodiak, Alaska, radar,which began operating at the end of 1999 but becamefully operational during early 2000. Funding for thePrince George radar was obtained through an NSERCMajor Installation Grant ($352 k) and Canadian Space

At the 2000 SuperDARN Workshop inBeechworth, Australia, the decision was made tochange the copy medium from Exabyte tape to CDs.In August, an “Auto Studio” CD facility was purchasedby the U of S SuperDARN team, and several monthswere taken to write scripts to automate the duplicationof the MR (Multiple Radar) data files which are

Agency (CSA) support ($60 k). Continued operationof the Prince George and Saskatoon radars is fundedthrough an NSERC Major Facilities Access (MFA)grant. The Prince George radar data transfer isaccomplished through routing to the Internet on agateway computer at the University of Northern BC,which receives the data from the radar site via an RFModem link. This RF Modem method was first triedwith the Saskatoon radar, and was so effective thatthe same technique was used for both the PrinceGeorge and the Kodiak radars.

The SuperDARN International Data Copy and Distribution Facility, U of Saskatchewan

transmitted electronically (FTP) from Johns HopkinsUniversity Applied Physics Laboratory (northernhemisphere data) and the British Antarctic Survey(southern hemisphere data), where the original dataare sent from each radar to generate the MR datafiles. The new system prints the labels onto the CDs,and was working reasonably well by the end of 2000.

The SuperDARN Scheduling Working Group - Chairmanship passes to the U ofSaskatchewan Team

At the Australia SuperDARN 2000Workshop, Dr. Dieter Andre of the U of S was electedto the role of Scheduling Working Group Chairman,in which he succeeded Dr. Catherine Senior of CETP/CNRS (St. Maur), France. Dr. Andre assumed theposition on August 1, 2000, just after the successfullaunch of the CLUSTER 4-satellite mission. Thescheduling is now done on a partial day basis, so

that during overpasses of important satellites, suchas CLUSTER, the SuperDARN operating schedulingcan be optimized for joint radar-satellite data gatheringat magnetically conjugate positions. During thesesatellite overpasses, the radars frequently operate inthe High Time Resolution Mode (1-minute scans)rather than the Normal Mode (2-minute scans).

Magnetosphere/IonosphereInteractions

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B. SuperDARN ScienceMagnetospheric Physics

During the year, there were 3 papers con-centrating on the effect of the IMF on SuperDARNconvection patterns observed, one paper for dominantBy+ conditions, and two papers for northward IMFBz+ conditions. The main results follow.

In the March 1, JGR, paper “Ionosphericconvection response to changes of interplanetarymagnetic field Bz component during strong Bycomponent” by Huang et al., a study of the convectionpattern determined by the MACCS and CANOPUSmagnetometers, supported by SuperDARNmeasurements, was performed for March 23, 1995,on which By remained strongly positive (in the period11 - 20 UT. In the period 13 - 15 UT, the Bzcomponent underwent five changes of sign but neverexceeded +6 nT or was less than - 6 nT, whereas Bywas in the range +7 to +10 nT. The results showedthat the northern hemisphere convection wasdominated by ONE large clockwise convection cellwhose “focus” was at high latitude above 80 MLAT.There were two results of the shift in Bz during thispredominantly By+ conditions. (i) The “focus” shiftsfrom prenoon during Bz+ to postnoon during Bz-, withthe shape of the overall pattern unchanged, butconvection velocities increase as Bz turns negative.(ii) When By is very strong compared to Bz, the focusremains relatively fixed when Bz changes sign butthe convection velocities increase within the pattern,whose overall shape again remains unchanged. It isto be noted that the shifting of the “focus” fromprenoon to postnoon is more dramatic than thatderived by the statistical convection patterns forderived for |Bz| < By by Friis-Christensen et al. (JGR,90, 1325, 1985) and Weimer (JGR, 100, 19,595,1995), but the overall patterns show good agreement.The delay of the initial convection pattern change afterthe IMF reached the nose magnetopause was 5 - 9minutes; the additional time for the pattern to reachfinal reconfiguration was 10 - 20 minutes.

In the April 1, 2000, JGR paper “SuperDARNobservations of ionospheric multi-cell convectionduring northward interplanetary magnetic field” byHuang et al., the SuperDARN data revealed both ofthe reverse convection cells on the dayside for strongnorthward Bz+ conditions. The cell locations wereobserved to be quite stable during their development,and the reverse convection conditions can remainfor 2-3 hours as long as the IMF conditions are stable.

In effect, these SuperDARN observations were thefirst direct in-sites observations of the “four-cellconvection” consisting of the two reverse cells andthe “normal” two cell-pattern that is usually observedduring Bz- conditions.

Finally, in the Dec. 1, 2000, JGR paper“Evolution of ionospheric multicell convection duringnorthward interplanetary magnetic field with |Bz/By|> 1”, the reverse convection cells were located whenthe ratio |Bz/By| changed from | Bz/By| > 3, to therange 2 < |Bz/By| < 3, to the range 1 < |Bz/By| < 2.The high ratio was associated with two reverse cells,the middle range with one or two cells (the prenooncell being at lower latitude and disappearing as theratio |Bz/By| became smaller) and the lowest ratiowith one one reverse clockwise cell centered on noon.

SuperDARN Gravity Wave Observations

(a) In the GRL Feb. 15, 2000, paper “SuperDARNobservations of medium-scale gravity wave pairsgenerated by Joule heating in the auroral zone” bySofko and Huang, it was shown that Joule heatingevents at high latitudes, which normally launch a singlegravity wave pulse per Joule heating interval, cansometimes launch two gravity waves per Joule heatingepisode, provided that the duration of the heatingevent at high latitude is as long as 50 minutes. Theconvection pattern seen by the SuperDARN radarsat high latitudes is closely related to the generation ofthe gravity waves, which are seen some 100-120minutes later at lower latitudes in the ground-scatterpattern of the SuperDARN radar. When the positive(southward flow, westward electric field) and negative(northward flow, eastward electric field) intervals ofconvection at high latitude are each of duration morethan 50 minutes, there are two gravity waves seenfor each half of the complete convection cycle.Usually, the convection oscillations are of shorterperiod (<30 min.) and during such oscillations, whichare associated with Joule heating bursts, there is onlya single gravity wave launched during each half ofthe convection cycle.

(b) Gravity Wave and Magnetic Pulsations of 40minutes during Bz+ IMF conditions. Huang et al.,GRL, 27, 1795, 2000). During an interval on Dec. 8,1997 (07 - 17 UT) when the IMF was quite stable andnorthward (Bz+), the solar wind showed little variation.

ISAS 2000

In the paper “Small scale vortices in the high-latitude F region” by Huber and Sofko [JGR, 2000],high spatial resolution (15 km) and temporal resolution(3 s) on adjacent beams were used to estimate thescale size and lifetime of the structures which causethe HF scattering that results in double-peaked (DP)spectra near magnetic local noon. Such spectra hadbeen originally investigated by Schiffler et al. in thepaper “Mapping the outer LLBL with SuperDARNdouble-peaked spectra”, GRL, 24, 3149, 1997, whereit was found that the particle spectra of DMSPoverflights of the SuperDARN field-of-view of theSaskatoon/Kapuskasing radar pair placed the mainoccurrence region of the spectra just equatorward ofthe cusp, namely the low-latitude boundary layer(LLBL) projection to the ionosphere, with fewerspectra in the cusp and mantle regions. The double-peaked spectra can be associated with scatteringcaused by the gradient-drift instability due to electrondensity gradients in the vicinity of narrow beams ofprecipitating particles. These narrow columns would

Ionospheric Structure Inferred from SuperDARN spectra

However, in the ionosphere, high-latitude magneto-meters showed a morning sector pulsation of periodabout 40 minutes, with amplitude only 10 nT.Subsequently, gravity waves with 40 minute periodappeared at low latitudes. It appears that themagnetosphere, which must have been very nearly

completely closed, is subject to tail oscillations of longperiod, which can be transmitted down to theionosphere. The associated ionospheric oscillationsin current and Joule heating lead to the gravity wavesseen subsequently with the same period at lowlatitudes.

have an outer core of positive charge and an innercore of negative charge due to the spreading of theions by efficient charge exchange with neutrals. Suchan effect was used to predict the intensity of Balmeremission by proton beams (G. T. Davidson, JGR, 70,1061, 1965). This radial electric field causes thevortical motion that produces the double peaks. Theradial electric field is on the average about 5 mV/mbecause the double peaks are found to have a Dopplervelocity separation of about 200 m/s. Huber et al.found from the high-resolution SuperDARN study thatthe upper limits on size and lifetime were ~26 km and4 s, respectively. The 26 km upper limit on size isvery consistent with the widths of the Balmeremissions predicted by Davidson (loc. cit.) in the F-region by proton precipitation at low energy. The 4 supper limit on lifetime is also consistent with the lowerfrequency portion of the wave activity in the 0.2 - 2.2Hz found by satellite measurements in the cusp region(Maynard et al. JGR, 96, 3502, 1991; Matsuoka etal., JGR, 98, 11,225, 1993).

In the GRL, May 15, 2000 paper by Gray,Mattar and Sofko,“Influence of Ionospheric ElectronDensity Fluctuaions on Satellite Radar Interferometry”,the presene of streaks on the C-band (5.5 Ghz)RADARAT satellite radar interferometry (SRI) datataken during remote sensing of the earth (usually icereconnissance and terrain mapping) at high latitudeswas shown to result from the phase shifts imposedby gradients in the integrated electron density alongthe two-way path of the transmissions from thesatellite down through the ionosphere to the earth,followed by the scattering from the ground target andpropagation back up through the ionosphere to thesatellite.

C. Graduate Student Projects

(a) M.Sc. work of Kari Toews using both the VHFSAPPHIRE radar system (50 MHz) and SuperDARNresults. In the fall of 2000, Ms. Toews completed herM.Sc. thesis (Spectral and Pulsation Studies Usingthe SAPPHIRE Radar Array), the principal results ofwhich were the behaviour of Ps6 pulsations studiedby radar (VHF and HF), ionosonde, magnetometer,riometer and satellites. It was shown that a sequenceof events, starting with frontside satellite IMF and solarwind data, followed by tail reconnection and substormonset with bursty bulk flows, could finally lead to thePs6 ionospheric disturbances in the ionosphere. Thetime-sequence of events gives one of the mostcoordinated and comprehensive pictures of the Ps6pulsation process to date.

all likelihood the signatures of flow bursts associatedwith reconnection at the near-earth neutral line.

D. The Effect of the High-latitude Ionosphereon Remote Sensing studies of the earth

(b) Ph.D. project of Jun Liang. Mr. Liang isstudying the latitudinally-extended but longitudinally-restricted radar structures seen near midnight duringthe substorm growth phase. These structures are in

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A.V. Koustov

Identifying the times of the strong magnetic substormonsets is a prime goal of numerous Space Weatherstudies. The most reasonable and widely usedapproach in this direction is a continuous monitoringof the Sun and the solar wind parameters andprediction of possible effects based on these (mainlyin-situ) measurements. We decided to use anotherapproach, namely an attempt has been made toidentify the preferential periods for substormoccurrence by looking at the long series of magneticindices available for more than 30 years. We considerAE and AO electrojet indices that are related tosubstorm activity, though indirectly. Since eachsubstorm corresponds to a sharp increase/decreasein AE/AO, we consider the derivatives of these indices,AEd and AOd, as measurers of substorm activity.

Large-scale luminosity undulations at theequatorial boundary of the diffuse aurora belt werefirst detected by the DMSP satellites. In this studywe consider one spectacular event of ground-basedobservations of such undulations, January 14, 1999.The event occurred in the evening sector. Thewavelengths and amplitudes of luminosityperturbations were ~ 200-900 km and ~40-400 km,respectively. We focus on the relation of undulationsto different substorm phases and to excitation of Pc5

�Giant� Undulations at the Equatorial Boundary of Diffuse Aurora and Pc5 MagneticPulsations (A.V. Koustov together with D.G. Baishev (Russia) and others)

geomagnetic pulsations. We show that theundulations began ~40 min after the substorm onsetand lasted for ~80 min, all the way to the end of thesubstorm. Concurrently with undulations, there wereobserved Pc5 magnetic pulsations of an oscillationperiod roughly equal to the ratio of the undulationwavelength to their propagation velocity. We interpretobservations in terms of the shear/ballooninginstability excitation near the plasmapause andsubsequent generation of drift hydromagnetic waves.

Magnetic Indices for Substorm Onset Determination

(L.V. Benkevitch, Ph.D. Student (Supervisor- A.V. Koustov))

Figure 1 gives an example of AEd and AOd variationswith season and universal time. To produce thisdiagram we set the thresholds to the rates of AE andAO change, 400 nT/hour and –100 nT/hour,respectively, and simply did not consider thoseperiods for which AEd and AOd were below thethresholds. In this way, we counted only strongsubstorms that are rare. We then averaged theindices over the whole period of measurements (thatis why the absolute values of shown in Figure 1 indicesare low numbers). Both AEd and AOd showenhancements at the same periods. These periodsare around equinoxes and between 10-14 UT(midnight is in the Alaskan sector). Further work isplanned on a comparison with observations on event-by-event basis and on interpretation of derivedseasonal and UT variations.

Magnetosphere/Ionosphere Interactions (contd)

ISAS 2000

Figure 1. Average AEd and AOd indices for various seasons. Areas of enhanced values correspond to preferredperiods for substorm onsets.

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Comparisons of DMSP plasma drifts and IZMEM convection model

(L. Xu, PhD Student (Supervisor - A.V. Koustov))

As an expansion of the previous study, acomparison of the IZMEM model predictions andDMSP measurements was performed. Figure 2 showsthat the model (based on a statistically inferred

relationship between magnetic perturbations on theground and variations of the solar wind parameters)performs reasonably well in terms of the convectionpredictions at specific points of DMSP measurements.

Figure 2. IZMEM electrodynamic model predicted velocity versus DMSP measured velocity for 31 satellite passesover the Saskatoon-Kapuskasing radar pair field of view.

ISAS 2000

Ionospheric Physics

A.V. Koustov

It has been suggested that HF E-region echoeshave more complex signatures on the parameterplots, such as the Watermann’s diagrams. In previousstudies by the Leicester group several unexpectedclusters of points were indeed identified. On the otherhand, no new physical mechanisms have beenproposed to explain them. In this project, we considerone short event of high-velocity E-region echoobservations by the Pykkvibaer HF radar in order toexamine the hypothesis that the observed echoes arerelated to the Farley-Buneman plasma instability. Weshow that one cluster of echoes corresponds to theclassical type 1 scatter with velocities close to thenominal ion-acoustic speed of 400 m/s while the othercluster has unusually large velocities of the order of

700 m/s. However, plotting of the echo parametersversus slant range clearly demonstrates that all ~700m/s echoes are coming from distances of 500-700km while all ~400 m/s echoes are coming from fartheraway (700-1000 km). We show that the difference invelocities for the two clusters occurs because of thedifference in the height of echoes. Such selection ofecho heights happens due to different amounts ofionospheric refraction at near and far ranges. Thusthe ionospheric refraction and related altitude variationof the ionospheric parameters are important factorsto be considered when various characteristics of E-layer decameter irregularities are derived from HFradar observations.

High-velocity E-region HF echoes

(A.V. Koustov together with M.V. Uspensky (Finland) and others)

Characteristics of E-region irregularities according to observations at Syowa station,Antarctica (R.A. Makarevitch, PhD Student (Supervisor- A.V. Koustov))

SuperDARN HF radars at Syowa (run by theNational Institute of Polar Research, Tokyo) are wellpositioned for the E-region irregularity studies in abroad range of flow angles. During 1995-1997, theSuperDARN radar observations were supplementedby 50-MHz radar measurements performed by theCommunications Research Laboratory, Tokyo. Thedata gathered are extremely useful for studies ofvarious aspects of E-region plasma physics. Severalfeatures are under investigation. One example is theflow angle distribution of echoes. Previous paper byKoustov et al., J. Geophys. Res., 106, 12,875-12,887,2001, (based on a very limited data set) has indicatedthat the dependence of 12-MHz echo power versusflow angle is much more uniform than that at 50 MHz.This effect was studied by employing other approachand by using significant data statistics. Figure 1 showsthe echo occurrence at various azimuths ofobservations (azimuth of ~1340 corresponds roughlyto the magnetic meridian direction) at 12 and 50 MHz.

At 12 MHz two separate echo regions are obvious:E-region echoes at short distances of 300-400 kmand F-region echoes at larger distances. E-regionecho region follows well the line of –10 aspect anglein a very similar fashion to 50-MHz echoes. One canclearly see that 50-MHz echoes do not occur for themagnetic meridian directions (~1340) but are quitetypical along the L-shell directions (i.e., along theelectrojet flow, ~83.70 and 183.70).

12-MHz echoes most frequently occur for thedirections ~200 closer to the magnetic meridian thanthe 50-MHz echoes. The large-distance (~700 km)F-region echoes are much rare, especially at largeazimuths corresponding to the field of view of theSyowa South radar (this radar is known for itstechnical problems). A number of other projects arecurrently under way including 12/50-MHz velocitycomparison, power-velocity relationship, and studyof types of VHF/HF coherent echoes.

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Figure 1. Echo occurrence at 12 and 50 MHz according to observations at Syowa, Antarctica, in March of 1997.Notice that the SuperDARN radars used 2 min scans while the 50-MHz radar had 4 min scans.

Figure 1. Overnight ATI striation activity showing a clear slope reversal. After Figure 3 from Haldoupis et al., 2001.

Mid-latitude Research

C. Haldoupis from the University of Crete andmyself took the lead in an investigation ofquasiperiodic (QP) coherent radar echoes observedin the mid-latitude summer E-region ionosphere. Forthis study we analysed data from the Valensole highfrequency (HF) radar located in southern France. Thisradar has a large azimuthal scanning region (86°;26°E to 58°W; 2° resolution).

The large azimuthal coverage of the Valensoleradar allows for study of QP echoes in the zonaldirection using azimuth-time-intensity (ATI) analysis.ATI plots show sequential sloping striations of scatterreminiscent of those detected routinely in the range-time-intensity (RTI) plots of mid-latitude radars, whichview the medium at a fixed azimuth about themeridian. It was found that ATI striation periods rangefrom a few minutes to less than 30 min, whereas thestriation slopes are systematically negative (motions

G.C. Hussey

My investigations of the E-region for 2000 was a balance between mid- and high-latitude studies.

westward) prior to local midnight, and turn positive(motions eastward) in the post-midnight hours. Thezonal rates, dx/dt, computed from the striation slopes,take values between ~30 and 160 m/s. These aredue to real motions of unstable plasma structures,most likely sporadic E patches that drift along withthe neutral wind, which have zonal scale lengths ofseveral tens of kilometres. The present observationsimply that the mechanism responsible for QP echoesis independent of azimuth and can basically operateeffectively in any direction in the horizontal plane.

This analysis is presented in the publication:C. Haldoupis, G.C. Hussey, A. Bourdillon, and J.Delloue, Azimuth-Time-Intensity striations ofquasiperiodic radar echoes from the midlatitude Eregion ionosphere, Geophys. Res. Lett., 28, 1933-1936, 2001. Below is presented Figure 3 from thepaper, reproduced here as Figure 1.

Ionospheric Physics (contd)

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High-latitude research

In 1999 the characteristics of electron densitygradients and their importance in E-region plasmainstability excitation was investigated using EISCATincoherent radar measurements (C. Haldoupis, K.Schlegel and G.C. Hussey, Auroral E-region electrondensity gradients measured with EISCAT, Ann.Geophys., 18, 1172 -1181, 2000). For 2000, TilmannBösinger from the University of Oulu, Finland, joinedour collaboration and an expanded statistical analysison Tromsø EISCAT CP1 data was initiated. Spec-ifically, we were searching for evidence of verticalplasma transport in the E-region. It is known that inthe F-region the physics and chemistry are highlydependent on vertical plasma transport (e.g., the F-region peak cannot be explained without taking theeffect into account). Under specific conditions in theE-region, namely low electron density and largeelectric field conditions, vertical plasma transporteffects cannot be excluded [Huuskonen et al., 1984].The now large EISCAT CP1 data set allowed for aninvestigation of this effect.

Figure 2. EISCAT CP1 occurrence distribution of altitude of electron density peak in the E-region versus the orientationof the electric field. The plot is generated from 12,609 electron density profiles from 10 years of EISCAT CP1observations.

Figure 2 is an occurrence distribution plot ofthe altitude of the electron density peak in the E-regionversus the direction of the ambient electric field. It isclearly seen that for eastjet conditions (E-field azimuth~0°) the average electron peak altitude is higher thanfor westjet conditions (E-field azimuth ~180°). Thisis expected as there is softer electron precipitationassociated with eastjet conditions than with westjetconditions. The direction of the electric fielddetermines the direction of vertical plasma transport.A northward (southward) electric field moves theelectron density upwards (downwards) comple-menting the altitude differences created by particleprecipitation. Analysis is still continuing, but it appearsthat the influence of vertical plasma effect is extremelysmall or absent. A paper on this research will besubmitted shortly.Reference - Huuskonen, A., T. Nygén, and L. Jalonen,The effect of electric field-induced vertical convectionon the precipitation E-layer, J. Atmos. Terr. Phys.,46, 927-935, 1984.

ISAS 2000

Aeronomy Research

E.J. Llewellyn, D.A. Degenstein

Graduate Students:

Research Associates:Adjunct Professor: Dr. R.L. Gattinger

Dr. N.D. Lloyd Dr. I. Khabibrakhmanov

E. IvanovM.M. (White) Hunt

B. Wilcox

Post-Doctoral Fellow: Dr. S. Petelina

Team Membersof the InfraRed Group (IRG)

Odin Project funded through PWGSC/CSA ContractsOdin projectOdin project (until July, 2000)Odin projectuntil May, 2000until August, 2000from September, 2000

This report describes the research progress that has been made by the InfraRed Group (IRG) of theInstitute during the last year.

Summer Students: A. BourassaT. RoschukT. Lengyel

The major focus of the group has continued tobe the Odin/OSIRIS instrument, in particular during2000 the first OSIRIS Comprehensive ElectricalPerformance Test (CEPT) and the complete Odinsatellite environmental test were made. OSIRIS wasoriginally shipped to Sweden in May 1998 and hasawaited the completion of the radiometer before beingmounted on to the spacecraft.

Finally in March 2000 the payload wassufficiently advanced, and complete, that it waspossible to undertake an OSIRIS CEPT at Linköping,Sweden. This procedure worked well, although some

problems were uncovered and rapidly corrected. Thetest period was also used to make a number ofadditional tests with spectral lamps supplied by Dr.Jacek Stegman of MISU, Stockholm University. Anexample of these lamp spectra is shown in Figure 1.The absence of lines at short wavelengths, <500 nm,is due to the kapton cover that is over the OSIRISentrance aperture to protect against dustcontamination. The absence of a short wavelengthresponse is also a clear indication that the spectralcross-talk of the spectrometer is unchanged fromwhen it was first delivered to Sweden.

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Figure 1. The OSIRIS neon lamp spectrum with the kapton cover in place.

These observations also showed that thewavelength calibration (pixel-to-wavelength map) atroom temperature is unchanged from that derivedfrom the Calgary calibration in January 1998.Following the Calgary calibration period the instrumentwas moved to Ottawa where the final thermal-vacuumtesting was made before delivery to Sweden. Thesetests indicated at low temperatures, <10 C, thewavelength calibration and the spectral resolutionwere significantly reduced from the room temperaturevalues. An example of this is shown in Figure 2 andit is readily apparent that there is a need for the opticalbench to be maintained at a temperature near 15 C.Thus during the thermal-vacuum (solar simulation)

tests for the entire Odin satellite the group tookparticular notice of the OSIRIS optical benchtemperature; it was subsequently decided to includea small heater under OSIRIS. These Odin thermal-vacuum tests were made at the CNES facility inToulouse, France, during June and July, 2000,following the preliminary vibration tests. An exampleof the thermal response of the OSIRIS instrumentduring part of the solar-simulation testing is shown inFigure 3. It is readily apparent that OSIRIS doesrespond to the day-night parts of the orbit, althoughthis orbit variation is not expected to impact on thequallity of the observations.

ISAS 2000

Figure 3. The measured thermal response of OSIRIS during the solar simulation tests in France.

Figure 2. The measured temperature response of the OSIRIS wavelength stability and resolution.

UV IS W aveleng th S tab ility vs O ptics B ench T em perature

791.0

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-3 0 .0 -1 5 .0 0 .0 1 5 .0 3 0 .0 4 5 .0O p tic s B e n c h T e m p e ra tu re (C )

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As we have mentioned in previous reports thecalibration and characterization of the infrareddetectors on OSIRIS is major undertaking as theozone profile determination relies on a knowledge ofthe absolute response of these detectors. During thelast year we have been able to advance ourunderstanding of the performance of these detectorsto the extent that the noise level associated with eachpixel is ~5 dn at all temperatures. This has been madepossible from an extensive analysis of the dark currentdata obtained during the cool down phase in theFrench thermal-vacuum tests. Another aspect of theFrench tests was to align the OSIRIS optical axis withthat of the Odin radiometer. We used the large CNEScollimator and an optical quality cover over the

OSIRIS entrance aperture to measure the position ofthe optical axis and the instrument field-of-view. Asthese tests were made at room temperature weneeded the real time data corrections that we havedeveloped for OSIRIS. Much of this capability owesto the efforts of Mr. Adam Bourassa, a summerstudent, who assisted Dr. Degenstein with thedevelopment of the required S/W. The systemperformed flawlessly and advanced the S/N ratio from~3 to >200 so allowing the optical axis to be clearlyidentified. As a final check on this work we madesome measurements without the protective opticalcover and were able to correct for the slight non-parallelism (2 arc minutes) of the cover. The testresults are illustrated in Figure 4.

Figure 4. The measured location of the OSIRIS optical axis, the SMR is aligned with Row 16.

ISAS 2000

The CNES beam alignment tests were also used tomake additional measurements of ozone and NO2 gascell absorption using both a laboratory continuumsource and the actual sky light. This latter is extremely

Figure 5. The measured ozone absorption spectrum for the ozone cell divided by the unabsorbed sky spectrumobtained a few minutes earlier. The magnified part of the spectrum shows the wavelength structure due to the ozoneabsorption feature.

The quartz-halogen lamp spectra also indicatedthe presence of obvious structure in the full slit images,see Figure 6, and this initiated a search for the causeof the problem. As part of this investigation it wasdecided to re-examine full slit spectra that had beentaken at Calgary in January 1998 and those from theCEPT earlier in the year. The re-analysis showed

important as the wavelength structure in the solarspectrum must be properly accounted for in the DOASanalysis. An example of the collected sky spectrawith an ozone absorption cell is shown in Figure 5.

that very small amounts of structure were present inthe Calgary images and that the CEPT imagesdisplayed exactly the same problem as thoseevidenced in the Toulouse observations. The slitimage structure was confirmed through the collectionof full slit images during the second CEPT that washeld in Sweden at the end of the year.

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It was concluded that the slit must havedeveloped some structure during the time sinceOSIRIS was manufactured and that a scheme shouldbe developed to examine the slit. The requiredprocedure, which used a small astronomicaltelescope, was evaluated with a series of tests of theDM version of OSIRIS in Ottawa. At the end of theyear it was announced that Odin would be launchedin February 2001 from Svobodny so that the effortsof the IRG are about to come to fruition.

Dr. Petelina has joined the Odin effort andwill concentrate on the detection of aerosols withOSIRIS. The approach here is to use the IRItomographic procedure to identify regions ofenhanced Rayleigh scattering and then to analyzethe optical spectrograph data in order to determinethe properties of the scatterers. This work representsan extension of some of her previous work in Swedenand the former Soviet Union.

Figure 6. The full slit image showing the striations in the observed spectra.

Other aspects of the research work undertaken bythe group have continued to involve the developmentof data analysis and presentation software. This workhas been led by Dr. Gattinger who was supportedwith the efforts of the summer students Mr. T. Roschukand Mr. T. Lengyel. Dr. Gattinger has also undertakena major role in the evaluation of the overall OSIRISperformance. In this latter context Dr. Gattinger wasparamount in the effort that developed the slitcharacterization and inspection procedure.

Mr. Eugene Ivanov completed his analysisof the InfraRed Imager scattered light performanceusing a software model of the imager. This work,which formed the basis of his graduate thesis, showedthat the measured performance is equal to thatexpected and that the imager is in fact operating atthe diffraction limit. Mr. Ivanov left the group inSeptember 2000 to take up a position as a designengineer with ADA here in Saskatoon.

ISAS 2000

Ms. Megan Hunt completed her thesis workon the Ring effect and showed that while the effect isindeed important for satellite observations of the Odin/OSIRIS type it is not important for ground-basedindustrial remote sensing. Ms. Hunt is presentlyworking for Kipp-Zonen, formerly SciTec, here inSaskatoon.

Mr. Brad Wilcox joined the group inSeptember and is initiating a ground-based OSIRISvalidation program using the DM version of OSIRIS.This work is presently in its infancy but it is importantif we are to confirm the on-orbit performance ofOSIRIS as early as possible in the mission.

Probably one of the most important peoplefor the Odin/OSIRIS mission is Dr. Nick Lloyd, he hasresponsibility for the flight software and flightoperations. The checkout procedures and the displaysoftware that he has developed enables the team todetermine quickly, and reliably, the overall status ofthe OSIRIS instrument and to report its operationalmode. The quality of this effort is demonstrated bythe fact that while OSIRIS is quite complicated only alimited number of commands must be up-linked inorder to change its complete operational mode.Indeed the external simplicity of the OSIRIS controlhas been lauded by the Swedish Space Corporationpersonnel who are responsible for overall Odinmission.

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Publications

Graduate Student Theses

Presentations (Talks, Papers, Posters)

Visitors to ISAS

Attendance at Meetings or Other Visits

Services and Distinctions

Vision Statement

Appendices

ISAS 2000

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Publications

Gray, L.A., Mattar, K.,E., and G.J. Sofko, Influence of Ionospheric Electron Density Fluctuations on SatelliteRadar Interferometry, Geophys. Res. Lett., 27, 1451-1454.

Haldoupis, C., K. Schlegel, and G.C. Hussey. Auroral E-region electron density gradients measured withEISCAT, Annales Geophysicae, 18, 1172-1181.

Haldoupis, C., A. Bourdillon, K. Schlegel, J. Delloue, and G.C. Hussey. Radio backscatter studies in SouthEurope of the midlatitude E-region ionosphere, Radio Science Bulletin, 295, 6-14.

Huang, C.-S., G.J. Sofko, A.V. Koustov, J.W. MacDougall, R.A. Greenwald, J.M Ruohoniemi, J.C. Foster,J.P. Villian, M. Lester, J. Watermann, V. Papitashvili, and W.J. Hughes, Long-period magnetospheric-ionospheric perturbations during northward interplanetary magnetic field. Accepted by J. Geophys.Res., Oct. 16, 2000. In press.

Huang, C.-S., G.J. Sofko, A.V. Koustov, D.A. Andre, J.M Ruohoniemi, R.A. Greenwald and M.R. Hairston,Evolution of ionospheric multicell convection during northward interplanetary magnetic field with B

Z

/ BY > 1, J. Geophys. Res.105, 27095-27107.

Huber, M. and G.J. Sofko, Small scale vortices in the high-latitude F region, J. Geophys. Res., 105, 20,855-20,897.

Hussey, G.C., C.E. Meek, D. Andre, A. H. Manson, G.J. Sofko and C.M. Hall, A comparison of NorthernHemisphere winds using SuperDARN meteor trail and MF radar wind measurements, J. Geophys.Res., 105, 18,053-18,066.

Huang, C.-S., D. Murr, G.J. Sofko, W.J. Hughes, and T. Moretto, Ionospheric convection response to changesof interplanetary magnetic field Bz component during strong By component, J. Geophys. Res., 105,5231-5243.

Lieberman, R.S., A.K. Smith, S.J. Franke, R.A. Vincent, J.R. Isler, A.H. Manson, C.E. Meek, G.J. Fraser, A.Fahrutdinova, T. Thayaparan, W. Hocking, J. MacDougall, T. Nakamura, and T. Tsuda. Comparisonof mesospheric and lower thermospheric residual wind with High Resolution Doppler Imager, mediumfrequency, and meteor radar winds. Journal of Geophysical Research, 105, 27,023-27,035.

Lou, Y., A.H. Manson, and C.E. Meek et al. The quasi 16-day oscillations in the mesosphere and lowerthermosphere at Saskatoon (52°N, 107°W), 1980-1996. Journal of Geophysical Research, 105,No. D2, 2125-2138.

MacDougall, J.W., D.A. Andre, G.J. Sofko, C.-S. Huang and A.V. Kustov, Travelling ionospheric disturbanceproperties deduced from Super Dual Auroral Radar measurements, Annales Geophysicae, 18, 12,1550-1559.

Sofko, G.J. and C.-S. Huang, SuperDARN observations of medium-scale gravity wave pairs generated byJoule heating in the auroral zone. Geophys. Res. Lett., 27, 485-488.

ISAS 2000

Burgdorf, M.J., Th. Encrenaz, E. Lellouch, H. Feuchtgruber, G.R. Davis, B.M. Swinyard, Th. de Graauw,P.W. Morris, S.D. Sidher and T. Lim, ISO observations of Mars: an estimate of the water vaporvertical distribution and the surface emissivity. Icarus 145, 79—93.

Clark, T.A., D.A. Naylor and G.R. Davis, Detection of the HI n=22—21 Rydberg line in emission at the solarsubmillimetre limb. Astron. Astrophys. 361, L60—L62.

Clark, T.A., D.A. Naylor and G.R. Davis, Detection and limb brightening of the HI n=20—19 Rydberg line inthe submillimetre spectrum of the Sun. Astron. Astrophys. 357, 757—762.

Hamza, A.M., M. Huber, W. Lyatsky, A.V. Koustov, D. Andre and G. Sofko. Eastward convection jet at thepoleward boundary of nightside auroral oval, Geophys. Res. Lett., 27, 2809-2812.

Huang, C.-S., D. Andre, G.J. Sofko, and A.V. Koustov. SuperDARN observations of Ionospheric Multi-CellConvection During Northward Interplanetary Magnetic Field. J. Geophys. Res., 105, 7419-7428.

Huang, C-S., G. J. Sofko, A. V. Koustov, J. W. MacDougall, D. A. Andre, W. J. Hughes, and V.O. Papitashvili.Quasi-periodic disturbance with a period of 40 minutes at high latitudes. Geophys. Res. Lett., 27,1795-1798.

Hussey, G.C., C.E. Meek, D. Andre, A.H. Manson, G.J. Sofko and C. Hall, A comparison of NorthernHemisphere winds using SuperDARN meteor trial and MF radar wind measurements. Journal ofGeophysical Research, 105, No. D14, 18,053-18,066.

Koustov, A.V. W. B. Lyatsky, G. J. Sofko, and L. Xu. Field-Aligned Currents in the Polar Cap at Small IMFBz and By Inferred From SuperDARN Radar Observations. J. Geophys. Res., 105, 205- 214.

McDade, I.C., K. Strong, C.S. Haley, J. Stegman, D.P. Murtagh, and E.J. Llewellyn, A Method for RecoveringStratospheric Minor Species Densities from the Odin OSIRIS Scattered Sunlight Measurements,Can. J. Phys., accepted for publication in Odin special issue, June 2000.

McLinden, C.A., J.C. McConnell, K. Strong, I.C. McDade, R.L. Gattinger, R. King, B.H. Solheim, W.F.J.Evans, D.A. Degenstein and E.J. Llewellyn, The impact of the OSIRIS grating efficiency on radianceand trace-gas retrievals, Can. J. Phys., accepted for publication in Odin special issue, June 2000.

Morris, P.W., Th. de Graauw, E. Lellouch, B.G. Henderson, S. Erard, Th. Encrenaz, H. Feuchtgruber, M.J.Burgdorf and G.R. Davis, A detailed assessment of carbonates in thermal infrared spectroscopy ofMars with the ISO Short Wavelength Spectrometer. Icarus, submitted..

Naylor, D.A., B.G. Gom, G.R. Davis, T.A. Clark and M.J. Griffin, Atmospheric transmission at submillimetrewavelengths from Mauna Kea. Mon. Not. R. Astr. Soc. 315, 622—628.

Sidher,S.D., M.J.Griffin, G.R. Davis, B.M. Swinyard, M.J. Burgdorf, G.S. Orton, D.J. Rudy, Th. Encrenaz, E.Lellouch and Th. de Graauw, ISO LWS observations of Mars—detection of rotational modulation inthe far infrared. Icarus 147, 35—41.

Sioris, C.E., W.F.J. Evans, R.L. Gattinger, I.C. McDade, D.A. Degenstein and E.J. Llewellyn, Ring effectmeasurements from ground-based viewing geometry with the OSIRIS DM, Can. J. Phys., submittedfor publication in Odin special issue, Accepted June 2000.

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Graduate Student Theses

D. Degenstein, Ph.D. Student – Thesis: Atmospheric Volume Emission Tomography from a Satellite Platform.Graduated October 1999 (winner of University Thesis award, nominee for NSERC Doctoral Prize).

J.J. Offiong, M.Sc. Student - Thesis: The Feasibility of using the ALIVE Hyperspectral Instrument to ExtractGeophysical Information from the Atmosphere. Graduated October 1999.

A.S. Sassi, M.Sc. Student (Division of Environmental Engineering) - Thesis: The Effect of some MeteorologicalFactors on Ozone Variations in the Northern Hemisphere. Graduated October 1999.

M. Hunt (nee White), M.Sc. Student - Thesis: The Ring Effect and Systematic Errors in Quantitative Absorp-tion Spectroscopy. Graduated August 2000.

E. Ivanov, M.Sc. Student - Thesis: The Computer Modelling of the OSIRIS IR Imager.Graduated September 2000.

K. Toews, M.Sc. Student - Thesis: Spectral and Pulsation Studies using the SAPPHIRE Radar Array.Graduated August 2000.

ISAS 2000

Presentations(Talks, Papers, Posters)

Baishev, D.G., E.S. Barkova, S.I. Solovyev, K. Yumoto, M.J. Engebretson, and A.V. Koustov, Formation ofLarge-Scale, «Giant» Undulations at the Equatorial Boundary of Diffuse Aurora and Pc5 MagneticPulsations During the January 14, 1999 Magnetic Storm. Proc. of Fifth Intern.Conf. on Substorm. St.Petersburg, Russia. Netherlands, Noordwijk: ESA, 427-430. May 16-20, 2000.

Benkevitch, L.V., W.B. Lyatsky, A.V. Koustov, A. Hamza, and G.J. Sofko, Two new indices for studies ofseasonal and diurnal variations in the substorm activity. Eos Transactions, American GeophysicalUnion, Vol. 81, No. 48, p. F1008, in San Franciso, December 15-19, 2000.

Burgdorf, M.J., Th. Encrenaz, J.R. Brucato, E. Lellouch, H. Feuchtgruber, G.R. Davis, B.M. Swinyard, T.G.Müller, S.D. Sidher, P.W. Morris, M.J. Griffin, L. Colangeli, and V. Mennella, The emissivity of Marsand Callisto in the far infrared. Proc. ISO Beyond the Peaks: The Second ISO Workshop on AnalyticalSpectroscopy (ESA SP-456), Villafranca del Castillo, Spain, February 9—12, 2000.

Burgdorf, M.J., Th. Encrenaz, H. Feuchtgruber, G.R. Davis, Th. Fouchet, D. Gautier, E. Lellouch, G.S. Orton,and S.D. Sidher, ISO far-infrared spectroscopic observations of Jupiter. Proc. The Promise of FIRST,Toledo, December 2000, in press.

Davis, G.R., T.R. Fulton, S.D. Sidher, M.J. Griffin, B.M. Swinyard, P.G.J. Irwin, G.S. Orton, M.J. Burgdorf,D.A. Naylor, Th. Encrenaz, and E. Lellouch, LWS measurements of HD in the giant planets. Proc.ISO Beyond the Peaks: the Second ISO Workshop on Analytical Spectroscopy (ESA SP-456),Villafranca del Castillo, Spain, February, 29—31, 2000.

Davis, G.R., T.R. Fulton, and D.A. Naylor, The D/H ratio in giant planet atmospheres. Annual Meeting of theCanadian Astronomical Society, Vancouver, May 2000.

Davis, G.R. and D.A. Naylor, SPIRE: The Spectral and Photometric Imaging Receiver. Annual Meeting of theCanadian Astronomical Society, Vancouver, May 2000.

Davis, G.R., SPIRE: The Spectral and Photometric Imaging Receiver. Canadian Astronomical Society GraduateStudent Workshop, Vancouver, May 2000.

Drummond, J.R. and MOPITT Science Team, Measurements Of Pollution In The Troposphere (MOPITT)global measurements of tropospheric composition. Canadian Meteorological and OceanographicSociety 34th Congress, Victoria, May 2000.

Drummond, J.R., G.S. Mand, G.P. Brasseur, J.C. Gille, J. Wang, G.R. Davis, J.C. McConnell, G.D. Peskett,H.G. Reichle, and N. Roulet, First results from the Measurements Of Pollution In The Troposphere(MOPITT) instrument: carbon monoxide and methane measurements. 33rd COSPAR ScientificAssembly, Warsaw, July 2000.

Huang, C.-S., G. Sofko, A.V. Koustov, D. Andre, J.M. Ruohonimei, R.A. Greenwald and M.R. Hairston, Theevolution of multi-cell convection during northward IMF with Bz/By >1, Abstracts of SuperDARN2000 Annual Meeting, p.20. Beechworth, Australia, May 22-26, 2000.

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Huang, C.-S., G. Sofko, A. Koustov, J. MacDougall, D. Andre, W.J. Highes, and V.O. Papitashvili, Long-period activity in the morning sector during northward IMF, Abstracts of SuperDARN 2000 AnnualMeeting, p.78. Beechworth, Australia, May 22-26, 2000.

Huang, C.-S., G. Sofko, A. Koustov, J. MacDougall, R. Greenwald, M. Ruohoniemi, J. Vilain, M. Lester, J.Watermann, V. Papitashvili, and W. Huges, Long-Period Magnetospheric-Ionospheric PerturbationsDuring Prolonged Northward Interplanetary Magnetic Field. Eos Transactions. American GeophysicalUnion, Vol. 81, No. 48, p. F1054, in San Franciso, December 15-19, 2000.

Huang, C.-S., G. Sofko, (presenter), A. Koustov, D. Andre, J.M. Ruohoniemi, R.A. Greenwald and M.R.Hairston, The Evolution of Multi-Cell Convection During Northward IMF with |Bz/By| > 1.

Huang, C.-S., G. Sofko, (presenter), A. Koustov, J. MacDougall, D. Andre, W.J. Hughes and V.O Papitashvili,Long-Period Oscillation Activity in the Morning Sector During Northward IMF.

Hussey, G.C., “Ground Based Ionospheric Radar Observations” Saskatoon, March 9, 2000.

Hussey, G.C., Future directions in ground-based Space Environment monitoring: Polar- and Auroral-ionosphere monitoring with VHF radars. Canadian Space Environment Program Workshop, Banff,AB, October 11-14, 2000.

Koustov, A.V., K. Igarashi, D. Andre, K. Ohtaka, N. Sato, H. Yamagishi, and A. Yukimatsu, Flow and aspectangle characteristics of 12-MHz and 50-MHz auroral coherent echoes according to observations atSyowa station. Japan-USA workshop “Alaska Project”, Tokyo, March 7-8, 2000.

Koustov, A.V. and D. Andre, K. Igarashi, and K. Ohtaka, N. Sato, H. Yamagishi, and A. Yukimatsu, On thephase velocity of 3-m and 12-m electrojet irregularities, DASP Annual Meeting, Toronto, February16-18, 2000.

Koustov, A.V., K. Igarashi, D. Andre, K. Ohtaka, N. Sato, H. Yamagishi, and A. Yukimatsu, Flow and aspectangle characteristics of 12-MHz and 50-MHz coherent echoes, Abstracts of SuperDARN 2000 AnnualMeeting, p.33. Beechworth, Australia, May 22-26, 2000.

Koustov, A.V., R.A. Makarevitch, D. Andre, K. Igarashi, K. Ohtaka, T. Ogawa, N. Sato, H. Yamagishi, and S.Yukimatu. Nearly Simultaneous Radar Observations of 3-m and 12-m Irregularities in the Auroral E-Region. Eos Transactions, American Geophysical Union, Vol. 81, No. 48, p. F1011, November 28,2000.

Koustov, A.V., and G.J. Sofko, Research with SuperDARN HF radars in Canada, Japan-USA workshop“Alaska Project”, Tokyo, May 2000.

Nishitani, N. (presenter), T. Ogawa, N. Sato, H. Yamagishi, J.-P. Villain and G. Sofko, A Study of the AfternoonConvection Cell’s Response to an IMF Southward Turning.

Orton, G.S., M.J. Burgdorf, G.R. Davis, S.D. Sidher, M.J. Griffin, B.M. Swinyard and H. Feuchtgruber,Photometric observations of Neptune by the SO Long Wavelength Spectrometer: the He/H

2 ratio

and the effective temperature. The 32nd annual meeting of the American Astronomical Society Divisionof Planetary Sciences, Pasadena, October, 2000. Bull. Am. Astro. Soc.,32, 1011, 2000.

ISAS 2000

Llewellyn, E.J., R.L. Gattinger, D.A. Degenstein, W.J. Evans, I.C. McDade and R. Guzzi, OSIRIS - Polarization,Limb, Albedo and Nadir observations for the Environment and Trace gas determination [OSIRIS -PLANET]. A proposal to CSA in response to the Concept Study AO, February, 2000.

Llewellyn, E.J., Quarterly Progress Report Contract 27SR.9F007-8-1044 Provision of Aeronomy OperationsSupport for the CSA’s OSIRIS/Odin Project, March 2000.

Llewellyn, E.J., Quarterly Progress Report Contract 9F007-4-6503-SR (SSC File No. 9F007-6-JRSC/001/SR) Provision of Scientific Support for the CSA’s OSIRIS/Odin Project, March 2000.

Llewellyn, E.J., Quarterly Progress Report Contract 27SR.9F007-8-1044 Provision of Aeronomy OperationsSupport for the CSA’s OSIRIS/Odin Project, June 2000.

Llewellyn, E.J., Quarterly Progress Report Contract 9F007-4-6503-SR (SSC File No. 9F007-6-JRSC/001/SR) Provision of Scientific Support for the CSA’s OSIRIS/Odin Project, June 2000.

Llewellyn, E.J., D.A. Degenstein, R.L Gattinger and N.D. Lloyd, The determination of the atomic hydrogenprofile in the MLT region from the OSIRIS observations on the Odin satellite - a value added product.27th European Meeting on Atmospheric Studies by Optical Methods, Stockholm, Sweden, 2000.

Llewellyn, E.J., R.L. Gattinger, W.M. Payne, D.A. Degenstein, I.C. McDade, R. Guzzi and N.D. Lloyd, A newversion of OSIRIS for atmospheric remote sensing. 27th European Meeting on Atmospheric Studiesby Optical Methods, Stockholm, Sweden, 2000.

Manson, A.H., Seasonal variations of solar tides, planetary and gravity waves in the MLT: mult-year MFradar observations from 2-70 N and modeling comparisons, S-RAMP, Sapporo, October, 2000.

Petelina, S.V., E.J. Llewellyn, and D.A. Degenstein, The Determination of Polar Mesospheric CloudsCharacteristics from the OSIRIS Observations on Odin, Paper SA11A-03, AGU Fall Meeting, SanFrancisco, CA, 2000.

Prikryl , P. (presenter), J.W. McDougall, J.M. Ruohoniemi, G.J. Sofko, and T.K. Yeoman. The geoeffectivenessof solar wind Alfvén waves. S4 - Interplanetary Disturbances, First S-RAMP Conference, Sapporo,Japan, October 2-6, 2000.

Sofko, G., D. Andre and A. Koustov, The PolarDARN concept. Abstracts of SuperDARN 2000 Annual Meeting,p.11. Beechworth, Australia, May 22-26, 2000.

Sofko, G., The Status and Future of the Canadian SuperDARN program. Space Environment Workshop inBanff, AB, October 15-17, 2000.

Sofko, G. (presenter), D. Andre and A. Koustov, The PolarDARN Concept, 2000 International SuperDARNWorkshop in Beechworth, Australia, May 22-26, 2000.

Uspensky, M.V., A.V. Koustov, P. Eglitis, A. Huuskonen, T. Pulkinen, and S. Milan, A refraction scan of thenearly homogenous auroral E-region filled with field-aligned irregularities, European GeophysicalSociety Meeting, Nice, April 25-29, 2000.

Xu, L., A.V. Koustov, V.O. Papitashvili, and F.J. Rich, Ionospheric convection inferred from SuperDARN,LiMIE, and DMSP observations, Abstracts of SuperDARN 2000 Annual Meeting, p.17. Beechworth,Australia, May 22-26, 2000.

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Dr. Leroy Cogger Visiting Space Environment Goup of CANOPUS February 11Dr. W.B. Lyatsky University of New Brunswick April 23 to May 7Dr. Christos Haldoupis University of Crete, Iraklion, Greece June 25 to July 22Dr. David Naylor University of Lethbridge July 26 to 30Dr. Glenn Orton Jet Propulsion Laboratory, Pasadena, USA July 30 to August 3Dr. Martin Burgdorf European Space Agency, Madrid, Spain July 30 to August 6Dr. Sunil Sidher Rutherford Appleton Laboratory, Qxon, UK July 30 to August 6Dr. Wayne Evans Trent University, Ontario September 22Dr. J.-P. St. Maurice University of Western Ontario October 10

Visitors to ISAS

ISAS 2000

Attendance at Meetings

G.R. Davis Ottawa, ON, SPIRE meeting at the CSA February 7E.J. Llewellyn Fairbanks, Alaska February 5 to 10G.J. Sofko and A.V. Koustov University of Toronto, DASP Conference February 16 to 20E.J. Llewellyn Ottawa, Odin/ORISIS Meeting February 21 to 26A.V. Koustov and C. Meek Tokyo Japan, USA Workshop “Alaska Project” March 7 to 8C-S Huang Florida, AGU Chapman Conference March 15 to 26G.R. Davis University of Lethbridge March 23 to 27E.J. Llewellyn Stockholm & Linkoping, ORISIS April 8 to 16G.R. Davis University of Lethbridge, research visit April 28 to May 2G.J. Sofko and A.V. Koustov Beechworth, Australia, SuperDARN Annual Meeting May 22 to 26A.H. Manson Ottawa, CSA STRAC-SAEAC Meeting May 11 to 14A.H. Manson Toronto, PSMOS SCOSTEP Conference May 22 to 26G.R. Davis University of British Columbia, Annual Meeting

of the Canadian Astronomical Society May 24 to June 1E.J. Llewellyn, D.A. Degenstein, N. Lloyd and S. Petelina York University, ORISIS Science Team Meeting June 7 to 11E.J. Llewellyn Stockholm Sweden, Odin Workshop June 11 to July 11

Bologna Italy, New Project on Remote Sensing June 11 to July 11D.A. Degenstein Toulose France, Odin Solar SIM June 26 to July 8G.R. Davis and J.K. Taylor Saclay, France, SPIRE Preliminary Design Review,

CEA Service d’Astrophysique June 24 to 28G.R. Davis and J.K. Taylor Oxon, UK, SPIRE project meetings at Rutherford

Appleton Laboratory, Mullard Space Science Laboratoryand Queen Mary and Westfield College June 29 to July 7

E.J. Llewellyn Odin Aeron Annual Team meeting re: optical methods August 19 to 25D.A. Degenstein France September 5 to 13E.J. Llewellyn Sweden & France September 4 to 17G.R. Davis Oxon, UK, research visit to Rutherford Appleton Lab. Sept. 28 to Oct. 15A.H. Manson Tokyo, Japan, S-RAMP Conference Sept. 30 to Oct. 7E.J. Llewellyn and N. Lloyd Sweden, Odin/OSIRIS October 6 to 13G.C. Hussey, A.V. Koustov andG. Sofko Banff, Solar-Terrestrial Environment Workshop October 11 to 14E.J. Llewellyn Ottawa, OSIRIS November 9 to 14D.A. Degenstein Toronto, Odin November 9 to 17E.J. Llewellyn Sweden, Odin November 17 to 24E.J. Llewellyn Ottawa December 4 to 6G.R. Davis and B.E. Hesman Hawaii, Observing run on the James Clerk Maxwell Telescope

December 6 to 21A.V. Koustov San Francisco, American Geoph. Union Fall Meeting December 14 to 19

or Other Visits

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G.R. Davis- Co-investigator, ISO Long Wavelength Spectrometerproject; Leader, LWS Solar System Team- Co-investigator, Herschel Spectrometric andPhotometric Imaging Receiver project-Member of FIRST/Planck Steering Committee- PI, Measurements of the Unresolved Spectrum ofthe Earth Concept Study

G.C. Hussey-Member of CANOPUS Team

A.V. Koustov-Member of CANOPUS Team-Member of SuperDARN Team-DASP Chair

D.A. Degenstein- Participant, Optical Aeronomy and AtmosphericScience experiment (OSIRIS) on the Swedish Odinsatellite

Services and Distinctions

A.H. Manson- Member of Steering Committee for Post-STEPInternational Programs; S-RAMP (STEP-Results,Applications, and Modelling Phase) (1997-2002)- Chair of COSPAR Sub-Commission C2, MiddleAtmosphere and Lower Ionosphere (1994-1998,1998-2002)- Member of STRAC (Solar Terrestrial RelationsAdvisory Committee) of the Canadian Space Agency(1992-2001 [Chair; 1994/95] )- Member of LTCS (Lower Thermosphere CouplingStudy), international project of CEDAR-Editorial Advisory Board member, “Journal ofAtmospheric and Solar-Terrestrial Physics” (1994-present)-Chair, Institute of Space and Atmospheric Studies,University of Saskatchewan (1991-1997; 1997-2000)

G.J. Sofko- The National Aeronautics and Space Administration(NASA) Group Achievement Award for ground basedinvestigation by Team/SuperDARN, “in recognition ofthe highly successful exploration of geospace by theGlobal Geospace Science Program”- Member of CANOPUS Team- Member of SuperDARN Executive Committee- Principal Investigator, DSS/CSA contract for SystemManagement at the Saskatoon CANOPUS node- Principal Investigator, NSERC CSP “The Canadiancomponent of SuperDARN, Phase II”

E.J. Llewellyn- Principal Investigator, Optical Aeronomy andAtmospheric Science experiment (OSIRIS) on theSwedish Odin satellite- Principal Investigator, satellite experiment: OGLOWII on STS-52 Mission- Co-investigator, satellite experiments: OGLOW(STS-17/41G); PHOTONS (STS-19); WINDII (UARS);ACE (Canadian SciSat); AEPI (EOM-1/1) renamedATLAS; WAMDII; VIKING-UV Imager- Co-investigator, rocket experiment: GEMINI- Chairman, Time Allocation Committee for WINDII/UARS- Member of CAP/NSERC Committee for Review ofPhysics in Canada

ISAS 2000

the Atmospheric and Geospace Environments of the Planet Earth: the Dynamicsand Chemistry of the Middle Atmosphere and Troposphere; the Magnetosphere,Thermosphere and Ionosphere with the imbedded Aurora Borealis. Expand thesestudies to the other Planets where possible and relevant.

a comprehensive suite of observational systems including ground-based, rocketand satellite; and support the development of comprehensive Space andAtmospheric Models consistent with observations. Strive to achieve levels ofexcellence in research consistent with the highest international standards in SolarTerrestrial Physics.

the investigations and observations to important societal issues such as theUnderstanding of Atmospheric Processes and Global Climate Change, andGeospace Weather Prediction.

balanced and complementary links with Agencies and Councils involved inAtmospheric and Space Research – CSA, AES, NSERC – and with high-technology industries, especially those in Saskatchewan.

a balanced working and educational ENVIRONMENT for graduate students,scientists and engineers, including involvement with local industries, and withthe wider life of the University of Saskatchewan – teaching and outreach.

collaborations within the Institute to maximize opportunities for comprehensive,complementary studies of the Atmosphere and Geospace.

to the community of Solar Terrestrial Physicists, and to the international communityengaged in Solar Terrestrial Physics.

the Saskatoon and Saskatchewan communities, including especially studentsand the media, with information and opportunities to share in the Solar TerrestrialPhysics activity in the Institute; recognizing that these contribute to the economichealth, quality of life and knowledge-base of the nation.

ESTABLISH

PROVIDE

RELATE

PROVIDE

CONTRIBUTE

University of SaskatchewanInstitute of Space and Atmospheric Studies

Vision for the 21st Century

ENCOURAGE

DEVELOP

INVESTIGATE

Solar Wind

SunBow Shock

Magnetopause

Earth

Tail

Magnetosphere

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