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MITHRAS: a Brief Description Radio Science,Volume 19, Number 2, Pages665-673, March-April 1984 MITHRAS: A brief description O. dela Beaujardidre,x V. B. Wickwar,x M. J. Baron,•'2 J. Holt,3 R. M. Wand,3 W. L. Oliver,3 P. Bauer,4 M. Blanc,• C. Senior,• D. Alcayd•,5 G. Caudal,• J. Foster,6'? E. Nielsen,8 and R. Heelis9 (ReceivedJuly 19, 1983;revised October 28, 1983;accepted October 28, 1983.) BetweenMay 1981and June1982 an intensivecampaign of 33 coordinatedobservations was carried out usingthe threeincoherent-scatter radars capable of probingthe auroral zone.During this period the groupsoperating the Dynamic Explorer satellitesand the STARE radar made specialefforts to acquiredata coincidentwith the radar observations.The objectiveof theseMITHRAS experiments and subsequentanalysis is to further our understandingof the interactionsof the magnetosphere,the ionosphere,and the thermos•here, with special emphasis on local time/universal time variations. Three experimentalmodes with different time resolutionand spatial coveragewere usedto examinedifferent aspectsof these interactions.The analysis of the extensivedata set involves collaboration among groupsof experimentersas well as betweenexperimenters and theoreticians. INTRODUCTION time and universal time dependenceof the observa- tions. The purpose of the MITHRAS (Magnetosphere- The incoherent-scatterradar is a powerfulresearch Ionosphere-ThermosphereRadar Studies)project is tool for the studyof auroral zone phenomenasuch as to study in detail the high-latitudeupper atmosphere ion convection,discrete and diffuse auroras, the mid- using primarily three incoherent-scatter systems: Chatanika (Alaska); Millstone Hill (Massachusetts); latitude trough,field-aligned currents, and neutral at- and EISCAT (Scandinavia),the European Incoherent mosphericcirculation. The radarsprovide data over an extendedaltitude range and a wide geographical Scatter facility. The coordinated experiments were area. The radars enable us to observe the evolution motivated by a need to better understand the cou- of events with a time resolution of a few minutes to a pling between the magnetosphere,the ionosphere, few tens of minutes. and the thermosphere.The upper atmosphereforms Measurements from the Scandinavian Twin Auro- a dynamic systemof considerablecomplexity which, so far, has hindered efforts to fully understand how ral Radar Experiment(STARE) were also utilized. this coupling takes place. A proper combination of STARE operatescontinuously and can measureelec- tric fieldsover a large portion of Scandinavia[Green- detailed and complete observations,together with wald et al., 1978]. In addition, arrangements were theoretical modeling, is necessaryfor progressto be made for the operation of the Dynamics Explorer made. Simultaneousexperiments from different sites (DE) satellitesduring the MITHRAS observations. are necessaryto resolve ambiguities between local The Chatanika, Millstone Hill, and EISCAT sys- tems have been described by Leadabrand et al. x SRI International. [1972], Evans et al. 1-1979],and Folkestad et al. 2 Now at EISCAT Scientific Association. [1983], respectively.The techniquesto infer iono- 3 NortheastRadio ObservatoryCorporation, Haystack Obser- sphericparameters from the direct measurementsare vatory. documentedby Wickwar [1975], de la Beaujardidre '• Centre National d'Etudesdes T616communications/Centrede Recherchessur la Physiquede l'Environnement. et al. [1980], and Holt et al. [1983a]. While • Centred'Etude Spatiale des Rayonnements. Chatanika and Millstone are monostatic, EISCAT is 6 Utah StateUniversity. tristatic.It comprisesa transmitter-receiverstation in 7 Now at HaystackObservatory. Tromso, Norway, and receivingstations in Kiruna, 8 Max-Planck-Institut fiir Aeronomie. Sweden,and Sodankyl•i,Finland. 9 Universityof Texasat Dallas. As illustratedin Figure 1, Chatanika and EISCAT Copyright1984 by the AmericanGeophysical Union. are about 11 hours apart in magnetic local time Paper number 3S1740. (MLT), and Millstone Hill precedesChatanika and 0048-6604/84/003S-1740508.00 follows EISCAT by more than 6 hours. Chatanika 665 666 DE LA BEAUJARDIP•REET AL.: MITHRAS MILLSTONE 06 CHATANIKA 50• INVARIANT 40 LATITUDE 30 24 MAGNETIC LOCAL TIME Fig.1. MLT-invariantlatitude plot of the positions ofthe EISCAT, Chatanika, andMillstone Hillradars whenMillstone Hillis at magnetic noon.The auroral oval is that of Feldstein andStarkov [1968], formoderate activity(Q= 5).The small circles represent theF region areaprobed at500-km altitude andwith an elevation of4 ø, 20ø, and 20 øfor Millstone, Chatanika, andEISCAT, respectively. MLTwas computed forthe month ofJune. andEISCAT are both located at about65 ø invariant signedfor Chatanika,Millstone Hill, and EISCAT. latitude,where they can probethe auroralzone in The objectivesand operatingmodes are outlinedin the E andF regions.Millstone Hill is locatedat 55ø Table 2. invariantlatitude and can probethe auroralzone MITHRAS 1. Thisexperiment was designed to onlyin theF region.The coverage of thethree radars provideF regionmeasurements with the broadest at 500-km'altitude,and the auroraloval for moder- ate activityare also shown in Figure1. Thegeo- TABLE1. Coordinatesfor Chatanika,EISCAT, and Millstone graphicand geomagneticcoordinates of the stations Hill Facilities are listed in Table 1. EISCAT Millstone In thispaper we describethe experimentalmodes Parameter Chatanika(Tromso) Hill and objectives,provide a catalogof the MITHRAS observations,and then briefly summarize some of the Geographiclatitude 65.1øN 69.5øN 42.6øN MITHRAS scientificresults. MITHRAS is described Geographiclongitude 147.5øW 19.2OE 71.5ow Invariantlatitude, A* 65.1ø 66.3ø 55.2ø in greaterdetail by de la Beaujardi•reetal. [1982]. Dipolegeomagnetic longitude 105øW 105øE 1.5ow A coverageat 350-km altitude 560-74ø 61ø-71ø-[- 420_70 ø EXPERIMENTAL MODES L value 5.6 6.2 3.1 Dip angle 77ø 77.6ø 70.5ø Threedistinct experiments were designed and car- Declination 29ø _0.5ø _ 14.1ø ried out for the MITHRAS program;each had a differentprimary objective resulting in different spa- *At 300-km altitude. '•Thesenumbers reflect the largest coverage for the vector veloc- tialcoverage and time resolution. Operating modes ity measurements duringthe MITHRAS operations. Thecoverage consistentwith the experimentobjectives were de- for densityand temperature is wider. DE LA BEAUJARDI•RE ET AL.: MITHRAS 667 TABLE 2. The Three MITHRAS Experiments Time Experi- Resolution, ment Objective min Chatanika Mode Millstone Hill Mode EISCAT Mode Widest latitudinal 30 to 45 11 positions(5 pairs + 1 350ø azimuth scan at 4 ø CP(3).* Several positions coverage parallel to B) elevation along plane at 15ø azimuth. Remote antennas intersect beam F region. Shortest time 10 Three positions(overhead At two north azimuths,and CP(0) or CP(- 1). Troms• resolution measurements);short-pulse for elevations2 ø to 17ø; beam parallel to B. Remote correlator for E region E and F region antennasintersect at parameters measurements heights110 to 700 km. Intermediate time 20 Elevation scanin meridian, 180ø azimuth scannorth of CP(3) (sameas 1). and latitude followed by scan to the west the station at 4ø elevation resolution *CP is commonprogram. The numbersin parenthesesare as follows:0 or - 1 for singleposition mode; 3 for three or more positions along a magneticmeridian; 2 for threepositions, one aboveeach antenna. possible latitudinal coverage. Large-scale studies of marily toward substormstudies of both the E and F electric fields, temperatures,and ionization were em- regions with the best possible time resolution (10 phasized.The time resolution of this experimentwas min). To realize this time resolution, which is neces- 30 to 45 min. sary to study substorm effects,this experiment con- The Chatanika radar was operated in an l 1- centrated on a narrow range of latitudes near the positionmode [Foster et al., 1981]: five pairs of posi- invariant latitude of Chatanika (A - 65øN). In addi- tions straddling the magnetic meridian plane, and tion to the F region electric field, temperatures,den- one position parallel to the magnetic field, B. With sities,and meridional wind, a wide range of E region this mode a large latitudinal coveragewas possiblein parameters were obtained at Chatanika. These E the F region, and at the same time the E region region parameters included conductivities, electron electrodynamic parameters could be determined energy depositionrates, differential energy spectraof closeto the radar latitude. Every hour and a half, the precipitating electrons, neutral winds, currents, and radar was scannedin elevation in the magnetic meri- Joule heating. At Tromso, some of these E region dian plane. This scan gave the cross section of the parameters were also measured. ionization profile as a function of height, with a fine The operating mode for Chatanika consistedof a latitudinal resolution. set of three positions, one parallel to the magnetic The Millstone radar was operated at a fixed eleva- field and the two others on either side of the mag- tion (typically 4ø ) in an azimuth scancovering almost netic meridian at 70ø elevation [Rino et al., 1977]. the full circle [Holt et al., 1983a]. This operating The velocity and temperatureswere obtained with a mode had the advantage that longitudinal effects fine (9-km) altitude resolution for E region measure- could be studied by comparing the measurementsto ments, and with a coarser (50-km) resolution for the the east and to the west. In 1982 the azimuth scans F region. were followed by an elevation scan, horizon
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