United States program report: International Years of the Quiet Sun, 1964-65; a report to the IVth General Assembly of the IQSY on the status of the United States program. (1967)

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A P P E N D I X I I : S U M M A R Y OF SATELLITE A N D R O C K E T L A U N C H E S D U R I N G THE l O S Y 169

A P P E N D I X n T A B L E 1: S A T E L L I T E AND S P A C E P R O B E S O F S C I E N T I F I C I N T E R E S T T O T H E IQSY O P E R A T I N G DURING IQSY (1964-65) Scientif ic Designation Popular Name Laimch Date Per igree (km) Apogee (km) Per iod Inclination (degrees) 1 9 6 2 - B A l Alouette 1* r 9/29/62 998 1,046 105 80 1963-24A T i r o s 7 6/19/63 620 646 97.4/3] 58.2 1963-39A V e l a 1 10/16/63 63,441 70,631 105 38.3 1963-39C V e l a 2 10/16/63 62,806 72,974 108.7 38.0 1963-46A Explorer 18(IMP-1) 11/27/63 192 197,616 5666 33.34 1963-53A E x p l o r e r 19 (AD) 12/19/63 592 2,385 115.8 78.60 1963-54A T i r o s 8 12/21/63 702 753 99 58.5 1964- lD S O L R A D l | l l / 6 4 909 931 103.4 69.9 1964-3A Relay 2 1/21/64 2,089 7,413 194.7 46 .3 1964-40A V e l a 3 7/17/64 63,369 65,024 100.3 39,5 1964-40B V e l a 4 7/17/64 58,766 69,482 100.1 40 .9 1964-40C T R S - 6 7/17/64 192 104,333 '36.'9—^ 1964-45B None 8/14/64 266 3,765 127.4 95.6 1964-5lA E x p l o r e r 20 8/25/64 866 1,009 103,8 89,9 1964-52A Nimbus 1 8/28/64 422 931 98.3 98,7 1964-54A OGO 1 9/^5/64 283 149,420 3839 31,1 1964-60A E x p l o r e r 21(IMP-2) 10/4/64 191 95,596 2097 33.5 1964-64A E x p l o r e r 2 2 ( B E - 2 ) 10/10/64 881 1,088 104,8 79.7 1964-76A E x p l o r e r 24 (AD) 11/21/64 524 2,497 116.20 81.4 1964-76B E x p l o r e r 25 (Injun-B) 11/21/64 524 2,492 116.15 41.4 1964-77A Mariner 4 11/28/64 heliocentric orbit on trans trajectory - M a r s 1964-830 None 12/13/64 1,029 1,080 106.3 90 1964-88A E x p l o r e r 26 12/21/64 306 26,200 456 20 •Canadian satellite 170

Scientific Designation Popular Name Launch Date Perigree (km) Apogee (km) Period Inclmation 1965-4A Tiros 9 1/22/65 740 2,580 119 96 1965-7A OSO 2 2/3/65 552 632 97 33 1965-16D SOLRAD 3/9/65 909 941 103,5 70.08 1965-32A Explorer 27(BE-C) 4/29/65 940 1,318 108 41 1965-42A Explorer 28(IMP-3) 5/29/65 190 264,000 8550 34 1965-5lA Tiros 10 7/2/65 752 839 100.8 98 6 1965-58A Vela 5 7/20/65 88,571 96,201 5148.2 35,27 1965-58B Vela 6 7/20/65 101,835 121,475 6726 1 34,99 1965-58C ORS 3-1 (ERS 17) 7/20/65 153 112,694 2610.6 34.39 1965-78A OVl -2 10/5/65 412 3,454 125,7 144.31 1965-81A OGO 2 10/14/65 414 1,510 87.36 104.31 1965-93A Explorer 30 11/19/65 709 883 100.79 59.72 1965-98A Alouette 2* 11/29/65 529 2, 956 121.39 79 72 1965-98B Explorer 31 11/29/65 521 2,963 121.37 78.82 1965-lOlA FR-1** 12/6/65 743 723 99.99 75, 8 1965-105A Pioneer 6 12/16/65 heliocentric orbi t * Canadian satellite **French satellite 171

SATELLITES AND SPACE PROBES OF SCIENTIFIC INTEREST TO THE IQ6Y OPERATING DURING IQSY (1964-65) NOTES Alouette 1 (1962-BA 1) See Alouette 2 (1965-98A) Tiros '7 (1963-24A) and Tiros 8 (1963-54A) Two meteorological satellites launched during 1963 operated during the IQSY: Tiros 7, launched on June 19, and Tiros 8, launched on December 21 , 1963. The Tiros 7 (Television and Infrared Observations Satellite) spacecraft was cy lmdr ica l , 107 cm in diameter and 48 cm in height, s imi la r to ear l ier members of the series. Slightly heavier than its predecessors, i t weighed 133 kg. Two television cameras havmg the same fields of view were aligned parallel to the spin axis, which was perpendicular to the base of the structure. When this axis was normal to the esirth, each camera provided pictures of areas covering 1,340 by 1,340 k m . Two infrared experiments were also car r ied as part of the satellite mstrumentation. One was a medium-resolution instrument designed at Goddard Space Flight Center, and the second was a radiation-balance mstrument designed at the University of Wisconsin. Tiros 7 was the f i r s t m the series to incorporate an electrostatic probe, designed to yield measurements of electron temperature, electron density, ion density, and photoemission current . Ti ros 8 carr ied an experimental camera system designed to give meteorolo- gists mstantaneous photographs of cloud patterns. A new experimental camera subsystem, called Automatic Picture Transmission (APT), was tested f o r the f i r s t t ime aboard Tiros 8. In addition to the APT camera subsystem. Tiros 8 contains a television camera s imi l a r to that f lown on previous Ti ros satelli tes. The automatic picture-transmission system. Unlike the television subsystem carr ied i n the early Ti ros satellites, APT transmitted pictures on the slow-scan pr inciple , s imi lar to that used to send radio photographs. By building relat ively simple and inexpensive receivers , meteorologists can obtain cloud-cover photo- graphs of their own regions as the image forms on the facsimile machine at their stations. (Meteorologists i n many countries have done so.) Each APT ground sta- tion can receive up to three photographs during one pass, depending on the satellite's angle above the horizon. The satellite must be wi thin a 2,300-km radius of the station fo r picture reception. A complete photograph cycle takes 208 seconds. 172

Four major elements make up the APT subsystem in the spacecraft: the sen- sory housmg containmg the camera, vidicon, and vidicon electronics; a video elec- tronics module consisting of a video detector and t immg and switchmg c i rcui t s ; power converters; and an F M transmitter . The entire subsystem weighed 11 kg. The lens used in the APT system is a 5,7 mm f / l . 8 Tegea Kmoptic wi th a 108° f ie ld that could photograph an area of approximately 1,340 km on a side ( 1 , 8 x 10^ km^) when the satellite was lookmg directly toward the Ear th . A 3-msec ex- posure controlled by the electromagnetic shutter produced an 800-scan-lme picture on the photosensitive surface of a special 2 .5-cm diameter vidicon. A t imer m the APT subsystem programmed the equipment fo r contmuous cycles of prepara- tion, exposure, development, and direct-readout fo r approximately 30 mmutes of each o rb i t . The prepare-expose-develop phases took place in the f i r s t eight sec- onds on each 208-second picture cycle. The remainmg 200 seconds were used to read out the photographs at a scan-rate of four Imes per second. Although the vidicon used in the APT subsystem resembles an ordmary tele- vision vidicon, an added polystyrene layer provides extended image-storage capa- b i l i t y . The image is projected on a prepared photoconductive layer, and is then transferred by potential change to the storage layer f o r readout. The television recordmg system. As on previous Tiros satellites, the record- mg television subsystem aboard Tiros 8 consisted p r imar i ly of a television camera and circui ts for magnetic-tape recordmg and transmission. The camera, wi th a 104° lens, can transmit images direct ly to a Tiros Command Data Acquisition Sta- t ion, or store the images on a tape recorder fo r readout when the spacecraft passes withm a 2,400-km radius of a ground station. Pictures transmitted f r o m the satellites are reconstructed on special kmescopes at the ground station and photographed by 35-mm cameras. The television tube is a 500-lme scan, 13-mm vidicon that permits a two-second scan t ime. A maximum of 32 pictures can be recorded and stored durmg each orb i t . Transmission t ime takes about three mmutes and begms when the satellite receives a radio command f r o m the groimd station. Velas 1 and 2 (1963-39A and C) See Velas 3 and 4 (1964-40A and B) Explorer 18 ( I M P - 1 , 1963-46A) See Explorer 21 (EVIP-2, 1964-60A) Explorer 19 (1963-53A) See Explorer 24 (1964-76A) 173

Tiros 8 (1963-54A) See Tiros 7 (1963-24A) SOLRAD (1964-lD) This satellite was launched in January 1964. As the only solar observatory functioning in orbi t during the f i r s t year of the IQSY, i t has provided important backgiound data on solar minunum x-ray fluxes in three wavelength bands: 1-8A; 8-2 OA , and 44-6 OA . Throughout the f i r s t eight months of 1964, the background x- ray f lux was as low as the minimum observed m 1953 to 1954. Evidences of solar activity took the f o r m of small mcreases m plage-associated activity and occasional weak f la res . Among the more mteresting observations of x-ray activity is a phenomenon that may be called a "solar x - ray noise s t o r m . " A smal l f l a re may mitiate a series of sporadic flashes appearmg m a l l three wavelength bands. These flashes may last only a minute or as long as 15 minutes and be over an hour apart. Once the series began, the bsickground mcreased markedly and was observed even at the shortest wavelengths, which normally show no detectable signals. Although sharp flashes (about 1 mmute duration) have m the past been observed by balloon-borne appara- tus sensitive to x-rays of energy greater than 20 keV and by the 20-100 keV detec- tor car r ied aboard OSO-1, the SOLRAD results were the f i r s t examples of sharp flashes at longer wavelengths. The duration of the noise s torm may be several days. It is rather remarkable that f lux increases of several hundred percent and the return to background can take place in one mmute of t ime at wavelengths as long as 50A. The emission areas fo r this wavelength range are normally of the order of f ive or more mmutes of arc in diameter. I t is also known f r o m highly r e - solved rocket spectra that at least 90% of the radiation m the 44-60A band o r i g i - nates in the coronal lines Si IX and Si X . The SOLRAD satellites have used real - t ime telemetry, which permits them to be received by foreign observatories. Reports of reception have been published or annoimced by the fol lowing: University of Adelaide, Austral ia ; Max Planck Institut f u r Aeronomie, Germany; Astronomical Observatory, Czechoslovakia; Physical Research Laboratory, India; University of Mi lan , I taly; A r c e t r i Observatory, I taly; DSIR Radio Research Station, Slough, England; University of Paris , France; Radio Research Laboratories, Japan; and K inma Geophysical Observatory, Sweden. Relay 2 (1964-3A) The experimental communications satellite 1964-3A (Relay 2) also car r ied some mstruments f o r monitormg energetic part icles . I t was launched on January 21 , 1964, mto an orb i t wi th perigee at 2,089 km and apogee at 7,413 km; mcl ina- t ion, 46° ; and period, 195 minutes. The spacecraft was spin-stabilized and, in 174

addition to the communications equipment, car r ied instruments prepared at the State University of Iowa f o r the measurement of protons m the energy ranges 1 to 8 MeV, 18-60 MeV, and 40-300 MeV; and electrons of 0.4-1.2 MeV. Additional detectors provided by the Bel l Telephone Laboratories measured protons of energies 2.5-25 MeV and electrons of 0.6-1.6 MeV. Vela 3, 4, 5, and 6; TRS-6 (ERS-13), and 0RS3-1 (ERS-17) The Vela satellites have been launched m pairs , and placed m high (100, 000 km) approximately c i rcu lar orb i t s . Each satellite is spin-stabilized, and carr ied out 40 kg of mstruments to detect gamma rays, x- rays , ultraviolet radiation, and neutrons, and a proton spectrometer to obtain data about particles and radiation origmatmg m the upper atmosphere, the Sun, or the galaxy. In addition, Vela 3 and 4 were accompanied by the 2-kg pickaback Tetrahedral Research Satellite TRS-6 (one of the Environmental Research series), which car r ied omnidirectional radiation detectors to measure electrons wi th energies greater than 0,7, and 5 MeV, and proton fluxes at 12-23 MeV and 39-50 MeV. I t yielded data on the radia- tion belts f r o m July 1964 to January 1965. Velas 5 and 6 were accompanied by the f i r s t Octahedral Research Satellite, Mark m, (0RS3-1), which weighed 5 kg and car r ied f ive experiments to measure trapped radiation, cosmic rays , solar and cosmic gamma rays, and solar x - rays . The satellites were a joint enterprise of the Advanced Research Projects Agency, the A i r Force, the Atomic Energy Com- mission and its contractors (Los Alamos Scientific Laboratory and Sandia Corp . ) , and others. Explorer 20 (1964-51A) Explorer 20 (nicknamed "Tops i , " also designated S-66 during early planning), car r ied a radio sounding experiment, ion mass-spectrometer experiment, and cosmic noise experiment, and was launched on August 25, 1964. The topside sounding experiment consisted of six transmitters that radiate upon command RF energy pulses in sequence on 1.2 MHz, 2.0 MHz, 2.85 MHz, 3.72 MHz, 5.47 MHz, and 7.22 MHz. The resultant reflections f r o m the topside of the F2 ionos- pheric region were received by three siq)erheterodyne dual-frequency sounder receivers in the mtervals between transmitted pulses. 175

Nimbus 1 (1964-52A) The Nimbus developmental meteorological satellite, launched f r o m the Western Test Range by a Thor Agena B laimch vehicle on August 28, 1964, was designed by NASA as a research spacecraft f o r testmg new camera systems and a control system to keep the cameras always pomtmg toward the Earth. RCA supplied the following major subsystems fo r Nimbus: i (1) Advanced Vidicon Camera System (AVCS). This comprised three 2 .5 -cm, vidicon cameras providing 800-line cloud-cover pictures of areas 800 by ; 2,400 km which were stored and played back to ground stations in Alaska and : in North Carolma, when the satellite was over the station. ' (2) Automatic Picture Transmitt ing System (APTS). This system transmits real- t ime cloud pictures to simple and relatively inexpensive groimd sta- i tions when the satellite is overhead. These pictures are reproduced on a facsimile recorder and cover an area 1600 km square, (3) Special tape recordmg and multiplexmg equipment f o r a high-resolution mfrared radiometer system (HRIR) fo r taking nighttime cloud pictures. (4) The spacecraft power system, comprismg approximately 11,000 sil icon photovoltaic cel ls , storage batteries, regulators, and control equipment. The solar cells are mounted on two 240 x 75 cm paddles which are kept facmg the Sun f o r greatest efficiency. It is believed that this is the largest and most powerful solar-cel l power sv5)ply yet to be put i n orb i t . The AVCS and APTS systems were later used m operational meteorological satellites of the Tiros fami ly (TOS) developed by RCA fo r the U.S. Weather Bureau. During 1964 a complete prototype of a commercial automatic picture taking station (APT) was developed and tested in conjimction with T i ros 8 and Nimbus 1. The imattended automatic operation feature, conceived and developed by RCA, is made practicable by an antenna that provides horizon to horizon high-gam coverage with electronic beam steermg. Pictures are taken whenever a satellite is in sight of the station without preprogrammmg or knowledge of the satellite t ime or position. Two to f ive pictures of the Earth can be obtamed durmg one pass. The high resolution infrared radiometer (HRIR) experiment on Nimbus 1 has demonstrated the capability of mappmgnighttime cloud-cover and cloud heights wi th suf- f icient resolution to permit synoptic meteorological analyses and to recognize t e r - ra in features such as mountain ranges, large r i ve r s , and the boundaries between land and water. Radiation intensity levels correspondmg to equivalent black-body temperatures withm a range f r o m 210° K to 330° K were resolved with an accuracy of 2°K or better. The spectral response of the radiometer was in the atmospheric window f r o m 3.4 to 4 .2^ . Radiative cooling of the PbSe ce l l to the desired t em- perature of -75°C was achieved within less than 3 hours after laimch, and the 176

cooling remained stable thereafter. The calibration of the radiometer remamed stable throughout its l i fe t ime , and there was no degradation of the characteristics of the detector ce l l , cooling cone, scanning m i r r o r , or interference f i l t e r . Dur - ing the 369 orbits of operation, data f r o m 260 nighttime orbits were acquired, each covering a s t r ip ranging essentially f r o m pole to pole as the mstrument scanned f r o m horizon to horizon along lines perpendicular to the orbi ta l t rack. The scan frequency was about 45 lines per minute, and the usable width of each orbi ta l s t r ip , determmed by the altitude of the satelli te, was of the order of 2000 k m . OGO 1 (1964-54A) The f i r s t of a series of large geophysical observatory satellites, OGO-1 was launched on September 5, 1964, into a high eccentric Earth orbi t which was mtended to permit the satellite to make measurements m the Earth's atmosphere and mag- netosphere and m interplanetary space beyond the influence of the geomagnetic f i e l d . I t weighed about 500 kg, of which nearly 100 comprised the payload of scien- t i f i c mstruments. The quality of the data f r o m some of the experiments was de- graded by the fai lure of the three-axis stabilization and its replacement by spm- stabilization at 5 r p m . OGO 1 carr ied 20 experiments, almost a l l relevant to the IQSY: (1) Scintillation detector f o r solar cosmic-ray fluxes (10-90 MeV), Anderson, U . California, Berkeley; (2) double gamma-ray spectrometer to measure positrons (0-3 MeV) and to monitor solar proton bursts (30 keV to 1.2 MeV), Cline, GSFC, and Hones, IDA; (3) directional scinti l lat ion detectors fo r trapped electron fluxes (10-100 keV), and proton fluxes (120-4500 keV), Konradi et a l , GSFC; (4) cosmic- ray telescope f o r galactic cosmic ray isotope abimdance, McDonald and Ludwig, GSFC; (5) charged-particle telescope low-energy galactic cosmic-ray f lux to study protons above 0.2 MeV, and other nuclei at higher energies, Simpson, Fan, and Meyer, Fe rmi Ins t . , U . Chicago; (6) Geiger tubes to measure omnidirectional mtensities of trapped electrons wi th E > 4 0 keV, 120 keV, and 1.5 MeV, Van Allen and Frank, U . Iowa; (7) magnetic electron spectrometer to measure electron energy up to 4 MeV; ionization chamber and Geiger counters to monitor trapped radiation and galactic cosmic radiation between 20 keV and 20 MeV, Winckler and Amoldy , U . Minnesota; (8) t r i ax ia l search-coil magnetometer, f o r fluctuations in vector magnetic f i e ld (0.01 to 1000 cps), Smith, J P L , and Holzer, UCLA); (9) rubidium vapor and t r i ax ia l fluxgate magnetometers f o r magnitude and direction of magnetic fields (1 to 14,000 gammas), Heppner, GSFC; (10) electrostatic analyser, f o r proton concentration (10~2 to 10~^/cm^) as a function of proton energy 0.2 to 20 keV), Wolfe, Ames Res. Center, NASA; (11) Faraday cup plasma to measure solar wind plasma f lux and energy spectrum, and their variations (10 eV to 10 keV), Bridge et a l , M I T ; (12) spherical three-electrode probe fo r density and energy distribution and positively and negatively charged particles (0 to 1.0 keV), Sagalyn and Smiddy, AFCRL; (13) planar ion and electron trap fo r densities, fluxes, masses, and energy distributions of thermal ions and electrons, Whipple, 177

GSFC; (14) continuous synoptic survey of V L F noise and propagation character- istics (0.2 to 100 kHz), Hel l iwel l and Rorden, Stanford U . , and Stanford Res. Ins t . ; (15) frequency receiver (2 to 4 MHz) f o r survey of cosmic radio emission. Haddock, U . Michigan; (16) atmospheric electron content using Imearly polarized radio beacon fo r electron content (40 to 360 MHz), Lawrence and Chivers, CRPL (now ITSA); (17) RF ion mass spectrometer f o r density of positive ions (1-50 AMU and 10 to Taylor and Spencer, GSFC; (18) micrometeoroids, Alexander and McCracken, GSFC; (19) ion chambers fo r Lyman-alpha scattermg to determine the distribution of neutral hydrogen m the geocorona. Mange, NRL; and (20) mult icolor Geigenschein photometry, Wolff , Hallam, GSFC and Wyatt, U , I l l i no i s . Explorer 21 (IMP 2, 1964-60A) The second mterplanetary Explorer satelli te, IMP 2 was laimched on October 4, 1964. In i t ia l perigee was 191 km; apogee, 95,956 km; mclination, 33.5"; and period, 34 hours 57 mmutes. Like the f i r s t IMP satellite, the p r imary objectives of IMP 2 were to meas- ure magnetic f ie lds , cosmic rays, and solar wmds in interplanetary space. The spacecraft did not achieve as highly eccentric an orbi t as planned, but useful data are being received f r o m a l l instruments. IMP 2 car r ied nme scientific exper i - ments f r o m several laboratories and universi t ies, as l isted below: Cosmic Rays (1) Range vs . Energy loss: The purpose of this experiment is to search f o r solar-proton or alpha-flare events. Hie apparatus is designed to measure protons of energies between 100 keV and 200 MeV. F i r s t flown on the Mariner spacecraft, the device employs solid-state detectors and a range-energy loss telescope to study the particle spectrum and its nuclear composition, concen- trating on hydrogen, helium, and l i th ium. (Simpson, U . Chicago). (2) Orthogonal Geiger-counter telescope ar ray: This experiment is designed to study the i so- tropy of solar proton events m cosmic-ray modulation. (McDonald and Ludwig, GSFC). (3) Part icle telescope: This experiment is to obtam data on t ime va r i a - tions m fluxes of energetic electrons m the mterplanetary region beyond the Van Allen region and to measure the energy spectrum of protons and other heavy par- t ic les . The apparatus is designed to measure the f lux of galactic cosmic rays; iden- t i fy hydrogen, deuterium, t r i t i u m , and helium in the energy range of 12 to 18 MeV; and to measure the f lux of electrons of energy f r o m 1 to 20 MeV. (McDonald and Ludwig, GSFC), (4) Neher-type ion chamber: This mstrument measures total ionization produced per unit volume of standard-density air as a function of t ime . I t IS intended to serve as a basic radiation monitor . Chambers of this type have been flown m Explorer 6 and Pioneer 5. (K. Anderson, U . Cal i fornia , Berkeley). Berkeley). 178

Solar Wind. (5) Low-energy proton analyzer: Proton concentrations are de- termined as a function ot kinetic energy. Particles enter the apparatus through a slit in the satellite skm and are separated according to energy by a variable curved-plate electrostatic analyzer. The energy range is from about 200 eV to 20 keV. (Wolfe, NASA Ames Res. Ctr) (6) Plasma probe: This probe measures the flux of low-energy particles m particle-velocity increments between 10 km/ sec and 100 km/sec. Charged particles entering a 15-centimeter-diameter aper- ture pass through a series of grids maintamed at potentials which reject electrons and low-energy positive particles. This mstrument has been flown on Explorer 10 (Bridge, MIT) (7) Thermal ion and electron experiment: This experiment measures the concentration and temperatures of thermal electrons (energies less than a few electron volts), and the concentration, masses, and temperatures of thermal ions. (Bourdeau and Serbu, NASA Groddard Space Flight Center.) Magnetic Fields (8) Rubidium-vapor magnetometer: The magnetometer measures the total vector magnetic field mdependent of orientation. A similar unit has been flown on Explorer 10and Banger 1. (Ness, GSFC) (9) Fluxgate magnetometers: Two saturable-core fluxgate magnetometers are used to determme the direction of fields m regions where the field strength is less than 30 gammas (30 x 10~5 G) . (Ness, GSFC) Explorer 22 ( B E - 2 . 1964-64A) Explorer 22, a polar ionospheric beacon satellite, was launched on October 10, 1964. Ionospheric irregularities were mapped by a three-station 150 km baselme system of Faraday receivers monitormg transmitters. The receivers contmuously monitored polarization orientation by electronically simulated antenna rotation and the signal was recorded on film. Explorer 24 (Air Drag Satellite, 1964-76A) Explorer 24, a 4-meter sphere inflated m orbit like Explorer 19, was launched mto a highly mclmed orbit on November 21, 1964. The high area-to-mass ratio of these two Explorer satellites makes them sensitive to atmospheric drag, which provides data on air density. The objectives were: (1) to extend the upper air density measurements to the polar regions; (2) to determme density and temperature variations of the atmosphere as a function of latitude; and (3) to determme sources of atmospheric, heatmg by comparison measurements with other satellites such as Explorer 19. ' The measurement of air density on Explorer 24 was similar to the experiment with Explorer 19, which was placed in orbit on December 19, 1963. World-wide optical-trackmg measurements of Explorer 24's orbital changes supplied the 179

information needed to determme drag and, hence, atmospheric density at selected pomts along the orbital path. Comparison of latitude and day-to-day density v a r i a - tions were obtamed by usmg data from both E x p l o r e r 19 and E x p l o r e r 24. The relative effects of solar-mduced disturbances on the atmosphere also were compared. E x p l o r e r 25 '(Injun-B, 1964-76B) The Injun E x p l o r e r satellite Exp lorer 25, built and operated by the State U n i - vers i ty of Iowa group, was launched on November 21, 1964. Init ial perigee was 524 km; apogee, 2492 km; period, 116.15 mmutes; and mclmation, 4 1 . 4 ° . The objectives of E x p l o r e r 25 were: (1) to measure the bombardment of the atmosphere by energetic part ic les f rom space, and (2) to sample the concentration and energy distribution of the charged part ic les over the energy ranges 0 .2-2 MeV for electrons and 0-40 MeV for protons. The pr imary scienti f ic mstruments of the satellite consisted of 5 omnidirectional sensors and 11 directional mstruments. Three of the omnidirectional sensors measured protons and electrons m different ranges of energy. The other two were spher ica l retardmg potential analyzers mounted on booms, The 11 directional detectors were mtended to look m great detail at the r a d i a - tion environment through which the satell ite passes , respondmg only to partic les a r r i v m g from specif ic directions. The detectors were: 4 Ge iger -Muel l er tubes, 2 scmtiUation counters, 3 cadmium-sulphide-type detectors; 1 cadmium-sulphide detector equipped with a shielding magnet to divert low-energy protons, 1 P - N junction detector with a d i scr immator c i r c u i t . M a r m e r 4 (1964-77A) M a r m e r 4 was launched from the E a s t e r n Tes t Range on November 28, 1964, and passed withm 10, 000 km of Mars on July 14, 1965. In addition to mstrumen- tation to take television pictures of M a r s durmg the f ly -by , M a r m e r 4 c a r r i e d seven experiments designed to make scientif ic measurements in mterplanetary space between E a r t h and M a r s as wel l as m the vicmity of M a r s itself . The scientif ic mstrumentation consisted of the followmg: (1) a so lar -p la sma probe was designed to measure velocit ies , temperatures, and directions of low- energy protons (0. 03-10 keV) of the so lar wmd (MIT and J P L ) ; (2) an ionization chamber and Geiger-Muel ler tube to measure galactic cosmic rays havmg energies > 10 MeV for protons, > 0.5 MeV for electrons, and > 40 MeV for alpha part ic les (the Geiger -Muel ler tube ceased functionmg properly as M a r m e r 4 approached the half-way pomt of the flight) (U. Chicago); (3) a trapped-radiation detector. 180

consisting of three G-M tubes and a solid-state detector; the G-M tubes were designed to detect > 0.5 keV protons and >0.04 keV electrons (tubes A and B) and >0 .9 keV protons and > 0.07 electrons (tube C), and the solid-state detector was designed to measure protons in the ranges 0.5 keV to 8 MeV and 0.9 keV to 5.5 MeV; this equipment measured cosmic rays and electrons durmg the cruise por- tion of the mission (U. Iowa); (4) a helium-vector magnetometer to de- termine whether Mars has a magnetic f i e l d , and to map the characteristics of such a f i e ld i f detected, as we l l as the magnitudes, directions, and variations of magnetic fields m space (JPL, UCLA, CITand Brigham Young U . ) ; (5) a cosmic- ray telescope to detect cosmic rays and determme types, energy levels, and directions of motions (CIT and JPL); (6) a cosmic-ray detector, and (7) a two- frequency radio transmitter to transmit through the Martian atmosphere. 1964-83C The A i r Force-Navy satellite 1964-83C was launched on December 13, 1964 into a c i rcular polar orbit with an altitude of about 1050 km; the satellite carr ied a Varian rubidium magnetometer for the Applied Physics Laboratory of the Johns Hopkms University to obtain scalar magnetic mtensity values. Explorer 26 (1964-86A) The energetic particles satell i te. Explorer 26 (1964-86A), was launched on December 21 , 1964. Ini t ia l perigee was 306 km; apogee, 26,200 km, period, 456 mmutes; and mclmation, 2 0 ° . The purpose of this satellite was to study the injection and loss of high-energy particles into and f r o m the magnetosphere. Measurements were made on the spatial and angular distribution and energy spectra of electrons and protons, the mtensity and angular distribution of electrons and protons; the magnitude and direction of the Earth's magnetic f i e ld ; the f lux of relat ively low-energy particles by type, and their energies as a function of direction, t ime, and position; and damage to solar cells by natural and trapped radiation. The f o U o w i i ^ is a l i s t of the experiments carr ied: (1) Electron-proton angular Distr ibution and energy spectra detectors: A series of solid-state detectors to measure the spatial and angular distribution and energy spectra of electrons and protons. (W. L . Brown, Be l l Telephone Labs). (2) Electron-proton direct ional- omni-directional detectors. Scintillator-type detectors or iginal ly developed fo r the Relay communications satell i te, to measure the intensity and angular d i s t r ibu - tion of protons and electrons. (C .E . Mcl lwain, U . C a l i f . , San Diego). (3) Magnetic- f i e ld measurements (flux gate magnetometer). This instrument is measuring the mag- nitude and direction of the Earth's magnetic f i e ld f r o m about 9,700 km above the Earth out to the satellite's apogee. (L . Cahi l l , U . New Hampshire). (4) I o n - Electron detector. Scintillation detector designed to measure relat ively low-energy 181

particles by type and energy as a function of direction, t ime, and position. ( L . R . Davis and J . M . Will iamson, GSFC) (5) Solar-cell damage. The purpose of this experiment is to provide a means of determming damage to a group of solar cells by radiation f r o m the Van Allen radiation region and a r t i f i c i a l radiation belt. ( L . W . S l i fe r , GSFC) Tiros 9 (1965-4A) Tiros 9 was launched on January 22, 1965, f r o m Cape Kennedy into a near- polar o rb i t . This satellite was part of a contmuing United States program to ob- tam worldwide meteorological mformation with satelli tes. Its major objectives were: (1) to produce observations of the atmosphere over the entire globe; (2) to provide as completely contmuous observations as are scientif ical ly required and technologically possible, and (3) to evaluate the cartwheel configuration of the Tiros satellite. Recordmg Television System. The recordmg television system included two identical TV camera and c i rcui ts fo r magnetic tape recordmg and TV transmission s imi la r to those carr ied on previous Tiros missions. The two cameras, moimted on the side of the spacecraft, are canted 26 degrees to each side of the plane of the satellite's rotation so they can view the Earth once every revolution (every six seconds). An on-board t imer programs the cameras to take pictures only when the satellite is looking straight down at Earth. The TV tube is a 500- scan Ime vidicon with a persistence that permits a two-second scan with less than 20% degradation m picture quality. Each camera uses a wide-angle (104°) Elgeet lens capable of photographmg a square f ie ld about 1200 km on a side, with a reso- lution of about 3 km at picture center. The camera system allows pictures to be stored on the Vidicon tube face fo r a brief period. An electron beam converts a stored picture into a TV-type electronic signal which is then radioed to a groimd station or recorded on magnetic tape fo r readout when the satellite is withm a 2400-km radius of a ground station. Up to 96 pictures can be recorded and stored by Tiros 9 durmg each o rb i t . Readout, which takes about three mmutes, is accomplished at a ground station by radio command. This process automatically erases the t ^ e s . Operation of the cameras, by direct readout or magnetic tape storage tech- niques, I S controlled by radio commands relayed f r o m a ground station. These commands set t imers m the satellite which activate the camera system when the satellite passes over an area f r o m which cloud-cover pictures are desired. At the ground stations, which are located at Wallops Island, Vi rg in ia ; Gilmore Creek, Alaska; and at San Nicholas Island, Cal i fornia , TV pictures received f r o m the satellite are reproduced on special kinescopes and photographed by 35-mm cameras. 182

OSO 2 (1965-7A) The second Solar Orbitmg Observatory, OSO 2, was launched on February 2, 1965 with the objective of studymg the Sun's structure and behavior and of deter- mming the physical processes by which the Sun mfluences Earth; seven experi - ments relevant to the IQSY were carr ied on the satellite: The four m the pointed section were: (1) a group of solar X - r a y monitors and X - r a y pmhole cameras covermg the wavelength regions 2-8 A, 8-20 A, and 44-60 A (NRL); (2) a white-l ight coronagraph (NRL); (3) a spectroheUograph operating m Lyman-alpha, at 304, 584 and 1216 A (NRL); and (4) an ultraviolet spectrometer-spectroheliograph, de- signed to scan the spectrum at 300-1400 A, or to scan the Sun's disc at a selected fixed wavelength (Harvard Universi ty) . The last experiment suffered a malfunc- tion and produced no useful data. The wheel section of OSO-2 car r ied the followmg mstruments: (1) a gamma- ray spectrometer f o r the energy range 0.1-3 MeV (GSFC); (2) a photometer to measure the mtensity and degree of polarization of the zodiacal light (U. Minnesota); and (3) a pr imary cosmic-ray detector f o r the energy range 50-1000 MeV (U. of New Mexico). SOLRAD (1965-16D) The solar radiation satellite, 1965-16D, was launched on March 9, 1965 to contmue the monitormg of solar X- ray emissions m six wavelength regions: 0.5-3, 1-8, 8-12, 8-14, 44-55, and 44-60 A, which began with earl ier solar radia- tion satellites. The 1965-16D detectors were considerably more sensitive and provided the f i r s t good readmgs durmg low-activity periods. To fur ther reduce their response to mterference, 0.25 mm thick beryl l ium sheets are cemented to the pole faces of the broom magnets to reduce bremsstrahlung production. An aspect sensor is mcluded to provide a measurement which may be used to make a correction to the X - r a y photometer responses fo r the angle between the satellite's equatorial plane (containing the photometer direction of view) and the direction f r o m the satellite to the Sun. The aspect angle changes slowly wi th time due to mteraction between the broom magnets m the satellite and the Earth's magnetic f i e l d . These magnets have been matched agamst one another to reduce the net magnetic moment of the satellite to the smallest practical value. This should result m a more stable and slower precession than was observed m 1964-lD. Explorer 27 (1965-32A) The Beacon Explorer satellite. Explorer 27 (also designated BE-3 or BE-C) was launched f r o m Wallops Island, V a . , on A p r i l 29, 1965, to allow a comprehensive study of the Earth's ionosphere, to measure the effects of i r regular i t ies m the 183

Earth's gravitational f i e ld usmg a Doppler t ransmit ter , and to measure the electron densities and temperatures m the immediate vicmity of the satellite. Experiment relevant to the IQSY were as fol lows: (1) Ionospheric beacon e:q)eriment: The ionospheric beacons transmit contmuously on 20.005, 40.010, and 41.01 at 250 MHz and 360 mW at 100 mW, a l l derived f r o m a common osci l lator . About 86 ground stations operated by some 62 scientific groups m 36 countries received signals and obtamed mformation on ionospheric electron con- tent and i r regular i t ies . Measurements of electron distribution along the Ime of sight between the satellite and a ground station can be made by the Doppler Shift or Faraday Rotation methods. (2) The electrostatic probe experiment: The electrostatic probe experiment measured direct ly the electron density and tem- perature m the spacecraft's immediate vicmity complementing the ionospheric beacon experiment at the startmg pomt of the radio beacon signals. Two sensors, one at the top of the spacecraft and the other at the bottom, extend 25 centimeters mto the plasma surroundmg the satellite. Each sensor consists of a cyl indr ical electrode msulated f r o m the spacecraft. A voltage is applied alternately to each sensor and the resultmg currents are detected and converted to telemetry signals. Explorer 28 (1965-42A) Explorer 28. Explorer 28 (Interplanetary Monitormg Plat form or IMP 3) was launched on May 29, 1965, mto an orbi t wi th apogee at 264,000 km, perigee at 195 km, and mclmation of 3 3 . 8 ° . The pr imary objective of Explorer 28 was to mvestigate the mterplanetary environment, specifically cosmic rays, the solar wind, and the mterplanetary magnetic f i e l d . Explorer 28 essentially a duplicate of Explorer 21 (IMP 2) car r ied a total of nine experiments, of which six performed as expected. The experiments aboard the spacecraft are as follows (cosmic rays, 1-4; solar wmd, 5-7, magnetic f ie lds , 8 & 9): (1) range vs . energy loss (Univ. Chicago), to observe solar proton or alpha f la re events; apparatus designed to measure protons of energies between 100 keV and 200 MeV; (2) orthogonal Geiger- ooimter telescope-array (GSFC), to study isotropy of solar events and cosmic-ray modulation and provide better understandmg of the mterplanetary magnetic f i e ld ; (3) particle telescope (GSFC), to obtam data on time variation of observed inter- planetary energetic electron fluxes beyond the Van Allen belt, (in order to obtain clues as to their or igm) , and to measure the energy spectrum of protons and other heavy particles; (4) Neher-type ion chamber and Geiger-counter tubes (Univ. Ca l . ) , m which ion chamber measured the total ionization per unit volume of stan- dard-density a i r as a function of t ime; Geiger-counter tubes detect fluxes of elec- trons of energy above 40 keV; (5) low-energy proton analyzer (Ames Research Center, NASA), to determme proton concentrations as a function of kinetic energy, in the range 200 eV to 20 keV, the highest energy level expected f r o m the solar-wind p ro - tons; (6) plasma probe (MIT) , to measure f lux of low-energy particles with velocities between 10 km/sec and 1000 km/sec, (7) thermal ion and electron experiment (GSFC), to measure concentration and temperatures of thermal electrons (energies 184

less than a few eV) and concentration, masses, and temperatures of thermal ions; (8) rubidium-vapor magnetometer (GSFC), to measure total magnetic-field mtensity mdependent of orientation; (9) fluxgate magnetometers (GSFC), to determme d i - rection of f ie lds . Tiros 10 (1965-51A) The second meteorological satellite of 1965, Tiros 10, was launched f r o m Cape Kennedy on July 2, 1965 to (1) produce observations of the atmosphere over the entire globe, (2) produce as complete and contmuous observations as scientif ically required and technically possible, and (3) provide maximum photographic mforma- tion on tropical s torms. Tiros 10, s imi la r to Ti ros 6 m that i t has two mdependent television systems moxmted m the base of the spacecraft, took pictures of about 60 to 80% of the Earth each day, which was about four times the coverage achieved with Tiros 6. The additional coverage was possible due to a combmation of a polar Sun- synchronous orbi t and a control system to change the satellite's attitude m space relative to the Ear th . This also permited a l imi ted amount of control in selecting specific areas of the Earth fo r observation. To get maximum photo coverage of the hurricane belt, the area where most tropical storms are born. Tiros 10 was programmed to be ver t ica l with the Earth at 20° north latitude. Usable pictures f o r meteorological purposes were taken f r o m the North Pole to 50° south latitude. A satellite in a perfect Sim-synchronous orbi t d r i f t s westward about 1° daily, the same direction and rate as the Earth moves around the Sun. The orbi ta l plane of the satellite always remains at a constant angle to the Earth-Sun Ime. Thus, Tiros 10 was in sunlight durmg each orb i t wi th the Sun being in the same relative position behind the satellite. This resulted in good i l lumination f o r photography. Additionally, because the solar cells are i n the same relative position to the Sun on each orb i t , the satellite's batteries remain f u l l y charged. ORS-3 (1965-58C) also ERS 17 See also Velas 3 & 4 (1964-40A and B ) . A 6-kg satellite, ORS-3 (1965-58C) was launched on July 20, 1965, and trans- mitted good data unt i l November 3, 1965. This satellite car r ied eight detectors that provided measurements of electrons wi th energies f r o m 40 keV to 3 MeV, protons f r o m energies f r o m 2 MeV to 35 MeV, solar X-rays around 8 A, cosmic gamma rays between 30 keV and 3 MeV and galactic cosmic rays. The orbi t covered the region of space f r o m 200 km altitude to 18.5 Earth r ad i i , the 185

equatorial mclmation was 3 4 . 4 ° and ecliptic mclmation was 5 8 ° . These data provided a complete samplmg of the radiation belts , the boundary region of the magnetosphere in the sunlit hemisphere , and X - r a y s and gamma rays m m t e r - planetary space. Aerospace R e s e a r c h Satellite O V l - 2 (1965-78A) O V l - 2 was mtended to perform a variety of radiation measurements . The satellite was launched from the Western Tes t Range on October 5, 1965, and op- erated sat isfactori ly . The satell ite and its propulsion module were ejective f ive mmutes after launch, then coasted to altitude of 890 km where the motor ignited to place O V l - 2 m retrograde orbit of 417 to 3480 km at 144° mclihation. A l l ex- periments operated sat is factori ly . Scientif ic mstrumentation mcluded proton and electron dosimeters and spectrometers . X - r a y detector, magnetometer and two tissue-equivalent ion chambers . Experiments were mounted m the cy lmdr ica l center section, spacecraft systems - telemetry, command, data storage and power supply - were located m domed ends. OGO 2 (1965-81A) The second m the s er i e s of orbitmg geophysical observatories and f i r s t with a polar orbit (Polar Orbitmg Geophysical Observatory or POGO) was launched on October 14, 1965. Its overal l design was like OGO 1; and like OGO 1, it c a r r i e d twenty experiments, most of which were relevant to the I Q S Y . These were: (1) Distribution of cosmic radio emission over the sky with sweep frequency rece iver (2 to 4 MHz) , Haddock, U . Michigan, (2) contmuous synoptic survey of V L F noise and propagation character i s t i c s (0.2 to 100 kHz) , Hel l iwel l , Stanford U . ; Rorden, Stanford R e s . I n s t . , (3) diurnal and latitude variations of V L F spectra m the range 0,5 to 10 k c / s . , Morgan and L a a s p e r e , Dartmouth College, (4) magnetic field fluctuations m the frequency range from 0,01 to 1000 H z , with search co i l magnetometers. Smith, J P L and Holzer , U C L A ; (5) World Magnetic Survey with rubidium-vapor and fluxgate magnetometers, at 10,000 to 65,000 gammas, Heppner and C a m , G S F C ; (6) monitormg of cosmic and trapped r a d i a - tion with ionization chamber, Anderson, J P L , and Neher, C I T , (7) study of low- energy protons and nucleons m cosmic and trapped radiation (from 0.3 to 30 MeV) with scmtiUation telescope, Simpson, Stone, and F a n , F e r m i I n s t , , U , Chicago, (8) energy spectrum and composition of galactic and so lar cosmic r a y s , as ob- served with a modified Cerenkov detector, Webber, U . Mmnesota, (9) net down- flux of corpuscular radiation m the aurora l zones and over the polar caps , with Geiger tubes as detectors, Van Allen and F r a n k , U . Iowa, (10) fluctuations m low-energy trapped radiation (electrons, 10-100 keV, protons, 100 keV to 4 .5 MeV) , with scintillation detector, Konradi , et a l , G S F C , (11) photometric a i r - glow measurements at 6300 A, 6200 A, 5890 A, 5577 A, 3914 A, and 2600 A, with photomultipliers and f i l t er s , Blamont, U . P a r i s , and R e e d , G S F C ; (12) airglow 186

measurements m the Lyman-alpha and the far ultraviolet between 1230 A and 1350 A, with ion chambers, Mange, et al, NRL; (13) airglow measurements, with ultraviolet spectrometer between 1100 Aand 3400 A, Barth, J P L , and Wallace, KPNO; (14) atmospheric neutral particle and ion composition (0-6 AMU and 0-40 amu), with Paul massenfliter mass spectrometer, Jones and Schaefer, U. Michigan; (15) atmospheric positive ion composition and density (1-6 amu and 7-45 amu), with Bennett RF ion mass spectrometer, Taylor and Brmton, GrSFC; (16) density of neutral atmospheric particles with Bayard-Alpert ioniza- tion gage, in pressure range from 10"^ to 10-10 mm Hg, Newton, GSFC; (17) (17) micrometeorites, Alexander, et al, GSFC; (18) electron temperature (800° to 3000''K), of ion or neutral gas temperature (800° to 3000°K) and charged particle density with a retarding-potential analyzer, Bourdeau, GSFC; (19) time varia- tions in solar x-ray emissions in the 0.5 - 3 A, 2 - 8 A, 8-16 A, and 44-60 A bands, with an ionization chamber, Kreplin, et al, NRL; and (20) monitoring of solar radiation (170-1700 A) in six ranges with six gratmg and photocathode combina- tions, Hinteregger, AFCRL. Explorer 30 (SOLRAD, 1965-93A) SOLRAD 1965-93A was launched by NASA as Explorer 30 in November 1965, and is the most sophisticated satellite in the SOLRAD series. It is equipped with a spm axis orientation system, a spm replenishment system, and a digital memory system as well as the analog real-time telemetry system. The detectors on board monitored solar radiation m the wavelength regions: 0.5-3, 1-8, 1-20, 8-16, 1080-1350, and 1225-1350 A. The two shorter-wavelength regions are monitored by Geiger counters as well as ion chambers. With the exception of the two ultra- violet chambers, which produce saturated signals at all times durmg periods of good aspect, the experiments are functionmg properly. A malfunction limited the usefulness of the memory system to about one month of data, but does not effect m any way the real-time data system. A failure of the spin replenishment system will eventually cause the satellite to begin a precessional motion similar to that of the earlier solar radiation satellites. The satellite is expected to provide useful data durmg periods of good aspect for 8-10 months. Durmg relatively quiet periods, variations in the 8-20 A region of approximately 50% were observed with a time scale of several mmutes, with no significant changes in the time scale of one second, which is the limit of resolution of the X-ray photometers. Data from these two SOLRAD satellites are currently bemg reduced and will be made available through the Institute for Telecommimication Sciences and Aeronomy of ESSA, Boulder, Colorado. Alouette 2 (1965-98A), and Explorer 31 (1965-98B) These two satellites, launched together on a smgle booster from the Western Test Range on November 28, 1965, mto nearly duplicate orbits of 520 to 2960 km and 80° mclinations, together form a system known as ISIS-X. The BIS 187

(International Satellite for Ionospheric Jtudies) program is a joint NASA/Canadian Defense Research Board undertaking. BIS continued the joint NASA/Canadian pro- gram begun with the Canadian satellite Alouette 1 by means of a series of ion- ospheric research satellites for performmg studies of the ionosphere from sunspot minimum through sunspot maximum. (Alouette 1 was still functionmg as of sprmg 1967). ISIS-X had as objectives both direct measurements m the upper atmosphere and topside soundmgs of the ionosphere. Alouette 2, the second Canadian-built space- craft, weighed about 130 kg, and the U.S. Explorer 31 weighed about 70 kg, these two constituted the complementary components of ISIS-X. The experiments on Alouette 2 were as follows: (1) topside soundmg, J . H . Meek, E . S . Warren, G . L . Nelms, Defence Research Telecommunications E s - tablishment, Canada, (2) measurement of energetic particles, D .C. Rose and I .B . McDiarmid, Canadian National Research Coimcil, (3) study of very low frequency (VLF) propagation, R . E . Harrington, Defence Research Telecommunications E s - tablishment, Canada; (4) cosmic radiofrequency noise, T .R . Hartz, Defence Re- search Telecommunications Establishment, Canada, and (5) electrostatic probe, L . H . Brace, GSFC. The experiments on Explorer 31 (Direct Measurements Explorer A or DME-A) were: (1) densities and temperatures of positive and negative ions with planar ion probe, Bourdeau and Donley, GSFC; (2) total current at a collector mounted flush with satellite skm, Bourdeau and Donley, GSFC; (3) electron density and tempera- ture with Langmuir probe, Brace, GSFC; (4) electron temperature usmg planar probe, A. P. Wilmore, University College, London, (5) ion temperature and den- sity with spherical ion mass spectrometer, R . L . Boyd and A, P. WiUmore, Uni- versity College, London, (6) particles in mass range, 1-32 amu, with high reso- lution magnetic mass spectrometer, Hoffman, NRL, and (7) energetic electron cur- rent monitor, Maier, GSFC. FR-1 (1965-lOlA) The French satellite FR-1 was launched on Dec. 6, 1965, by NASA as part of its mtemational cooperative program. The purpose of this spacecraft was to inves- tigate the propagation characteristics of V L F waves, with particular emphasis on the whistler mode, by performmg independent measurements of the electric and mag- netic field components of the waves, and determmmg at the same time the local electron density with a capacitance probe developed by an English group. Both natural signals and especially programmed ground transmissions were used m this mvestigation. 188

Pioneer 6 (1965-105A) The deep-space probe, Pioneer 6, was launched m the last weeks of the IQSY on December 16, 1965, into a heliocentric orbit. The spacecraft first reached its perihelion of 0.8143 a.u. approximately 155 days later and orbits the Sun with a period of 311.3 days. The objective of Pioneer 6 is to investigate the solar wind, interplanetary magnetic fields, and galactic cosmic rays and their modulation by the Sun. All experiments and spacecraft systems vital to the mission appear to be operating properly. The experiments carried by Pioneer 6 are as follows (magnetic fields 1; solar wind, 2-4; cosmic rays, 5 and 6): (1) single-axis flux- gate magnetometer (GSFC), to chart the strength and direction of the Sun's magnetic field from many locations in the plane of the Earth's orbit (the ecliptic); the magnetometer can sense field strengths from +64 gammas to -64 gammas, with a sensitivity of 1/4 gamma; (2) plasma cup detector (MIT), to measure the number, density, direction, and energy of positive ions and electrons m the solar wmd; the instrument measures electrons with energies of 500-2500 eV and protons of 40-10, 000 eV, at particle fluxes from 4 x 10^ to 4 x lO^cm^ sec; (3) quadri- spherical plasma analyser (Ames Research Center, NASA), to measure quan- tities, directions, energies, and temperatures, of solar-wmd particles; the ex- periment measures electrons with energies of 2-500 eV and positive ions with energies of 200-10,000 eV, at particle fluxes of 5 x 10"* to lO^/cm^ sec; (4) radio- progation detector (Stanford Univ. and Research Institute), to determine varia- tions in total electron content in the space between Pioneer and Earth; these inves- tigations will be useful m detectmg sudden mcreases m electron density resultmg from solar flares; (5) cosmic-ray anisotropy detector (Graduate Research Center of the Southwest), to measure the number, mass, energy, and directional charac- teristics of both solar and galactic cosmic rays; the energy range for protons is 7.5 to 90 MeV and for helium nuclei 130 to 360 MeV; (6) cosmic-ray telescope (Fermi Institute, Univ. Chicago), to measure solar and galactic cosmic rays; for galactic cosmic rays, variations of energy and composition of particles as the spacecraft moves near the Sun are of interest, as well as whether their distribu- tion changes as the Sun's activity increases dviring the current solar cycle; this experiment also attempts to determine numbers and energies of hydrogen and helium cosmic-ray particles in the energy range 10-200 MeV arriving from inter- stellar space, and it may provide clues concemmg interstellar forces that have accelerated them. 189

to o T A B L E 2 S U M M A R Y O F S O U N D I N G R O C K E T L A U N C H I N G S 1984 - 196S E x p e r i m e n t s • o 2 ^ i s •P h y si c s g- t Date T i m e R o c k e t N u m b e r o r S p o n s o r i n g 2 ^ 1 ^ I I l l - l " ^ a 1 A U i t u d A P r i n o E x p e r l m e n t e r ( s ) ( U T I (UT5 T y p e C o u n t r y L a u n c h i n g Si te % S ^ S I S S d o ( i i m , 6 I n s t l t u t l o n ( 8 ) 1964 8 Jan 1316 N A S A 1 4 . 1 2 9 l A Tnrt ln/IIRA I l m m b a V 177 P D S h a v s a r ^ d l a ) 1 2 Jan 0026 N A S A 14 130 l A I n d i a / U S A T h u m b s V ITO P 0 Shavsa r ( l n d l i 4 16 J a n 2240 N A S A 1 4 . 1 0 6 C A USA W a l l o p s I s l a n d V l i s J F B e d i n g e r ( G C A ) 16 Jan 0800 N A S A 14 126 CA USA W a l l o p s I s l a n d V 169 J F B e a n g e r ( G C A ) 18 Jan 1134 N A S A 14 126 CA USA W a l l o p s I s l a n d V 197 J F B e d i n g e r ( G C A ) 17 J a n 0601 N A S A 8 3 1 D A USA W a l l o p s I s l s n d X X X 946 J H H o f b n a n ( N R L ) 24 J a n 0016 N A S A 10 6 1 G A USA W a l l o p s I s l s n d G 128 W S S m i t h ( G S F Q 26 Jan 0814 N A S A 1 4 79 U E I n d i a / U S A T h u m b s X X 164 L . J C a U U ( U N e w H a m p s h i r e ) 27 Jan 0430 N A S A 14 80 U E I n d i a / U S A T h u m l i a X X 164 L . J C a h l U ( U N e w H a m p s h i r e ) 29 Jan 0411 N A S A 10 7 1 G A USA W a l l o p s I s l s n d G 114 W S S m i t h ( ( S F C ) 29 Jan 0417 N A S A 10 89 G A USA F o r t C h u r c h i l l G 123 W S S m i t h ( G S F Q 29 J a n 0418 N A S A 10 81 GA USA A s c e n s i o n I s l G 124 J S T h e o n ( G 8 F C ) 29 Jan 1100 N A S A 14 8 1 U E b u t i a / U S A T h u m b s X X 167 L . J C a U U ( U N e w H a m p s h i r e ) 3 1 J a n 1330 N A S A 14 82 U E I n d i a / U S A T h u m b a X X 167 L . J C a U U ( U N e w R a m p s U r e ) 4 F e b 0136 N A S A 14 22 U A USA A s c e n s i o n I s l I 168 J J Horva t fa ( U M i o U g a n ) 4 Feb 0146 N A S A 10 82 GA USA W a l l o p s I s l s n d G 116 W S S m i t h (GSFC) 6 F e b 0320 N A S A 10 63 G A USA W a l l o p s I s l s n d G 119 W S S m i t h (GSFC) 5 F e b 044O N A S A 10 87 G A USA F o r t C h u r c h i l l G 126 W S S m i t h (GSFC) 9 F e b 0417 A C 3 606 USA F o r t C h u r c h i l l X X 228 J U l w i c k ( A F C R L ) 13 F e b 0430 N A S A 10 88 G A USA F o r t C h u r c h i l l G 119 W S S m i t h (GSFC) 13 F e b 0430 N A S A 10 136 G A USA W a l l o p s I s l a n d 0 119 W S S m i t h (GSFC) 13 F e b 0486 N A S A 10 82 GA USA A s c e n s i o n I s l G 122 J S T h e o n (GSFC) 17 Feb 1000 N D 3 143 USA W h i t e Sands X 196 D M P a c k e r , o t h e r (NRI4 20 F e b 0723 N A S A 14 43 G E USA F o r t C h u r c h l U X X 204 D S E v a n s (GSFC) 27 F e b 0318 N A S A 4 124 U A USA F o r t C h u r c h i l l X 181 W G F a s t l e ( Johns H o p U n a ) 29 F e b 0633 N A S A 1 4 4 4 G E USA F o r t C h u r c h l U X X 204 D S E v a n s (CSFC) 7 M a r 0246 N A S A 10 137 G A USA W a l l o p s I s l a n d G 114 W S S m i t h ( G S F Q 1 1 M a r 1800 A C 6 342 USA E g l i n X X 108 R N a r c i s s i ( A F C R L ) 18 M a r 0811 N A S A 14 161 UE USA F o r t C h u r c h i l l X X 161 B J O ' B r i e n ( R i c e U ) 20 M a r 0623 N A S A 1 4 . 1 6 2 UE USA F o r t C h u r c h i l l X X 161 a J O ' B r i e n ( R i c e U ) 23 M a r 1037 N A S A 1 4 163 UE USA F o r t C h u r c h l U X X 153 B J O ' B r i e n ( R i c e U ) 24 M a r 0423 N A S A 1 4 118 GE USA F o r t C h u r c h l U X X 188 D 8 E v s n s (GSFC) 26 M a r 0330 N A S A 1 4 119 GE USA F o r t C h u r c U U X 194 D S E v a n s ( G S F Q 3 0 M a r 1900 A D 3 614 USA W h i t e Sands X 248 H . H n t e r e g g s r ( A F C R L ) 1 1 A p r 0630 N A S A 1 4 . 1 2 1 UE USA F o r t C h u r c h l U X 171 W M u r c r a y ( U A l a s k a ) S y m b o l s f o r T y p e o f Eaqperiment C — C h a f f - w i n d s D — D e n s i t y Gage - D e n s l f y G — ( i r e n a d e s - w l n d s , t e m p e r a t u r e , p r e s s u r e s n d d e n s i t y I — I n s t r u m e n t s o n r o c k e t - p r e s s u r e , t e m p e r a t u r e a n d d e n s i t y P — P a r a c h u t e a n d i n s t r u m e n t s - w i n d s , t e m p e r a t u r e a n d d e n s i t y S - F a l l i n g s p h e r e - w i n d s , t e m p e r a t u r e a n d d e n s i t y V — V s p o r t r a i l - w i n d s M — M o l e c u l a r o x y g e n d e t e r m i n a t i o n N — N o c t i l u c e n t c l o u d s O — O t o n e d e t e r m i n a U o n T — C l o u d p h o t o g r q ) ! ? X — O t h e r e x p e r i m e n t s

S U M M A R Y O F SOUNDING R O C K E T L A U N C H I N G S 1B84 - 1965 (continued) Date T i m e Rooket Number o r Sponsor ing o a (UT) (UT) Type Coun t ry Launch ing Site < 1984 15 A p r 0122 NASA 14. 24 UA USA Ascens ion I s l I 15 A p r 0840 NASA 14 .122 UE USA F o r t c l i u r c h l U 15 A p r 1658 NASA 14. 23 UA USA Ascens ion I s L I 16 A p r 2325 NASA 12 OSGT-QI USA W a l l o p s I s l a n d 16 A p r 2106 NASA 14.143 U I USA W a l l o p s I s l a n d 17 A p r 2315 NASA 10 142 UA USA W a l l o p s I s l a n d S 18 A p r 0039 NASA 10 73 OA USA F o r t C b i r c U U G 18 A p r 0069 NASA 10 83 GA USA W a l l o p s I s l a n d G 22 A p r 0854 NASA 14.123 UE USA F o r t C h u r c h i l l 18 M a y 0820 A E 6 479 USA Cape Kennedy 19 M a y 0845 A £ 6 481 USA Cape Kennedy 19 M a y 1800 A E 6 482 USA Cape Kennedy 10 J i m 0503 A £ 15. 373 USA St. Nicho las I s l S 10 Jun 1610 NASA 14.156 GE USA W a l l o p s I s l a n d 16 Jun 0900 N B 3 147 USA W U t e Sands 25 Jun 1468 NASA 14.156 GE USA W a l l o p s I s l a n d 28 Jon 0063 NASA 14.157 (3E USA W a l l o p s I s l a n d 7 J u l 2242 N B 3 184 USA Whi t e Sands 9 J u l 0413 NASA 14 164 UE USA W a l l o p s I s l a n d 15 J u l 0068 NASA 14. 49 CA USA Wal lops I s l a n d V 15 J u l 0409 NASA 14. 50 CA USA W a l l o p s I s l a n d V 16 J u l 0800 NASA 14 .144 U I USA W a l l o p s I s l a n d 15 J u l 0806 NASA 14. 61 CA USA W a l l o p s I s l a n d V 15 J u l 0906 NASA 14. 52 CA USA W a l l o p s I s l a n d V 16 J u l 0920 NASA 14 .146 U I USA W a l l o p s I s l a n d 15 J u l 1025 NASA 14.146 U I USA W a l l o p s I s l a n d 16 J u l 1822 NASA 14.127 a USA W a l l o p s I s l a n d 18 J i l l 1322 A C 16 383 USA F o r t C h u r c h i U 23 J u l 1843 NASA 4 .107 GE USA F o r t C h u r c h i l l 26 J u l 1735 NASA 4 . 1 0 8 GE USA F o r t C h u r c h i U 28 J u l 2114 NASA 6 10 GA USA F o r t C h u r c h i U I 7 A u g 0016 NASA 10 138 GA Sweden A J S A K r o n e g a r d G 7 A u g 0100 NASA 10 78 OA USA W a l l o p s I s l a n d G 8 A u g 0400 NASA 10 104 GA USA F o r t C h u r c h i l l G 12 A u g 0149 NASA 10 84 OA USA W a l l o p s I s l a n d G 12 A u g 0216 NASA 10 106 GA USA F o r t C h u r c h i U G 16 A u g 0113 NASA 10 140 GA SwedenAlBA K r o n o g a r d G 16 A u g 0315 NASA 10 86 GA USA W a l l o p s I s l a n d G 16 A u g 0563 NASA 10 115 GA USA Ascens ion I s l G 17 A u g 0049 NASA 10 141 OA SwedmAJSA K r o n o g a r d G 17 A u g 1256 NASA 10 116 GA I B A Asoens lon I s l G 18 A u g 0115 NASA 10 106 GA USA F o r t C h u r c h i U G E x p e r i m e n t s i l — -3 1 ^ 4 I f 5 < p< s A l t i t u d e (tan) 168 164 158 729 169 150 127 128 168 152 150 190 251 146 121 149 188 216 187 190 192 166 192 192 180 171 137 208 233 216 322 130 118 139 116 126 136 122 124 129 122 125 P r i n c E]q>er imenter (s ) & Ins t l t u t lon ( s ) J J H o r r a t h ( U . M i c h i g a n ) W M u r c r a y (U Alaska ) J J H o r v a t h (U M i c h . ) J L Donley , L H B r a c e (GSFC) GCA, U U l i n o l B W a Hansen (U Mich igan ) SEC, T e x West . OoU SEC, Tex W e s t CoU W M u r c r a y (U Alaska ) N W Rosenberg ( A F C R L ) N W Rosenberg ( A F C R L ) N W Rosenbe rg ( A F C R L ) F Fauoher ( A F C R L ) T N Oavls (CSFC) E T B r y a m ( N R L ) D a v i s (GSFC) Davis (GSFC) B r y a m ( N R L ) O ' B r i e n (Rice U ) Bedinger (GCA) Bedlnger (GCA) B o w h l l l ( U n i i n o l s ) , J Wager B i r m i n g h a m , Eng l ) I . G S m i t h (GCA) Bedinger (CCA) Bedlnger (GCA) B o w U U (U l U i n o l s ) , L . G Smi th (GCA) S A B o w U l K U n i i n o l s ) , L . G S m i t h ( G C A ) R G Stone, J K A l e x a n d e r (GSFC) S S i l v e r m a n ( A F C R L ) C E Flcfate l (GSFC) F t o h t e l (GSFC) C a n g c a n (U M i c h i g a n ) Smi th (GSFC), G W i t t (U Stockholm) S m i t h (GSFC), SEC S m i t h (GSFC) S m i t h (GSFC) , SEC a n i t h (GSFC) W S S m i t h (GSFC), G W i t t W S S m i t h ( G S F O , G W i t t J S Theon ( G S F O W 8 S m i t h , G W i t t (GSFC) J S Theon ( G S F O W S S m i t h ( G S F O T N T N E T B J J F J F S A (U J F J F S A C E G R W S W S W S W S W S

S U M M A R Y OF SOUNDING R O C K E T L A U N C H I N G 1964 - 1965 (contl imed) E x p e r i m e n t s Date T i m e Rocket Number o r Sponsor ing » s •t m os lo m p 3n o 'h y sl cs P a rt ic le s & F lo ld s A lr g lo w b A u ro ra o la r P h y si cs > th er ( te st ) A l U b d e P r i n c E x p e r i m e n t e r ( B ) (UT) (UT) Type Coun t ry Launching Site < Q, u P a rt ic le s & F lo ld s A lr g lo w b A u ro ra ai (km) & Ins t i tu t ion(s ) 1964 18 Aug 0125 NASA 10 113 GA USA Wal lops I s l and G 120 W S. Smi th (GSFC) 26 Aug 1601 NASA 14 34 G I USA Wal lops I s l and X X X 153 S. J Baue r , R E Bourdeau (GSFC) 18 Sept 1717 NASA 4 115 NA USA Wal lops I s land X X 168 C A . B a r t h ( J P L ) (Ea r th ' s albedo) 26 Sept 1204 NASA 4 13 G P - G T USA Wal lops I s l and X X X 120 J R. Busse (GSFC), T Donahue (U P i t t sburgh) 7 Oct 2304 NASA 14 195 CA USA Wal lops I s l and V X 172 i F B e d i n g e r , L G Smi th (GCA) 8 Oct 0532 NASA 8 03 CA USA Wal lops I s land X X 1004 G Sharp (Lockheed) 8 Oct 1023 NASA 14 194 CA USA Wal lops I s land V X 1S9 J F Bed inge r , L G Smi th (GCA) 8 Oct 1034 NASA 14 159 GE USA Wal lops I s land X 140 T N D a v i s (GSFC) 17 Oct 1043 A E 5 487 USA E g l m V 156 N W Rosenberg ( A F C R L ) 23 Oct 1600 NASA 8 33 GR USA Wal lops I s land X l lOO a.R. Weber , J K. Alexander (GSFC) 24 Oct 0433 S K O L 154-30 USA Bar tung Sands V 160 L . B , Smi th 27 Oct 0725 S K O L 154-31 USA B a r k i n g Sands V 160 L . B . S m i t h 27 Oct 1657 A B 6 197 USA F o r t C h u r c h i l l X 100 J U l w l c k ( A F C R L ) 27 Oct 1657 AC 17 606 USA F o r t C h u r c h U l X 148 J U l w i c k ( A F C R L ) 30 Oct 1930 NASA 4 116 GS USA White Sands X X 189 W S. Muuey (GSFC) 1 Nov 0600 NASA 14 197 CA USA F o r t C h u r c h i l l V X 1 F Bed inge r , K G Smi th (GCA) 1 Nov 0615 S K O L 154-32 USA B a r k i n g Sands S 140 L . B . S m i t h 1 Nov 0618 S K O L 154-34 USA B a r k i n g Sands V 160 L . B . S m i t h 3 Nov 0432 S K O L 154-36 USA B a r k i n g Sands V 160 L . B . S m i t h 3 Nov 1002 A E 5 550 USA E g l m X X 153 M Smiddy , A . F a i r e ( A F C R L ) 3 Nov 1738 NASA 10 132 GA USA Wal lops I s land G 123 J S. Theon (GSFC) 5 Nov 1700 NASA 10 107 GA USA Wal lops I s l and G 123 J a Theon (GSFC) 5 Nov 1903 NASA 8 34 UA USA Wal lops I s land X 884 W Fas t i e (Johns Hopkins) 5 Nov 2038 NASA 14 104 D I USA F o r t C h u r c h i l l X H . Zancanata , J Conley ( B R L ) 5 Nov 2039 NASA 8 19 D I USA F o r t C h u r c h i l l X X 840 H Zancanata , J Conley ( B R L ) , A Nagy (U M i c h . ) 6 Nov 0002 NASA 10 133 GA USA Wal lops I s land G 120 J S. T h e o n (GSFC) 6 Nov 0008 NASA 14 1 3 1 I A I n d i a / F r / U S T h u m b a V 192 K. R. M e d r o w (GSFC) V A Sarabhai (India) 6 Nov 0520 NASA 10 134 GA USA Wal lops I s l and G 121 J S. Theon (GSFC) 6 Nov 1000 NASA 10 135 GA USA Wal lops I s l and G 125 J S. Theon (GSFC) 7 Nov 0513 NASA 14 105 D I USA F o r t C h u r c h i l l X 134 H . Zancanata , J Conley (BRL) 7 Nov 0514 NASA 8 20 D I USA F o r t C h u r c h i l l X X 715 H . Zancanata , J Conley ( B R L ) , A Nagy (D M l c U g a n ) 9 Nov 1254 NASA 14 204 l A I n d l a / F r / U S Thumba V 192 K- R. M e d r o w (GSFC), V A. Sarabhai (India) 10 Nov 0005 NASA 14 205 l A I n d l a / F r / U S Thumba V 192 K . R . M e d r o w (GSFC), V A. Sarabhai (India) 10 Nov 1107 NASA 14. 147 U l USA Wal lops I s l and X X 117 E G S m U h , S. A B o w h l l l (U I l l i n o i s ) 10 Nov 2225 NASA 14 114 GA USA 36 ' 1 0 ' N 7 4 ' 4 3 ' W V J F B e d i n g e r , (GCA) 10 Nov 2228 NASA 14 53 CA USA Wal lops I s l and V 197 J F B e d i n g e r , (GCA) 10 Nov 2326 A E 5 551 USA E g l m X X M . Smiddy , A F a i r e ( A F C R L ) 11 Nov 0119 A E 5 552 USA EgUn X X M . Smiddy ( A F C R L ) 11 Nov 2224 NASA 14 115 CA USA 3 4 » 2 7 ' N 7 4 * 4 0 ' W V J F Bed inger (GCA) 11 Nov 2227 NASA 14 112 CA USA Wal lops I s land V 197 J F Bed inger (GCA)

S U M M A R Y O F SOUNDINO R O C K E T L A U N C H I N O 1S64 - 1866 (contl imed) Date (UT) T i m e (UT) Boctaat Number o r T^rpe Sponsoring Coun t ry i j u n r h l T i g Site E x p e r i m e n t s A l t i t u d e (km) Pr i t t c E x p e r i m e n t e r ( s ) b iDst t tuUon(s) A tm o s P h y si cs A tm o s C om p lo n o P h y si cs P a rt ic le s b F ie ld s A ir g lo w 6 A u ro ra S o la r P h y si cs o th e r (t es t) 1 3 M 12 Nov 1053 NASA 14.116 C A USA 33* SS'NTe* 16'W V — J F Bedinger (OCA) 12 Nov 1830 NE 3 155 USA Whi te Sands X 188 J D P u r c e l l , D L . O a r r e t t ( N R L ) 16 Nov 1818 NASA 4. 45 OA USA Wal lops I s l a n d X X X 188 0 R C a r i g n a n (U M i c h i g a n ) 17 Nov 174S NASA 14. 233 U A USA 3 7 ' 4 5 ' N 7 6 " 2 2 ' W X 218 W U Hansen ( D . M i c h i g a n ) IT Nov 2110 NASA 10 163 U A USA 3 7 ' 4 7 ' N 7 8 ' 2 0 ' W X 148 W a Hansen ( U . M I o U g a n ) IS Nov IT 15 NE 3 1 6 4 R USA Whi t e Sands X 218 J D P u r o e l l , o the r s (NRI4 IS Nov 1802 NASA 10 117 O A USA Wal lops I s l a n d 0 125 W S. S m i t h (OSFC) IS Nov 2020 NASA 14. 148 U I USA Wal lops I s l and X 165 L . 0 S m i t h (OCA) , S. A . B o w h i l l (U n i l n o i a ) 18 Nov 2202 NASA 14.148 U I USA S r 45 'N75*22 'W X 188 1 . 0 S m i t h (OCA) , & A . B o w h i l l (U m i n o l a ) 22 Nov 1630 A D 6 811 USA E g l i n X 80 R H a r v e y ( A F C R L ) 23 Nov 1707 NASA 14. 117 0 1 USA Wal lops I s l and X X X 178 J L . Donley , o the r s (OSFC) 25 Nov 11S4 N E 3 161 USA Whi te Sands 2 0 1 E T B r y a m (NRL) 27 Nov 1331 A E 7 312 USA EgUn X 165 C P H o u l t , ( A F C R L ) 30 Nov 1311 NASA 14. 135 l A P a l d s t a n / F r / USA Sonzniani V 200 S M e h m u d (Pakis tan) I D e o 0120 NASA 14. 138 U I F a i d s t a n / F r / flnnwinnj V 200 8. M e h m u d (Pakis tan) I D e o 0616 NASA 4. 83 OA USA Whi t e Sands X 182 J P Hennes (OSFC) l O e o 1620 ION 1-64-1 A r g / U S A C h e m i c a l X X 134 S. RadioeUa (Argent ine) I D e o 1806 I O N 1-64-2 A r g / U S A C h a m l c a l X X 137 S. RadioeUa (Argen t ine ) 16 Deo 1430 NASA 4 .122 OA USA Whi t e Sands X 202 0 E B e r g , E C Whipp le (OSFC) 16 Deo 1457 NASA 14.208 0 1 USA Whi te Sands X 185 A . C A i k l n , E C Whipp le (OSFC) I T Deo 0688 NASA 4 .125 U A USA Whi t e Sands X 236 W 0 F a s t i e (John Ho^ddns), C A . B e r t h ( J P L ) 1866 7 Jan 0360 NASA 14. 142 N A USA Wal lops I s l a n d s X 147 A E Po t t e r ( L e w i s Res Cen te r ) 12 Jan 1068 J D - 1 1 . 0 8 I n d i a / U S A T h u m b a c 77 M & V Rao (India) IS Jan 1016 J D - I L OS Ind ia /USA T h u m b a c 77 M S. V Rao ( b d l a ) IS Jan 2348 NASA 4. I l l NA USA Wal lops I s l a n d X 178 C A . B a r t h ( J P L ) 2 1 Jan 2030 N A 3 183 USA Whi t e Sands X X 226 D P M o N u t t (NRL) 27 Jan 2132 NASA 10 124 O A USA Po in t B a r r o w 0 J & Theon (GSFC) 27 Jan 2224 NASA 10 118 OA USA Wal lops I s l a n d 0 118 W S. S m i t h (GSFC) 27 Jan 2324 NASA 10 121 OA USA F o r t C h u r c h i l l G 125 W a. S m i t h (OSFC) 3 Feb 1808 NASA 14. 6 1 U E USA Wal lops I s l a n d X X X 141 J A . Lookwood , o the r s (U N H a m p s h i r e ) 4 Feb 0445 NASA 10 126 OA USA Po in t B a r r o w O 121 J & Theon (OSFC) 4 Feb 0510 NASA 10 118 OA USA Wal lops I s l a n d 0 118 W & S m i t h (OSFC) 4 Feb 1735 NASA 10 122 O A USA F o r t C h u r c h i l l 0 W 8 S m i t h (GSFC) 8 Feb 2 2 U NASA 10 128 OA USA Poin t B a r r o w 0 124 J & Theon (OSFC) 8 Feb 2263 NASA 10 120 O A USA Wal lops I s l a n d 0 107 W 8. S m i t h (OSFC) 6 Feb 2300 NASA 10 123 OA USA F o r t C h u r c h i l l 0 121 W S. S m i t h (OSFC) CO

CO Z-te (UT) 1965 1 1 Fob 18 Feb 19 Feb 19 Feb 19 Feb 27 Feb 27 Feb 27 Feb 128 Feb 28 Feb 28 Feb 28 Feb 28 Feb S M a r 3 M a r 4 M a r 6 M a r 8 M a r S M a r 9 M a r 9 M a r 10 M a r 11 M a r 11 M a r 11 M a r 12 M a r 12 M a r 13 M a r 16 M a r 16 M a r 17 M a r 18 M a r 18 M a r 18 M a r 18 M a r 19 M a r | 2 0 M a r S U M M A R Y O F SOUNDING R O C K E T L A U N C H I N G 1964 - 1965 (contlmied) T i m e (UT) 1756 2009 0025 0451 0918 2100 2133 2230 0021 0415 0915 1130 1130 0009 1416 1411 0732 1536 174S 0626 1625 1600 0935 1038 2007 1330 1600 0742 1615 1662 1510 0604 0641 1601 1638 1809 0542 Rockot Number o r Typo A E 3 153 NASA 14. 11 U A A E 5 492 NASA 4. 129 UA NASA 14. 95 U A A E 5 556 NASA 10 155 UA A E 5 486 NASA 14. 196 C A A E 5 494 A E 6 653 A E 5 496 A E 5 497 A E 3 516 A E 3 617 A E 3 518 A E 3 613 NASA 14. 160 GE NASA 14. 64 U A NASA 14. 65 UA NASA 14. 85 U E NASA 14. 83 UE NASA 14. 98 UA N A 4 A 10 166 U A NASA 14. 99 U A NASA 14. 07 U E NASA 14 .84 U E A D 3 612 NASA 14. 171 G E NASA 14. 177 0 1 NASA 4. 63 GS NASA 14. 172 GE NASA 14. 178 G I NASA 14. 176 GE NASA 14. 179 G I NASA 12 05 OA NASA 6 1 1 O A Sponsor ing Coun t ry Launch ing Site USA USA USA USA USA USA USA USA USA USA USA USA USA USA USA USA USA USA USA USA USA USA USA USA USA USA USA USA USA USA USA USA USA USA USA USA USA Whi t e Sands F o r t C h u r c h l U E g l i n F o r t C h u r c l i l U F o r t C h u r c h l U E g l i n S7» 47'N79" 2 3 ' W E g l i n F o r t C h u r c h U l E g l i n E g l i n E g l i n E g l i n Whi te Sands Whi t e Sands Whi te Sands F a r t C h u r c h i l l 0 ' 0 1 ' N 8 4 ' 1 9 ' W 0 0 ' 0 1 ' N 8 4 ' 0 8 ' W 0 - S 2 ' S 8 4 ° 0 9 ' W 3-07 'S84*22'W e-30 'S84'32 'W 9 ' 2 7 ' S 8 2 ' 2 6 ' W 9 '36 'S82-21 'W 9P 32'S84' 14 'W 11*23'S81-25'W 1 1 ' 2 5 ' S 8 1 ' 2 0 ' W F o r t C h u r c h l U I 2 M 7 ' S 7 8 ' 3 ' W 12*49'S78-15 'W/ | Whi te Sands 12 '47 'S77 ' 58 'W 12'48'S77- 5 6 ' W 1 2 ' 4 7 ' S 7 8 ' 0 0 ' W 12'47'S77* 5 0 ' W WaUops I s l a n d WaUops I s l a n d E x p e r i m e n t s I f Ifi S s V G V s GV GV X X X X X X X X X X A l t i t u d e (km) 161 150 187 157 132 170 145 143 139 2 4 1 252 245 193 162 184 P r l n c E x p e r i m e n t e r ( 8 ) b Ins t l t u t lon ( s ) A . J u r s a ( A F C R L ) E J Schaefer (U m c U i ^ ) N W Rosenberg ( A F C R L ) W O Fas t l e (John H o p k i n s ) , C A . B e r t h ( J P L ) E J Schaefer (U M l c U ^ ) A . F a i r e ( A F C R L ) W H Hanson (U M i c h i g a n ) J U l w i c k ( A F C R L ) L . G S m i t h , J F Bed inge r (GCA) N W Rosenberg ( A F C R L ) J U l w i c k ( A F C R L ) N W Rosenberg ( A F C R L ) N W Rosenberg ( A F C R L ) H . E H i n t e r e g g e r ( A F C R L ) H E H in t e r egge r ( A F C R L ) H E H i n t e r e g g e r ( A F C R L ) J U l w i c k ( A F C R L ) T N D a v i s , J P Heppner (GSFC) J J H o r v a t h (U M i c h i g a n ) J J H o r v a t h (U H l o U g a n ) L . J C a h l U (U N H a m p s h i r e ) ! l . J C a h U l ( U N H a m p s h i r e ) E J Schaefer l(U^ m ^ l g m ) W H Hansen[(U m o U ^ ) E J Schaefer (U M i c h i g a n ) I . J C a h l U (U N H a m p s h i r e ) L . J C a h l U (U N H a m p s h i r e ) J U l w i c k ( A F C R L ) T N D a v U . J P Heppner (GSFC) A . C A i k e n , L . J B l u m l e (GSFC) W W Munsy (GSFC) T N D a v i s , J P Heppner (GSFC) A . C A l k i n , I . J B l u m l e (GSFC) T N D a v i s , J P Heppner (GSFC) A . C A l k l n , L J B l u m l e (GSFC) G B . Car ignan | (U* I f l l o U g a n ) G R. C a r l g n a n ; ( U . M i o U g a n )

S U M M A R Y OF SOUNDING R O C K E T L A U N C H I N G 1964 - 1965 (continued) Date (UT) T i m e (UT) 1965 20 M a r 20 M a r 20 M a r 21 M a r 22 M a r 22 M a r 24 M a r 24 M a r 25 M a r 26 M a r 26 M a r 27 M a r 27 M a r 28 M a r 29 M a r 30 M a r 1 A p r 2 A p r 3 A p r 4 A p r 5 A p r 5 A p r 6 A p r 9 A p r 9 A p r 12 A p r 12 A p r 12 A p r 13 A p r 13 A p r 13 A p r 15 A p r 15 A p r 20 A p r 1320 1628 1704 0645 0744 0849 1624 1707 1600 1541 1613 0301 1808 1550 1547 0550 0207 1321 0638 1606 1346 1942 1634 1918 2026 1448 1714 1937 0405 1600 1710 1045 1600 1540 Rocket Number o r Type 20 A p r 2204 NASA 14 228 U I A E 5 293 A E 6 252 NASA 15 02 G l A E 5 294 A E 6 253 NASA 14 174 GE NASA 14 180 G I AE 5 295 NASA 14 173 GE NASA 14 181 G l NASA 14 182 G I NASA 14 175 GE A E 5 296 NASA 14 70 GE ND 3 159 NASA 14 132 NA NASA 14 185 UE NASA 14 207 UE NASA 14 66 UA NASA 14 230 U I NASA 14 184 UE NASA 14 26 UA NASA 14 231 U I NASA 14 63 UA NASA 4 49 OS NASA 14 232 U I A E 7 313 NASA 14 67 UA NASA 14 27 UA NASA 14 186 UE NASA 4 127 UA NASA 14 25 UA NE 3 156 AO 6 841 ExperlmenlB Sponsoring Count ry Launching Site ID USA USA USA N o r w a y / U S A USA USA USA USA USA USA USA USA USA USA USA USA USA USA USA USA USA USA USA USA USA USA USA USA USA USA USA USA USA USA USA 12'00 'S78'00 'W 12-55'S7e'00iW i r 5 7 ' S 7 7 * 5 8 ' W Andoya 12'54'S77*54'W 12'57'S77'50'W 11-24'S78*25'W 11'24'S78'25'W 9'10'S80*00'W 10*10'S79*30'W 10*10'S79*27'W 1 2 ' l l ' S 7 8 ' 4 5 i W 14-10'S77'57'W 15*59'S77*59'W 12 '07 'S78n3 'W White Sands Wal lops I s land 12*07'S78'13'W F o r t C h u r c h i l l 2 4 ' 0 5 ' S 7 6 ° 0 8 ' W 29*34'S75-13'W 3 0 ' 3 8 ' S 7 5 ° 0 2 ' W 35°14 'S74°15 'W 4 4 ' 1 5 ' S 7 5 ° 4 0 ' W 44 '23 'S77M7'W White Sands 58 ' 19'S78'00'W EgUn 60°00 'S78*00 'W 0 0 ' 0 0 ' S 7 8 ° 0 0 ' W 60*00'S78''00'W Whi le Sands 52°35 'S78*20 'W White Sands Wal lops I s land ^ 3 < < A l t i t u d e (km) 201 122 76 206 120 217 139 200 143 198 201 80 P r i n c E x p e r i m e n t e r ( s ) & Ins t l tu t ion(s ) S A B o w h l l l (U I l l i n o i s ) , L 0 Smith (GCA) B Shuman ( A F C R L ) M Smiddy ( A F C R L ) J A Kane (GSFC) B Shuman ( A F C R L ) M Smiddy ( A F C R L ) A C A l k i n , L J B k i m l e (GSFC) A C A l k i n , L J B h i m l e (GSFC) B Shuman ( A F C R L ) T N D a v i s , J P Heppner (GSFC) A C A l k i n , L J B l u m l e (GSFC) A C A l k i n , L J B l u m l e (GSFC) T N Davis J P Heppner (GSFC) B Shuman ( A F C R L ) T N D a v i s , J P Heppner (GSFC) D M P a c k e r , I S GuUedge ( N R L ) A E Po t te r ( L e w i s Res Center ) R E Hous ton , J A Lockwood (U N H a m p s h i r e ) B J O ' B r i e n (Rice U ) J J Horva th (U Mich igan) S A B o w h i U (U I l l i n o i s ) , L G S m i t h (GCA) R E Hous ton , J A Lockwood (U N H a m p s h i r e ) J J Horva th (U Mich igan) S A B o H k l l l (U I l l i n o i s ) , L G Smi th (GCA) J J Horva th (U Mich igan) B o w h i U (U Hous ton , J Horva th (U B o w h l l l (U Horva th (U K Fredga (GSFC) S A B o w h l l l (U I l l l n o l a ) C Houl t ( A F C R L ) J J Horva th (U Mich igan) J J Horva th (U J A Lockwood , A O C N i e r (U J J Horva th <U W E A u s t i n , D J D P u r c e l l (NRL) C E l l i s ( A F C R L ) L G Smi th (GCA) Mich igan ) R E Houston (U N H a m p s h i r e ) Minnesote) Mich igan) L G a r r e t t , (C B ) S m d e r ,

CO <3) S U M M A R Y O F SOUNDING R O C K E T L A U N C H I N G 1964 - 1965 (continued) Date (UT) T i m e (UT) Rocket Number o r Type Sponsor ing Coun t ry T a i^nf'hfwg Site Expc r i m e n t s A l t i t u d e (km) 1 A tm oi , P h y si cs A tm os c O lo no P h y si cs a ^ .2 •§ » u _o - — "bc B - n. s) < A u ro ra S o la r P h y si cs O th er ( te st ) P r l n c Exper imenter (5) & Ins t l tuUon(s ) 1965 23 A p r 0301 NASA 10 171 NA USA Wal lops I s l and V 128 R A . H o r d , H B T o l e f s o n (Langley Res Cent ) 23 A p r 0402 NASA 14 255 NA USA Wal lops I s l and V 145 R A H o r d , H B T o l e f s o n (Langley Res Cent ) 29 A p r 1732 NASA 10 94 l A P a k i s t a n / U S A / A K SonmJani G — Pakis tan Space & Upper A t m Res C o m m . 30 A p r 1857 Rehbar 8 P a k i s t a n / U S A / A K Sonmlani G Pak i s t an Space & Upper A t m Res C o m m 5 May 0323 NASA 4 89 GG USA Wal lops I s l and 145 D U W r i g h t , A Boggess (GSFC) 19 May 2011 NASA 8 29 U I USA Wal lops I s l and X 947 J S Nisbe t (Perm State) , 0 K i n g (Space C r a f t , Inc ) 22 May 0202 NASA 14 47 UA USA Ascens ion I s l I 158 J J Horvatfa (U Mlctalgao) 22 May 1400 NASA 14 48 UA USA Ascens ion I s l I 158 J J Horvatfa (U M i c U g B n ) 25 May 2320 A O 13 815 USA E g l i n X 488 R H a r v e y ( A F C R L ) 25 May 1959 NASA 15 18 G I New Zea l and / Cape K a r i k a r l X 88 A C A l k l n , J A Kane (GSFC) USA 26 May 0320 A D 13 812 USA E g l i n X 488 R H a r v e y ( A F C R L ) 30 May 1900 NASA 15 05 G I New Zea l and / Cape K a r i k a r l X 88 A C A l k l n , J A Kane (GSFC) USA 30 May 1920 NASA 15 06 G I New Zea l and / Cape K a r i k a r l X 88 A C A l k l n , J A Kans (GSFC) USA 30 May 1940 NASA 15 07 G I New Z e a l a n d / Cape K a r i k a r l X 88 A C A l k l n , J A Kane (GSFC) USA 30 M a y 2000 NASA 15 08 G I New Z e a l a n d / Cape K a r i k a r l X 88 A C A l k l n , J A Kane (GSFC) USA 30 May 2020 NASA 15 09 G I New Z e a l a n d / Cape K a r i k a r l X 88 A C A i U n , J A Kane (GSFC) USA 30 May 2100 NASA 15 10 G I New Z e a l a n d / Cape K a r i k a r l X 88 A C A l k d n , J A Kane (GSFC) USA 2 Jun 1020 A O 6 580 USA E g l i n V X 121 N Rosenberg ( A F C R L ) 2 Jun 1030 A E 6 498 USA E g l i n V X 121 N Rosenberg ( A F C R L ) 14 Jun 0913 NASA 14 245 U I USA Wal lops I s l and X 177 L G Smi th ( G C A ) , S A B o w h l l l (U I l l i n o i s ) 17 Jun 2107 NASA 4 140 GE USA F o r t C h u r c h i l l X 233 C E F i c h t e l , o the r s (GSFC) 17 Jun 2141 NASA 14 246 U I USA Wal lops I s l and X 177 L G Smi th ( G C A ) , S A BowhlU (U I l l i n o i s ) 23 Jun 0103 NASA 14 72 C M USA Wal lops I s land V 190 J F Bedinger (GCA) 23 Jun 0159 NASA 14 71 C M USA Wal lops I s l and V 204 J F Bedinger (GCA) 23 Jun 0400 NASA 14 201 CA USA Wal lops I s land V X 164 L G S m i t h , J F Bedinger (GCA) 23 Jun 0847 NASA 14 73 C M USA WaUops I s land V 196 J F Bedinger (GCA) 23 Jun 0852 NASA 14 74 C M USA Wal lops I s land V 143 I F Bed inger (GCA)

S U M M A R Y O F SOUNDING R O C K E T L A U N C H I N O 1864 - 1865 (continued) Data (UT) T i m e (UT) 1865 23 J u n 28 Jun 30 Jun T J u l IS J u l 21 J u l 21 J u l 21 J u l 23 J u l T A u g 7 Aug 7 A u g 7 Aug 7 A u g 7 A u g 8 A u g 8 Aug 8 A u g 8 Aug 8 Aug 8 A u g 8 A u g 9 Aug 12 A u g 24 A u g 26 A u g 1 Sept 9 Sept 1546 1800 0533 0825 2050 0250 1033 2000 1705 1114 1200 1830 1840 184S 2006 0340 0400 0415 0840 1002 1015 1010 1112 1715 2159 1803 1117 2358 15 Sept 2028 16 Sept 3305 17 Sept 1544 I T Sept 2161 20 Sept 1608 22 Sept 1007 23 Sept 1436 24 Sept 0400 25 Sept 2164 Rocket Number o r Type NASA 4 141 GE NASA 4 112 NA NASA 11 03 UR A E 3 117 NASA 4.128 UA J D - 1 4 A E 7 347 A E 3 3TS NASA 10 128 G M NASA 10 151 O M NASA 10 96 G M NASA 10 154 U A NASA 10 162 O M NASA 10 165 O M NASA 10 168 G M NASA 10 169 G M NASA 10 166 G M NASA 10 163 G M NASA 10 15T U A NASA 10 167 O M NASA 10 170 G M NASA 10 164 O M NASA 10 151 G M A F 3 519 NASA 14 210 0 1 A E 3 614 NASA 14 213 U I NASA 14 TS OR NASA 14 244 U I A E 18 315 NASA 14 235 UE NASA 4 .138 n NASA 14 236 UE NASA 4.14T CG NASA 8 38 G I A D S T22 NASA 4 .139 n Sponsor ing Coun t ry T s u n r h i n g Site E x p e r i m e n t s A l U h l d e (km) P r l n c E x p e r l m e n t e r ( s ) ft Ins t i tuUon(a) A tm o s P h y si cs A tm o s C om p lo no I% y 6 lc s P a rt ic le s b F ie ld s A ir g lo w 6 A u ro ra S o la r P h y si cs o th e r (t es t) USA F o r t C h u r c h i l l X 214 C E F i c h t e l , o t h e r s (GSFC) USA Whi te Sands X 195 C A . B a r t h , J B Pearce ( J P L ) USA Wal lops I s l and X X 1770 W J L indsay (GSFC) USA F o r t C h u r c h i l l N 166 R Soherman ( A F C R L ) USA Whi te Sands X 196 A D C N i e r (U Ulnneso t e ) I n d i a A ' S A Thumba C 77 M S V Rao (India) USA E g l i n S X 179 G Faucher ( A F C R L ) USA White Sands X 193 R N a r c l s i ( A F C R L ) USA Wal lops I s l and GS 116 W S Smi th (GSFC) USA P o i n t B a r r o w G 120 W S Smi th (GSFC) USA F o r t C h u r c h i l l G 113 W S Smi th (OSFC) USA Wal lops I s l a n d S 166 J W P e t e r s o n ( U . M l o b l g a n ) USA P o i n t B a r r o w G 127 W S Smi th (GSFC) USA F o r t C h u r c h i l l G 108 W S Smi th (GSFC) USA Wal lops I s l and G 120 W S Smi th (GSFC) USA Wal lops I s l s n d G 122 W S S m i t h (GSFC) USA F o r t C h u r c h i l l G 116 W S Smi th (GSFC) USA Po in t B a r r o w 0 124 W S Smi th (GSFC) USA Wal lops I s l a n d S 166 J W Pe te r son (U Mlob lgan ) USA F o r t C h u r c h i l l G 119 W S Smi th (GSFC) USA Wal lops I s l a n d G 120 W S Smi th (GSFC) USA P o i n t Ba i r row G 124 W S Smi th (GSFC) USA P o i n t B a r r o w G 120 W S Smi th (GSFC) USA White Sands X 241 H H i n t e r e g g e r ( A F C R L ) B r a z i l A J S A Wal lops I s l a n d X X 162 R E Bourdeau (GSFC) USA E g l i n X 109 J U l w l c k ( A F C R L ) USA Wal lops I s l a n d X 150 W J H e i k k i l a , J A F e ] e r (SW Cent A d v Stud. USA Wal lops I s l a n d X 171 R G Stone (GSFC) USA W a l l o p s I s l and X X 180 S A B o « h l l l (U I l l i n o i s ) , L 0 S m i t h (OCA) USA E g l i n X 344 C H o u l t , ( A F C R L ) USA F o r t C h u r c h i l l X 160 K . A A n d e r s o n (U C a U l o m l a , Bexke le i r ) USA Wal lops laipwH X 182 L R 0 Storey (Centre Na t . d 'Etudesede C o m m i u i l c a t l o n ) USA F o r t C h u r c h i l l X 148 K . A . A n d e r s o n ( U . C a l i f o r n i a , B e r k e l e y ) USA Whi te Sands 200 R G iacoon i , o t h e r s ( A m Sol b Eng ) USA Wal lops I s l and X X 806 0 P Serbu (GSFC) USA Whi te Sands X C C u n n l f f ( A F C R L ) USA W a l l o p s I s l a n d X X 182 L R. 0 Storey (Centre Na t d 'Etudesde C o m m u n i c a t i o n ) -9

;o 00 S U M M A R Y OF SOUNDING R O C K E T L A U N C H I N G 1964 - 1965 (continued) Date (UT) T i m e (UT) Rockot Number o r Typo Sponsor ing Coun t ry Lanunchlng Site E x p e r i m e n t s A l t i t u d e (km) P r l n c E x p e r i m e n t e r ( s ) <i InsUtut lon(s) A tm o s P h y si cs A tm o s C om p lo no P h y si o s P a rt ic le s & F ie ld s A ir g lo w & A u ro ra S o la r P h y si cs o th e r (t es t) 1965 28 Sept 0910 NASA 4 ISO GA USA Whi te Sands X X X 183 0 E B e r g , o the r s (GSFC) G I - G B l O o t 0130 NASA 4 121 CG USA White Sands 148 F C F i s h e r (Lockheed) 5 Oct 0907 N B 2 0 170 USA Vandenberg A F B X X 5 Oct 2321 NASA 14 202 GA USA F o r t C h u r c h l U V X 206 J E Bed inge r , L . G Smi th (GCA) 13 Oct 1601 NASA 10 152 G M USA Point B a r r o w G W S Smi th (GSFC) 13 Oct 1612 NASA 10 97 G M USA F o r t C h u r c h l U G 124 W S Smi th (GSFC) 13 Oct 1651 NASA 10 129 G M USA WaUops I s l and GS 110 W a Smi th (GSFC) 18 Oct 0931 A E 7 618 D USA F t W a l n w r i g h t X 103 J U l w i c k ( A F C R L ) 19 Oct 1730 NASA 10 177 G M USA Point B a r r o w G W S SmUh (GSFC) 19 Oct 1730 NASA 10 98 G M USA F o r t C h u r c h l U G 123 W S Smi th (GSFC) 19 Oct 2000 NASA 4 142 NA USA WaUops I s l and 179 C A . B a r t h ( JPL) 19 Oct 2310 NASA 10 174 G M USA WaUops I s l and G 114 W S S m i t h (GSFC) 20 Oct 2035 NASA 4 146 DS USA White Sands X 184 M J Koomen , o the r s (Naval Res Cot ) 2 1 0 c t 1600 NASA 4 164 UA USA WaUops i s l a n d 190 W G Fas t l e (Johns Hopkins) 2 1 Oct 2054 A E 7 619 D USA F t W a l n w r i g h t X 137 J U l w i c k ( A F C R L ) 23 Oct 0530 ND 3 167 USA White Sands X 257 L S GuUodgo (NRL) 23 Oct 1538 NASA 10 178 G M USA Poin t B a r r o w G W S SmlUi (GSFC) 23 Oct 1614 NASA 10 175 G M USA Wal lops I s l and G 118 W S. S m i t h (GSFC) 23 Oct 1638 NASA 10 172 G M USA F o r t C h u r c h l U G 114 W S S m i t h (GSFC) 27 Oct 2348 NASA 10 179 G M USA Point B a r r o w G W S. S m i t h (GSFC) 27 Oct 2348 NASA 10 173 G M USA F o r t C h u r c h l U G W & S m i t h (GSFC) 28 Oct 0010 NASA 10 176 G M USA WaUops I s land G 117 W S. S m i t h (GSFC) 2 Nov 2000 A E 13 5S9 USA E g l i n S 502 A . C F a i r s ( A F C R L ) 2 Nov 2340 S-1 USA E g l i n V X 134 N W Rosenberg ( A F C R L ) 3 Nov 0917 A E 6 557 USA E g l i n S 137 A . F a l r e ( A F C R L ) 3 Nov 1900 A E 3 520 USA White Sands X 210 H H in t e r egge r ( A F C R L ) 9 Nov 0700 NASA 18 02 GA USA F o r t C h u r c h U l X 328 G R C a r l g n a n { ( U . M i c h i g a n ) 9 Nov 1840 NASA 14. 168 UA USA F o r t C h u r c h U l 1 G R C a r l g n a n , J H o r v a t h (U Mich igan ) 9 Nov 1900 A F 3 523 USA White Sands X 238 H H in t e r egge r ( A F C R L ) 10 Nov 0230 A D 3 356 USA White Sands ISO J Sa l i sbu ry 10 Nov 1823 A E 6 379 USA E g l i n X 114 R Sagalyn ( A F C R L ) 10 Nov 1916 NASA 18 03 GA USA F o r t C h u r c h U l X 328 G R C a r l g n a n ' ( U M i c h i g a n ) 11 Nov 0410 Ae 6 378 USA E g l i n X 113 R Sagalyn ( A F C R L ) 11 Nov 0415 S-2 USA E g l i n V X 137 N W Rosenberg ( A F C R L ) 16 Nov 1600 NASA 4 199 NA USA White Sands 144 N H F a r l o w (Amos Res Cnt ) 17 Nov 0425 NASA 14. 23S UE USA F o r t C h u r c h U l X X 178 W a M u r c r a y (U A l a s k a ) 18 Nov 0220 S-4 USA E g l i n V X N W Rosenberg ( A F C R L ) 18 Nov 0S2O A E 6 382 USA E g l i n X 116 R Sagalyn

SUMMARY OF SOUNDINO ROCKET LAUNCHINa 1 9 8 4 - 1965 (continued) Date T i m e (UT) (UT) Backet Number o r Type Sponsoring Country E i p e r l m e n t s T Al t i tude (km) P r inc Exper]mei i ter (8) ft Instltutloa<B) 1965 18 Nov 0801 IS Nov 1121 IS Nov 1431 20 Nov 0037 20 Nov 0520 24 Nov 0404 24 Nov 1537 2 Dec 1730 9 Dec 2133 10 Dec 0600 11 Dec 0562 11 Dec 1866 15 Dec 1700 16 Dec 1919 18 Dec 0469 S-6 A E 6 484 NASA 14. 78 UA NASA 14.109 G I NASA 14.238 UE NASA 14. 124 UE NASA 14.242 UE NASA 4.145 GS A A 6 174 A A 6 173 A A 6 . 1 7 2 A E 6 668 NASA 14. 247 U I NASA 14. 88 n NASA 14. 69 n USA USA USA Norway/USA USA USA USA USA USA USA USA USA USA BrazU/USA B r a z i V U S A EgUn E g l l n White Sands Andoya F o r t Church iU F o r t Church iU WaUops I s land White Sands F o r t Church iU F o r t Church iU F o r t Church iU F o r t Church iU WaUops Is land Nata l Nata l X X X 137 155 149 122 189 186 138 142 165 155 182 179 188 N W Rosenberg N W Boaenberg C L. Hemenway (Dudley Obs ) J A . Kane, J T r o i m (OSFO W B . M u r c r a y (U Alaska) W a M u r c r a y (0 A l a s k ^ R. C Haymes (Rice U ) K . F redga ( O S F Q A . F a l r e ( A F C R L ) A . F a i r s ( A F C R L ) A . F a i r e ( A F C R L ) A. F a l r e ( A F C R L ) L . 0 Smi th (GCA), & A . B o w U U (U Rl ino i s ) F deMendonca ( B r u U ) L . J B l u m l e ( O S F O F deMendonca (BrazU) L . J B l u m l e (08FC) NASA ROCKET CODE Place 1 Type of vehicle Place 2 F l i g h t number ot se r ies . Place 3 Ins t rument ing agency — Place 4 Type of exper iment Example Type of Vehic le to NASA L — Aerobes 100 0 2 — A r c on N 3 — Nike Asp U 4. — Aerobee 160, ISOA D 5 — I r i s A 6 — Aerobee 300 C 7 — A r g o E-6 I 8 — Javel in 9 — Skylark 10 — Nike Cajun I L — Journeyman 12 — Special p ro jec t s 14. — Nike Apache 16 — Areas 18 — Astrobee 1600 17 — Aerobee 350 18 — Nike Tomahawk Ins t rument ing Agency - College o r Un ive r s i t y • Depar tment of Defense - Other Government Ageni • I ndus t r i a l Corpora t ion Type of Exper iment A — Aeronomy B — Bio log ica l E — Energet ic p a r t i c l e s ft fields 0 — Galact ic estonomy 1 Ionospheric physios M — Meteoro logy P — Special p ro jec t s B — Radio as t rc t tomy S — Solar physios T — Tes t and support