spacelab 3 mission science review

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4 N A S A Conference Publichion-2429- 1 e

Spacelab 3MissionScienceneview

Proceedings of a sympos i um he l d a tNASA George C . Marshall Space Flight CenterMarshal l S pace Fl ight Center , Alabama

December 4 , 1985


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NASA Conference Publication 2429

Spacelab 3MissionScienceReviewEdi ted byGeorge H. FichtlGeorge C . Marshall Space Flight CenterMarshall Spac e Flight Center, Alabam a

John S. TheonNational Aeronautics and Space Administration

Washington , D. C.Charles K. Hill and Otha H. VaughanGeorge C . Marshall Space Flight CenterMarshall Space Flight Center, Alabam a

Proceedings of a symposium held atNASA George C. Marshall Space Flight CenterMarshall Space Flight Center, AlabamaDecember 4. 1985

NASANational Aeronauticsand Space AdministrationSiientific and Technical

Information Branch1987


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TABLE OF CONTENTS

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Spacelab 3: Research in Microgravity. . . . . . . . . . . . . . .. . . . . . . . . . . . . . .. . . . . . . . . . . . . ..Spacelab 3 Vapor Crystal Growth Experiment . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .Gro wth of T riglycine Sulfate (TG S) Crystals Aboard Spacelab-3 .......................Dynamics of Rotat ing and Oscil lat ing Drops . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .A Laboratory Model of Planetary and Stellar Convection . . . . . . . . . . . . . . . . . . . . . . . . . . . . .High Resolut ion Infrared Spectroscopy from Space: A Prel iminary Report o n theResul ts o f th e Atmospheric Trace Molecule Spectroscopy (ATMOS) Experimenton Spacelab 3 . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .Auroral Images from Spacelab I11 . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .Ions (Anuradha): Ionizat ion States of Low Energy Cosmic Rays . . . . . . . . . . . . . . . . . . . . . .Ames Research Cen ter Research Anim al Holding Facilities on SL-3 . . . . . . . . . . . . . . . . . . . . .Autogenic-Feedback Training: A Preventive Method forSpa ce Adaptation Syndrome . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .LS-3 Urine Monitoring Investigation . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .

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I --N8 7 - 221 0 4SPACELAB 3: RESEARCH IN MICROG RAV ITYG. H. Fichtl, J . W. Cremin, C. K. Hill, and 0. H. VaughanNASA Marshall Space Flight CenterMarshall Space Flight Center, Alabam a 35 8 12

J . S. Theon and R. SchmitzNASA HeadquartersWashington, D.C. 20546

ABSTRACTThe Spacelab 3 mission, which focused on research in microgravity, took place during the periodl 29 throug h May 6, 1985. Spacelab 3 was the second flight of the National Aeronautics and Spaceinistrations mo dula r Shuttle-born e research facility. An overview of the mission is presented here.

ll Space Flight Center on Dec ember 4, 198 5. This special issue is based o n reports presented at

INTRODUCTIONSpacelab 3, the second f l ight of the National Aeronautics and Space Administrat ions (NASA)orato ry, signified a new era o f research in space. The primary objective of the mission waso conduct applications, science, and technology experiments requiring the low-gravity environment ofa rth o rbit and stable vehicle attitude over an extended period (e.g., 6 days) with emph asis o n materialsprocessing. The mission was launched on Apri l 29, 1985, aboard the Space Shutt le Chal lenger whicha w eek later o n M ay 6. Th e multidisciplinary payload included 15 investigations in five scientificfields: mate rials scienc e, fluid dynam ics, life sciences, astrophysics, and atmo sph eric science.The basic Spacelab hardware for the mission included a pressurized long module and an Experi-me nt S upp ort Stru cture (ESS). The pressurized module provided a shirtsleeve environ men t where thepayload crew condu cted the experiments . The ESS provided a s t ruc ture for mo unting experimen ts whichrequired direct expos ure to space. Reference 1 provides additional details on the Spacelab 3 missionconfiguration. T he first Spacelab mission in late 1983 verified tha t the facility provided a suitableenvironment for research activities in a variety of fields. With this assuran ce, the S pace lab 3 mission wasdedicated solely to scientific experim ents, with no further verification testing. (Spacelab 3 was actuallythe second flight of t he laboratory because of delays in the developm ent of a point ing system for theSpacelab 2 mission.)The NASA Office of Space Science and Applications (OSSA) has overall responsibility for all

NASA Sp acelab and attach ed payload missions. Th e Spacelab 3 mission develop men t and operatio n wasmanaged and perform ed for OSSA by the NASA Marshall Space Flight Cen ter (MSFC). Spacelab 3investigations were selected by a peer review process and were judged on the basis of their intrinsicscientific merit and su itability for flight. Proposals for exp erimen ts came throu gh several channels,including NASA Announcements of Opportuni ty that sol ici ted research ideas from the worldwidescientific com mu nities and agreements with foreign governments. NASA selected 15 investigations forflight, including 1 2 investigations from the United States, tw o from France, and one from India. Tab le 1provides a list of the experiments and investigators by scientific discipline along with each investigationsacronym which will be used to refer to the instrument throughout this report .


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Soon after selection, experimen ters convened in an Investigators Working G roup (IW G) that met periodicallyto guide th e scientific planning for the m ission. Th e IWG included the principal investigator for eachexperiment chosen for flight and was chaired by the mission scientist, Dr. G. Fichtl, from MSFC. The IWG wasresponsible fo r allocating resources to different experim ents, organizing in flight science opera tions, and nominatingand selecting payload specialists. Over the years, the IWG served as a valiable forum for resolving conflictingscientific interests.

The Spacelab 3 mission was designed and o pera ted to provide the best low-gravity environm enttha t cou ld be achieved within th e capabilities of S pace Shuttle and Spacelab systems. Th e high qualitymicrogravity environment was conducive to materials processing and fluid dynamics research and at thesame time maximized the scientific return for the tota l payload. Five experim ents - three in crystalgrowth and two in fluid mechanics - were extremely sensitive to gravity, vehicle accelerations, andmaneuvers. Mission management gave careful consideration to the elements influencing the Spacelabenvironment. Maneuvers fo r an astronomical expc?rlrr?entwere sched~?!edduring th e first 18 hours of themission. Fo r the remain der of the mission, the orbiter was maintained in a gravity gradient attitudewith the tai l pointed toward Earth, the wings oriented in the orbi t plane, and the payload bay open tothe S outh ern Hemisphere. Maintenance of this stable attitu de required th e least num ber of verniercon trol system thruster firings and , thus, reduced disturban ce of the delicate experiments. Th e attitu dewas also sui table fo r th e atmospheric and cosmic ray astronomical observat ions made by three o therSpacelab 3 instruments. Th e particular flight attitu de was also selected for a subtle reason which will bereferenced later in a discussion of th e fluid dynam ics experiments. Th e materials science and fluidphysics experiments were clustered around the center of mass of the vehicle, a location least affected byforces proportional to the distance from the center of mass.

The Spacelab 3 mission operations were managed by a MSFC ground control team working inthe Payload Operat ions Control Center (POCC) a t the John son Space Center (JSC). Science teams foreach of the experiments worked in user rooms adjacent to the POCC and interacted with the payloadscience crew through the POCC com mun ications system. Spacelab 3 demonstrated the value of directcom mu nication between the science crew in space and th e research teams on the groun d. The missionset a record for downlinked video with over 3 million recorded images. The mission clearly demonstratedtha t Spacelab represents the merger of science and m anned spaceflight. Scientists in space collaboratedwith their colleagues on the ground, solving problems and modifying experiments to enhance scientificyield.

Payload specialists (PSs) cond ucted the onb oard scientific investigations. They were selected andtrained by the Spacelab 3 principal investigators (PIS) and instru me nt facility developers. Th e flight pay-load specialists were Dr. Taylor Wang of the Jet Propulsion Laboratory in Pasadena, California, and Dr.Lodewijk van den Berg of th e EG&G C orporation in S anta Barbara, California. Th e alternate PSs wereDr. Eugene Trinh of the Jet Propulsion Laboratory and Dr. Mary Helen Johnston of the Marshall Center.The alternate PSs supported the mission operations in the POCC. Dr. Wang was the principal investiga-tor for the Drop Dynamics Module experiment (see below), and Dr. Trinh was a co-investigator for thatexperim ent. Dr. van den Berg was a co-investigator for the Vap or Crystal Gro wth System expe rime nt(see below).

These four scientists were selected f o r their specialized backgrounds and experience in materialssciences and fluid mechanics, Drs. van den Berg and Johnston are materials scientists with expertise incrystal growth, and Drs. Wang and Trinh are fluid dynamics experts. The flight payload crew consistedof the PSs and the m ission specialists (MSs). T he design ated MSs inclu ded Drs. Don L ind, WilliamThornton, and Norman Thaggard. The f l ight crew was charged with operat ion of the Shutt le and wasstaffed by commander Col. Robert Overmyer and pilot Lt. Col. Frederick Gregory. Th e MSs were

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practical applications as a pyroelectric infrared detector. Th e crystals are the basis of advanced sensorsystems for applications which include Earth resources surveying, pollution monitoring, thermal imagingfor medical diagnostics, fire location d etectio n, and infrared astro nom y. Improved crystals (i .e., crystalswith few imperfections) potentially resulting from spaceflight could result in improved detector cap-ability.

Mercuric Iodide (Hg12) Growth for Nuclear Detectors (VCGS)Th e purpose of this investigation was to grow m ore perfect m ercuric iodide crystals in a low-gravity environment by taking advantage of diffusion-controlled growth conditions and by avoiding theproblem of strain dislocations pro duc ed by the crystals weight. A single crystal was grow n in this

facility for approximately 120 hours. The pay-load and mission specialists initiated the crystal growth process, monitored the growth phase through amicroscope, and responded to crystal growth behavior by making changes in the hardware parametersettings.

This experiment required extensive crew participation.

After returning to Earth, the crystal grown in space was subjected to gamma-ray rocking curvediffraction measurements. Th e results obtained to da te indicate that the space-grown crystal is of higherqual i ty and more homogeneous than any mercuric iodide crystal grown thus far on the ground. Addi-tional experiments will be made to determine the electronic properties of the space crystal and to evalu-ate th e e ffect of reduced gravity o n th e vapor transp ort process. This crystal substance has considerablepractical importance as a sensitive gamma-ray detector and energy spectrometer that can operate at roomtempera ture. Presently, cumbersome cryogen ic systems are used to c ool available dete ctors to near liquidnitrogen temperatures. However, the performance of m ercuric iodide crystals only rarely approa ches theexpected performance, presumably because some of the free electrical charges produced within thecrystal are not collected at the electrodes but instead remain trapped or immobilized as crystal defects.An eff icient high atomic number semiconductor detector that is capable of operat ing at room tempera-ture utilizing single mercuric iodide crystals offers potential beyon d existing de tector technology.

Mercuric Iodide Crystal Growth (MICG)The objectiveof this experiment w as to study crystal seed and growth processes w ith the vapor crystal growthtechnique in two and three zone furnaces. The crystal material, mercuric iodide, is the same as that grown in theVCGS, and onc e again vapor growth process was used. In this experim ent, the focus is on the location and number ofnucleation sites as a function of temperature distribution and partial pressure of an inert host gas (argon). Sixampoules, approximately 20 cm long and 1.5 cm in diameter, were flown on Spacelab 3 . A distribution in tempera-ture is maintained between the en ds of the ampoule with and w ithout material sinks at the cold en d. A Stefen flow ofmercuric iodide occurs from the hot to the cold ends of the amp oule. Nucleation occu rs on the walls in the cold zone

(1/3 of amp oule). The number and location of these sites, as well as the crystal seeds , are the quantities of interest.The effec t of argon gas is to increase the number of nucleation sites and reduce the growth rate. T wo experimentswere perform ed, each in sets of three ampoules. The facility was operated over the entire mission. Th is experimentbuilds upon knowledge gained from similar experiments performed with the same facility on the S pacelab 1 missionwherein the goal was to grow single large crystals. This furnace was automated and required with minimal crewinteraction.

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F LU D D YNAM Cs EXPE R IMENTSThe Spacelab 3 f luid dynamics experiments are aimed at the study of fundamental f luid dynamicprocesses associated with rotatin g and oscillating drops and conv ection in spherical geom etry.

Geophysical Fluid Flow Cell Experiment (GFFC)The primary objectives of the geophysical fluid flow experiments are to simulate large-scalebaroclinic (density-stratified) flows which occur naturally in the atm osph eres of rotating planets and starsand to gain insights concerning the large-scale nonlinear mechanics of global-scale geophysical flows inspherical geometry. In particular, the investigators hope to identify those external conditions related tofluid viscosity, rotation, gravity, etc., which allow qualitatively different modes of instability or waves in themodel.The experiments were accomplished with a rotating hemispherical shell of fluid wherein radialgravitational forces are simulated with electrical polarization forces cre ated in a dielectric fluid by apply-ing a radially d irecte d voltage d ro p across th e fluid. The GFFC provides a simulated gravitational field

of approximately 0.1 g o r less. Spa ceflight is required to insure the spherical symmetry of the totalgravitational field in t he exp erim ent; in a terrestrial lab orato ry, gravity will destroy th e sphericalsymmetry of the gravitational field in the GFFC. Total experiment t ime was 103 hours. The obser-vations of temperature fluctuations in the fluid indicate that strongly rotating bodies exhibit global-scale convective patte rns tha t tend to align themselves in Taylo r columns oriented parallel to th erotatio n axis. However, as the degree of thermal instability is increased, strong buoyancy-driven turbu-lence sets in at high latitudes. At very large heating rates (or high Rayleigh numbers), this polar con-vection spreads toward th e equa tor and eradicates the Taylor columns. When the imposed radiallyunstable tem pera ture g radient includes a latitudinal com pon ent, new spiral instabilit ies are observed.At high heat ing and high rotat ion, th e Taylor columns reappear bu t interact s t rongly with mid-lat i tudemotion s. The ex perim ents are in agreement with linear theo ry and num erical simulations tha t can becarried ou t a t th e least e xtrem e therm al cond itions (lower Rayleigh num bers) of the laboratory model[41.

It is interesting to note that a vehicle attitude in which the angular velocity vectors of the vehicleand the exp erim ent conv ection cell are parallel is preferred to minimize precessionally-driven fluidmotions from occurr ing in GFFC. The Spacelab 3 vehicle attitude satisfied this requirement.

Dynamics of Rotating and Oscillating Free Drops (DDM)The experiments performed in the DDM provided the first experimental data on free rotatingand oscillating drops. The DDM is a three-axis acoustic facility wherein liquid drops can be formed and

excited to exe cute r otatio nal an d oscillatory mo tion. Spaceflight is required because very stron g acou sticforces would be required in terrestrial-based experiments which in turn would introduce physicalphenomena that would overwhelm the physics under investigation.The DDM research conducted on Spacelab 3 has yielded the first concrete experimental evidenceon the ma nipulation of liquid drop s using acou stic radiation pressure forc es in microgravity. Drop s ofwater and water and glycerin mixture s were successfully deploy ed and cap tured by the acoustic potentialwell w ithou t introducing any significant static distortion on th e samples. Ro tation aro und a fixed axis

of the drops was also induced through acoust ic torque and has al lowed a s tudy of the equi l ibr ium dropshape depen dence on the r otatio n rate, Results of some shape oscillation sequences have also confirmedthe feasibility of surface tension a nd viscosity measurement schemes.5


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The axisymm etric regime of a freely suspended rotatin g dro p has been stud ied in detail usingvolumes ranging from 0.5 to 10 cc, with viscosities between 1 and 100 cSt , l iquid densi ty around 1.16g/cc, and surface tension centered at 65 dyne s/cm. Very repeatable results have been ob tained fo r thespin-up rate, the critical rotation speed for bifurcation between axisymmetric and two-lobed shapes, theaxial deformation dependence on the rotation rate, and finally for the critical velocity at fission. N oexperimental evidence for any transition to higher multi-lobed shapes have been obtained in this firstset of experiments.

The experiments are of fundamental interest because they are the f i rs t control led experiments tobe performed on essentially free drops and thus provide the first experimental data for testing theoreticalpredictions. They also provide guidance for deve lopm ent of theoretical models. The experiments arealso of practical interest because acoustic manipulation of liquids is a prime candidate for containerlessprocessing applications in space.

LIF E SCIENCES EXPERIMENTSThe Spacelab 3 mission life sciences experiments were aimed at (1 ) verification of design andbiocompatibility assessment of research animal holding facilities, (2 ) calibration and verification of aurine monitoring system, and (3) test and application of autogenic feedback processes as a counter-measure to space adaptat ion syndrome.

Ames Research Center Life Science PayloadIn response to a recognized ne ed for an in-flight animal housing facility t o su pp ort Spacelab lifesciences investigations, a Research Animal Holding Facility (RA HF ) was developed. Th e Spacelab 3mission provided an oppo rtun ity to perform an in-flight Verification Test (VT) of the RAHF . Lessonslearned from the RAHF-VT and baseline perform ance data will be invaluable in preparation fo r subse-quent dedicated life sciences missions.The RAHF is designed to support animals ranging in size from rodents to small primates. It isanticipated that such a system will satisfy the experimental requirements of a great majority of prospec-tive investigators working with comm only-used lab orato ry animals.On Spacelab 3, one RAHF was dedica ted to supporting two monkeys in separate cages while theother suppor ted 24 rats. The primate RA HF has the capabi l i ty to house fou r monkeys; however, becauseof a decision to fly monk eys free of herpes virus Sam uri only tw o m onkeys w ere f lown o n this checkoutmission. A photocel l method wasused to record animal act ivi ty. Fo ur of the rats were mo nitored by a biotelemetry system (BTS) whichrecorded deep body temperature, heart rate, and waveform. Fo ur rats were intermit tent ly photographed

during the mission by a movie camera programmed at given frame rates; the film was used to assessbehavioral response to launch/recovery cond itions and to weightlessness. Th e environ men t was auto-matically mon itored and con trolled for factors such as tem pera ture, hu mid ity, and airflow. During ascentand entry a dynamic environment measuring system (DEMS) was used to measure noise, vibration, andacceleration forces in the vicinity of the RAHF.

Over the 7-day flight, food and water were dispensed automatically.

The RAHF worked very well, with some exceptions involving particulate release. The rats andmo nkey s w ere recovered unstressed, in excellent condition, and m icrobiologically clean. This informationallows us to s tate that the RAH F maintains animals in a manner analogous to vivarium animals in labora-tories and permits support of animal research in space in a realistic manner.

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While the data is only part ial ly reduced at this point , mu ch inform ation has already been obtainedanimals. One monkey demon strated symptom s of space adaptat ion syndrome while the other didThe ra ts returned to Earth with the following changes: they were flaccid, showing a markedease of muscle t on e; marked loss of muscle and fiber diam eter; reduce d activity of the Krebs cycle

in ep ythr opo ietin. As data analyses are com pleted, it is expected that this mission willthe mo st significant con tribu tion o n biological systems in sp ace ever gained from a single mission.

Urine M onitoring Investigation ( UM S)This investigation was designed to evaluate the UMS and to monitor the urine biochemistry of thew. Th e primary objectives of th e Urine Monitoring Investigation were (1) to verify the operation ofUrine Monitoring Sys tem (UMS) in the collection and sam pling of urine, (2) to perform in-flight

(3) to est imate the crew members rat io of f luid intake to urine output , andto m easure the e ffects of microgravity on a number of biochemical con stitue nts of urine. Subse-

vity exposure. Because of insufficient air flow through the UMS, only a few urine sampleshe sample. The calibration and testing objectives of th e investigation were com pleted.

Autogenic Feedback TrainingThe object ive of this experiment was to test the effectiveness of th e com bined use of au togenic(SAS) and to gain basicological data associated with SAS. Autogenic feedback training is a proced ure th at enables hum ann volu ntary c ontr ol of several physiological responses simultaneously. Autogenic and

to mot ionckness. However, i t appears th at a com bination of these tw o techniques for con trol of bodily responsesbe learned in a relatively short period of time. Theigator a t the NASA A mes Research Center has obtain ed excellen t results in ground-basedg chair experim ents fo r subjects with a wide-range of susceptibility to mo tion sickness. The

3 mission AFT experiments involved the flight payload specialists as subjects and two of theas contro ls, Th e subjects were given exercises to pract ice in the event of discomfort .During th eir awake periods, both subjects and controls were instrumented with sensors to measurerecord hea rt rate, body temp erature, galvanic skin response, air volume, and breathing rate. These

to the subjects on a wrist readout an d used during A FT exercises by the su bjectsto discom fort associated with space adaptation as well as during rou tinely scheduled exercisesAnalysis of th e Spacelab 3 AFT results is now underway.ATMOSPHERIC OBSERVATIONS

The Spacelab 3 mission environmental observation experiments are aimed at the (1 ) measurement(2) observat ion of southern aurora from a Spacelab orbi t

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Atmospheric Trace Molecule Spectroscopy (ATMOS)This investigation was designed to obtain fundamental information related to the chemistry andphysics of Earths upper atmosp here using the techniques of infrared absorption spectroscopy. The reare two principal objectives. The first is the determination, on a global scale, of the compositionalstructure of the upper atmosphere and its spatial variability. The establishment of this variability repre-sents the first step toward determining the characteristic residence times for upper atmosphere consti-

tuents, the magnitudes of their sources and sinks, and, ultimately, an understanding of their effects onthe stability of the stratosphere. The second objective is to provide the necessary high-resolution, cali-brated spectral information required for detailed design of advanced instrumentation for global mini-toring of specific species.The experimental approach for acquir ing the data from Spacelab was to view the Sun with theATMOS instrument during the periods just pr ior to entry intoj a n d shnr?!y a f t e r emergng ~TCE , a s d a roccultation . Specifically, the viewing periods were timed t o occ ur when the ATM OS instrum ents view o fthe Su n was occulted by th e upper atmosphere. During these periods, the instru me nt mad e a set of inter-ferometric measurements of the solar radiation incident as a function of optical path difference withinthe instrument . Subsequent Fourier t ransformation of these measurements produced spectra of the solarcont inuum between 2 and 16 m with a resolut ion of 0.02 cm-1. The characteristic abs orptio n features

are associated with stratospheric layers approx imately 2 km thickness.The instrument operated superbly. A total of 20 occultations were taken encompassing altitudes

from approximately 5 to 120 km.Preliminary analysis of the data has revealed th e presence of mo re than 3 0 different molecularspecies whose concentrations can be measured over altitude ranges that vary, depending on the particu-lar const i tuent , f rom the upper t roposphere through the st ratosphere and mesosphere to the lower ther-mosphere (approximately 130 km). Several of the t race const i tuents (for example N2O5 and ClON 02)have not previously been detected with certainty. Th e stratosphe ric spectra provide simu ltaneous mea-surements of most of the species of importanc e in the nitrogen, chlorine, and hydro gen families of

molecules involved in the ozone photochemistry of this region; the observations of the mesosphere andthermosphere, which include measurements of CH4, C 02 , CO, H2 0, and 0 3 , provide new insights intothe photochemistry and dynamics of the region of the atmosphere characterized by dissociation of theminor gases and by the effects of the breakdown of local thermo dyna mic equi l ibr ium [5 I .In addition to the telur ic spectra, the Spacelab 3 ATMOS flight returned a sufficient number ofhigh resolution solar spectra to produce a very high signal-to-noise ratio solar atlas of the near and mid-infrared wavelength region. When published, this atlas will show fea tures of the Suns photo sphere andchromosp here that have n ot been previously observed, NASA plans to fly the ATMOS instru m ent atapproximately yearly intervals for the next 10 to 15 years to provide an archive of the composi t ion ofthe uppe r atmosphere and its variability. The d ata will provide a valuable reco rd to aid in the assess-

men t of long-term changes in the properties of the atmosphere.Auroral Observations

The Spacelab 3 mission provided a unique opportuni ty to make detailed observations of SouthernHem isphere aurora from space. Observations of aurora are available from the groun d and from spacelooking downward from satellites (Dynamics Explorer, Defense Meteorological Satellite Program, forexamp le). However, sy stematic observations o f auror a fro m a lateral vantage point like tha t provided by

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3 mission o rbit with 57 deg inclination and sufficiently large angle (angle between the S un-to penetrate the average auroral oval in darkness were not availableously. The typical aurora altitude is appro xima tely 11 0 t o 160 km and range in vert ical extent from15 to 5 0 km. Thus, with a 350 km orbi t al t i tude and range to the aurora target f rom

0 to 800 km, the viewing perspective varies from a downward looking one to a sidewardThe orbiters video imager was used to acquire fiveof data. By using th e orb ital mo tion to provide the

have been viewed stereoscopically.The crew also took 274 color photographs.

The data provide the first views from outside the atmosphere of thin horizontal layers ofaurora. The layers , once thought t o be rare, were recorded on tw o ou t of three passes. Thisbeen a n o ptical il lusion caused by atmospheric refraction. Also, for the first t ime, verticallyin diffuse aurora. This is a measurement that is possible only from space,

ASTRO PHYSICA L OBSERVATIONSThe Spacelab 3 mission astrophysics experiments were aimed at the (1) study of ionization states

(2) study of galactic and faint extragalactic sources and

Cosmic Ray Experiment (IONS)The Indian ex perime nt, IONS (also called ANURADHA by th e science team , ANU RADH A is the

3. The flight period was( 1 ) absence of solar flares and by (2 ) low-level of solar activity close to that of solar3 Mission was most favorable for the present studies of low-energycosmic ray heavy nuclei. The Anu radha experiment measures, in near Ea rth space, th e flux,of all heavy ions of all major elements, from helium to i ron ,of abou t 5 t o100 MeV/amu. Fr om the arrival direction of heavy ions in space, the threshold magn etic rigidities (i .e. ,

of cosmic ray trajectories in geomag-By com bining the da ta of mag netic rigidities with m om entu m of ions measured in the mainf heavy ions are determined. The measurements of the ionizat ion states ,of the ACR which

Fro m th e initial stud ies of track d ensity of cosmic ray events, i t is calculated that t he m ain detec-of abou t 10,000 particles and similar number of C, N, 0 and heavierAnalysis of t he main d etecto r stack is in progress.

Ultraviolet Astronomy Experiments (VWFC)The proposed experiment was designed to s tudy (1 ) large scale distribution of ultraviolet radiation

of stellar clouds and spectral distribution, (3 ) diffusion ofof galactic material), (4) sky background relative to


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discrimination between galactic and extragalactic light and Sun light scattered by interplanetary dust(zodical light), and ( 5 ) spectral dist r ibut ion of extended sources (as noted above) and nebular spectro-graphy. Measurements were t o be taken with a Schmidt camera which uses a 4 m square photocathodeproximity (diode) light intensifier to sense the incoming UV (1 550-2300 angstroms) radiation. Threeinterference filters a t wavelengths of 15 50, 1 900 , and 25 00 angstrom s with a slit provided spectrogra phcapability. The instrument field of view if 54 deg with angular resolution of 3 arc minutes. Th e instru-ment was designed to operate out of the scientific air lock after sunset. Six targets were planned forthis mission. This instru me nt flew on the Spacelab 1 mission and acquired data on the lower half of thecelestial sphere. Th e Spacelab 3 mission targets were primarily located in the northern half of thecelestial sphere [3 I .

Because of a malfunction of the Spacelab scientific air lock, it was not possible to carry out thisinvestigation.

S UM M ARYThe Spacelab 3 mission, by any measure, was an outstanding success. We have learned how toutilize the Shuttle/Spacelab system to provide the best low-gravity environment achievable from thissystem . This knowledge is being used in the develop me nt of Space Station and low-gravity facilit ies.T he Spacelab 3 mission is a model for designing and operating future low-gravity Spacelab missions.Much of the research begun on Spacelab 3 will continue on future Spacelab missions and will help setthe stage for research aboard Space Station.

REFERENCES1. Hill, C. K., NASA TM-82502, 50 pp., November 1982.2. G. Cou rtes, M. Viton, J. P. Sivan, R. Decher, and A. Ga ry: Science, Vol. 225 , 1984, p. 179.3. S . Biswas, et al., ibid, p. 64.4. J . E . Hart, et al ., ibid, p. 27.5 . C. G. Farmer and 0. F. Raper, ibid, p. 42.

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ORIGINAL PAGE N8 - 22 1 1POOR QuALm AURORAL IMAGES FROM SPACE 3

Thomas J . HallinanGeophysical Institute University of Alaska, Fairbanks, AK 99775-0800Don Lind

NASA Johnson Space Center, Houston, TX

The Spacelab 3 space shuttle mission of April 29-May 6, 198 5, provided an excellent opportunity to surveythe Aurora Australis from near-Earth orbit. T he orbital inclination and Beta angle were such that the orbit penetratedthe average auroral oval in darkness. (Some aspects of the observations were compromised by scattering ofmoonlight from the clouds below.) Since this was a manned mission, it was practical to use imaging detectors thatrequired aiming and high-bandwidth recording. W e obtained 274 color photographs of the aurora and approximately5 hr of black and white video recordings. T he data cover 22 separate passes from seven da ys. O n several occasionsthe Or biter passed above the auroral form s. By using the orbital motion to provide the parallax, we have been able toview both the color photographs and the video recordings stereoscopically.

The d ata provide the first views from outside the atmosphere of thin horizontal layers of enhanced aurora(Fig. 1) . The layers, once thought to be rare, were recorded on two out of three passes. This first observation ofenhanced aurora from space eliminates concerns that the ground-based observations might have been an opticalillusion caused by atmospheric refraction. Also, for the first time, vertically thin layers were observed in diffuseaurora. This is a measurement that is possible only from space ideally in nearth-Earth orbit.

Figure 1 . The A urora Australis seen from Spacelab 3 . The thin uniform band parallel to the Earths curved line is anedge-o n view of the airglow layer at -95 km altitude. A rayed auroral arc is seen just above the airglow layer andbending equatorward to pass under Challenger seen in the foreground. The rays in the arc have vertical extents of-60 to 200 k m , but there is a very thin (< 2 km ) band of enhanced auroral emission running through the aurora nearthe base of the rays. In the color photographs this is easily distinguished from the airglow layer beneath it.

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N8 2- 221 1 1IONS (ANURADHA): IONIZATION STATES OF LOW ENERGY COSMIC RAYS

S. Biswas, R. Chakraborti, R. Cowsik, N. Durgaprasad, P. J. Kajarekar,R. K. Singh, M. N. Vahia, and J. S. YadavTata Inst i tute of Fundamental Research, Bombay 400005, IndiaN. Dut t , J. N. Goswami, D. Lal, H. S. Mazumdar, and D. V. Subhedar

Physical Research Laboratory, Ahmedabad 380009, IndiaM. K. PadmanabhanISRO Satellite Centre, Bangalore 560 017, India

ABSTRACTIONS (ANURADHA) (1 ), the experimental payload designed specifically to determine the ioniza-tion states, flux, composition, energy spectra and arrival directions of low energy (10 to 100 MeV / amu)anom alous cosmic ray ions of helium to iron in near-Earth space, had a highly successful flight andoperation in Spacelab-3 mission. Th e experimen t combines the accuracy of a highly sensitive CR-39

nuclear track detector with active com pon ents included in th e payload to achieve the experimen talobjective s. Post-flight analysis of detector calibration pieces placed within the payload indicated nomeasurable changes in d etecto r response due t o its exposure in spacelab environm ent. Nuclear tracksproduced by @particles, oxygen group and Fe ions in low energy anomalous cosmic rays have been iden-tified. It is calculated tha t the main de tector has recorded high quality events of abo ut 10,0 00 a-part iclesand similar number of oxygen group and heavier ions of low energy cosmic rays.D SCUSSlON

The low energy (5 to 100 MeV/amu) anomalous compon ent o f cosmic rays discovered in th e earlyseventies has been studied in great detail over the last decade. Comp rehensive information on composi-tion, energy spectra, radial gradient and time variation of the anomalous cosmic rays (ACR) in the inter-planetary medium have been obtained using instruments on board the IMP, Pioneer and Voyager space-crafts [ 2,3 ] . The near-Earth comp onent o f the ACR was fi rst ident i fied in a Skylab experiment [ 41 ;this has, however, not been studied in detail . Th e spacelab mission offered a unique op portu nity forsuch a stud y an d the Indian exp eriment IONS (or Anu radha) on board Spacelab-3 was primarilyintended for this purpose.

Several suggestions have so far been m ade ab out the origin of the anomalous cosmic rays [5 ] .The major distinguishing features of these models are the predicted charge states of ACR and its radialgradient and time variation. Fur ther, the models of Fisk et al. [SI a nd Fow ler et al. [ 5 ] suggest pro-duction of the anomalous component within the solar system, whereas Biswas et al. [SI suggested astellar origin for these low energy particles. Extensive studies of the interplan etary ACR com pon ent[3,6] have yielded valuable information on their radial gradient and time variation for the period 1973-19 84 which indicate an extra solar system origin fo r these particles. Howev er, n o direct measurement ofionization states of ACR is presently available, The prima ry objective of the IONS experiment was toobtain this crucial information for the near-Earth component of ACR. Addit ional information on com-position and intensity of this comp onent will also be obta ined f rom this experim ent. In this repo rt wepresent the salient features of the IONS payload, the experimental approach, f l ight operat ions and per-formance of the instrument and also preliminary results on anomalous particle fluences based on analysisof auxiliary detector elements placed inside the payload. The processing and analysis of the maindetec tor stacks are currently in progress.64


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Instrument and Experimental ApproachThe IONS payload flown in Spacelab-3 is shown in Figure 1. It is 48 cm in d iam eter, has aheight of 53 cm, and weighs 45 kg. The payload houses two detector m odules, the main detectormodule (bot tom stack) being about 40 cm in diameter and 4.5 cm thick. I t is composed of 174 sheets ,mostly of CR-39, All Diglycol Carbonate (DOP), nuclear track detectors along with a few sheets of LexanPolycarbonate each of thickness of 25 0 pm. On the top of this s tack, separated by a gap of 500 pm is a

single sheet of CR-39 of thickness 250 pm which is held rigidly to the instrument frame by a s tainlesssteel ring structure . During experimen t operation the main stack is rotate d using a high resolutionstepper m oto r and a gear assembly in discrete steps of 4 0 sec of arc once every 10 sec., so as to makeone complete revolut ion in 90 hrs . The movement of the stack is mon itored by a 15 bi t absolute shaftencoder coupled to i t . A thin 75 pm aluminum alloy dom e acts as the top enclosure of the sealed pay-load which is maintained at a pressure of 0.1 atmosphere during i ts space exposure. The payload wasmo unted direct ly o n a cold plate f ixed to a specially prepared ex perimental support s t ru cture to m aintainthe instrument temperature at a nominal value of 25"-40"C. The IONS instrument is mounted on space-lab with its Z-axis ti l ted by 25 deg so as to reduce the Earth shadow on the viewing cone during theflight. Th e gravity gradien t stabilized attitude of the shuttle provided very favourable celestial viewingof IONS with a viewing cone of abo ut 11 0 deg. Inside th e payload a tem pera ture sensor was placedclose to the detector module to monitor i ts temperature during the durat ion of the exposure. Smallsamples of test CR-39 detector elements, irradiated to energetic heavy ion beams from accelerators, arealso included in the payload for monitoring any possible changes in the detector response due to i t sexposure in pressure and temperature conditions within the payload. The ent i re operat ion of the IONSinstrument was control led by onboard computer and the relevant data regarding instrument funct ions(e.g. BMT, stack movement, temperature, etc.) are telemetered down link once every second for recordand monitoring by experimenters . The instrument operat ion could be ini t iated and interrupted, i frequired, by crew interface or via ground command.

The experimental approach for obtaining ionization states of ACR involves several major steps.The atomic number, energy and arrival direction of each energetic particle incident on the detectormodules are determined from an analysis of the t rack records lef t by the ions in the two CR-39 detectorstacks. The revelation of latent track s for optical viewing in these detec tors is achieved by etching thedetector sheets in a 6.25 N NaOH so lution at 70C for suitable duratio ns of several hours. Track parame-ters like length, diameter, and residual range are measured and used in conjunction with energetic accel-erator ion cal ibration data, f or the same CR-39 detector samples to determine a tomic num ber and energyof the tracks forming ions using standard procedures [71. The arrival time information will be obta inedfrom the angular displacement of each t rack in the bot tom detector s tack compared to i ts locat ion onthe top CR-39 sheet . This inform ation will be coupled with space shuttle's trajectory d ata. Thu s, th earrival direction of each ion in space is determined. Th e threshold m agnetic rigidities (i.e., m om en tum /charge) of ions are the n derived from th e computation of charged particle trajectories in geomagneticfield fo r the know n latitud e, longitud e, altitud e, and arrival directions. By combining the d ata of mag-netic rigidities with momentum of ions measured in the main detector, the ionization states of the heavyions are determined.

Flight PerformanceThe Spacelab-3 with IONS on board was successfully launched on day 119 at 16:02:18 GMT fromKen nedy Space Cen ter, Florida. Several factors contributed to make the Spacelab-3 mission ideally suitedfor t he stud y o f low energy cosmic rays. First, the flight period was characterized by very low level of

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solar activity free from any flare events. This is il lustrated in Figure 2, where we show two specificparameters characterizing the solar activity during the flight period and also their levels during solarminimum and m aximum. Second, the instrumen t operat ion period was also free from any signif icantgeomag netic activity. Fu rther, recent studies of anomalou s cosmic rays in interp lane tary space [31 haveindicated that during the last solar magnetic field reversal in 1980-81 the intensity of ACR was at i tsminimum value, and the A CR flux fo r 1 0 MeV/N o xyge n ions showed a steady rise from its 198 1 valueby a factor of about 10 during early 1985.The IONS instrument was act ivated on the third day into the mission via ground command.Following the act ivat ion, a snag was not iced as the payload was not responding to some of the comm andssent by the onboard computer. The cause was finally traced to a faulty cable connecting thecomputer to the remote acquisi t ion uni t through which commands were fed to the ins t rument . The faul twas rectified by the crew following procedures drawn up by NASA ground support personnel, and IONSstarted operation from day 123, 12:44:08 GMT. The performance of the instrument was excellent during theent ire period of operation of 64 hours, which was 71 percent of the planned ope rat ion durat ion. Thethermal control system also worked perfect ly and the temperature within the instrument was maintainedin the range of 22"-4OoC during the entire period of ope ration. We show in Figures 3(a) a sample ofencoder readings showing the actual and commanded positions of the ro ta t ing bot tom detec tor s tack

versus GMT. Each encoder ste p correspo nds to about 40 sec of arc once every 10 sec. An offset of 10divisions in comm anded position is introd uce d for t he sake of clarity. Figure 3(b) shows the instrum enttemperature for the same t ime sl ice, monitored by the temperature sensor kept inside the payload closeto the de tecto r module. Following th e successful comp letion of the mission, the IONS payload wasexamined and al l subsystems including the two detector modules were found to be in perfect condit ion,with no sign of any physical stress or strain suffered during its space exposure.

Detector Response and Preliminary ResultsThe CR-39 (DOP) (Allyl Diglycol Carbonate) plastic used in the present experiment is anextremely sensitive nuclear track detector, and was specially manufactured by Pershore Co. (UK) adoptinga long curing cycle and doping treatment with 1 percent dioctyl phthalate. Prior to the f l ight , samplepieces of this CR-39 (DOP) plastics were exposed to accelerator beams of low energy, upto 10 MeV/Na-particles, 12C, l6O , 20,22N e, 28Si, 52Cr, 58Ni and high energy, 1.88 GeV/N 5 6F e and 200 MeV/N238U ions to determine its nuclear track recording characteristics. The results obtained fro m m easure-me nt of trac k parameters in these calibration sam ples are show n in Figure 4, where we plot the ratio oft rack etch rate to bulk etc h rate, Vt/Vb, as a funct ion o f energy loss, dE /dx, for different ions. I t canbe seen that in the low energy loss region the etch rate ratio is a linear function of energy loss, whereasat higher energy loss region it can be approximated as a power function of energ y loss. A least squarefi t to th e d ata yielded the following response fun ction fo r the dete ctor over the energy loss region ofinterest.

v t / v b = 1 + 5.67 x (dE/ dx) + 1.22 x 10-l' ( ~ E / D x ) ~ * ~ (1)The results of the calibration studies also showed that the CR-39 (DOP) detector used in this experimentefficiently records tracks of all energetic particles with Z/p 2 8, where Z is the nuclear charge and pc isthe velocity of the ions and it should be possible to achieve a charge resolution of 0.2 charge unit.Sample pieces of CR-39 exposed to alpha particles, neon, iron, and uranium beams were also kept insidethe IONS payload to monitor an y change in i ts response funct ion due to th e ambient pressure (0.1 atm )and tempera ture (25-4OoC) within the payload. Post flight analysis of these calibration pieces indicates6 6


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that response characteristics of these CR-39 detectors remained the same during its exposure in spacelabenvironmen t. This can b e clearly visualized from Figure 4 where we have plotted the track et ch ratiofor neon and uranium ion t racks obtained from measurements made in cal ibrat ion detector pieces f lownin the payload. Hence the response curve [equat ion ( l )] is adequate for ident i fying atomic number ofthe t rack forming nuclei in th e IONS detecto r s tack.For zero t ime marking of the f ixed top de tec tor and the moving bot tom detec tor module , thedetector assembly was exposed to a narrow collimated beam of 50 MeV alpha particles in the VariableEnergy C yclotron , Calcutta. We first completed the analysis of a set of small area auxiliary dete ctors ofCR-39 f lown in the IONS detec tor module in order t o obtain ini t ial information on the types of lowenergy cosmic ray particles an d their fluxes. These CR-39 samples were etched in 6.25 N NaOH a t 7OoCfor 6 hrs. Figure 5 shows photomicrographs of some samples of tracks produced by low energy cosmicray alpha part icles , oxygen group (Z = 6-10) and Fe nuclei recorde d during the flight. The sharp defini-tion of the tracks is clearly evident in these photomicrographs. Based on the measured num ber of tracksof different io ns th e fluxe s of low ene rgy cosm ic ray alpha particles, o xygen grou p and iron nuclei w eredeterm ined. Th e time-average differential flux of alpha particles at 8 MeV/N is obtained as (1.3 f 0.23)x 10-5 particles cm-2 sr-l sec-l (MeV /N)-l. Assuming that th e energy spectrum of alpha particles is flatin th e region 8-50 MeV/N as in interplanetary space. We expect to ob tain abou t 10,000 times annotated

alpha particles in 8-40 MeV/N energy interval in the main dete ctor. Th e time-average differential flux ofoxyg en g rou p particles at 17 MeV/N is obtained as (1.7 f 0.5) x lom6particles cm-2 sr-l sec-l (Me V/N )-l.This value is in th e range expec ted from th e interplanetary flux measured in early 19 85 in Voyager-2,which is ab ou t 1 x p/(cm2.sr.sec.MeV /N) a t 15 MeV/N, considering the radial gradient of ACR an dthe transmission facto r in the geomagn etic field. At 26 M eV/N, the time average oxyg en group flux isobtained as (5.8 f 2.0) x p/(cm2.sr.sec.MeV/N). T his shows the steady recovery of ACR since solarmax imum in 1980 -81, and by April-May 19 85 it has increased by a large factor and has reached a level,being only 5-10 t imes lower from max imum flux of 197 4 level. Th e expected numbe r of anomalouscosmic rays of the oxygen grou p in the IONS detector in the energy interval of 15-30 MeV/N with arrivalt ime information is est imated to be about 8000 events . Th e expected numbe r of othe r com ponen ts ofanomalous cosmic rays can be est imated from the above num ber of events . In addi tion to anom alouscosmic rays we expect to obtain more than 10,000 galactic cosmic ray nuclei of oxygen and heaviernuclei in the IONS detector . Several impo rtant types of measurements such as isotopic composi t ion ofiron group nuclei can be carried ou t with high degree of reliability. Th e top CR-39 sheet and severalupper sheets of the bot tom s tack of the main detector of the IONS have been processed and themeasurem ents an d analysis of track s in these are currently in progress. Th e results obtained from thesedata will provide us the information on the ionization states and also on the compo si t ion, intensi ty andenergy spectra of low energy anomalous cosmic rays in near-Earth space which will provide new cluesto the origin of this enigmatic component of energetic particles in our solar system.

REFERENCES AND NOTES1. ANU RAD HA is the Sanskrit nam e of the star 6-Scorpii or a part of the constallation Scorpius.As cosm ic rays originate fr om som e typ e of stars in so me phase of their evolution, th e stellarname is given to the experiment .2. Hovestadt, D., Vollmer, O., Gloeckler, G., and Fan, C. Y .: Phys. Rev. Lett. , Vol. 31, 19 73 , p.65 . Ap. J . (Let ters) , Vol . 182, 1973,p. L81; Apl . J. , Vol. 202 , 1975, p. 265. McDonald, F. B., Teegarden, B. J. , Trainor , J . H., and

Webber, W. R.: Ap. J . , Vol. 187, 1974 , p. L105. Klecker, B., Hov estadt, D., Gloeckler, G., andFan, C. Y.: Ap. J., Vol. 212, 1977, p. 290, and references therein.

Garcia-Munoz, M., Mason, G. M., and Simpson, J. A.:

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3.

4.

5.

6,

7.

Cummings, A. C., Stone , E. C., and Webber, W. R.: Proc. 19th Int . Cosmic Ray Conf. , Vol . 5,19 85, p. 163. Mewaldt, R. E. and Sto ne, E. C.: Ibid, Vol. 5 , 198 5, p. 167 . Mason, G. A.,Klecker, B., Galvin, A. B., Hovestadt, D., and Ipavich, F. M.: Ibid, Vol. 5, 1985 , p. 168.Webber, W. R., Cummings, A. C., and Stone, E. C.: Ibid, Vol. 5 , 1985 , p. 1 72. McKibben, R. B.,Pyle, K. R., and Simps on, J. A.: Ibid , Vol. 5, 198 5, p. 1 98 .Biswas, S., Durgaprasad, N., Nevatia, J., Venkatavaradan, V. S., Goswami, J . N., Jayanthi, U. B.,Lal, D., and Mattoo, S. K . : Astrophys. Sp. Sci., Vol. 35 , 1 975 , p. 33 7.Biswas, S. and Durgaprasad, N.:N., and Trivedi, S .:and Ramaty, R. :Swordy, S. P.: Nature , Vol. 279 , 1 979 , p. 622.

Sp. Sci. Rev., Vol. 25, 198 0, p. 28 5. Biswas, S ., Durgaprasad,Fisk, L. A., Kozlovosky, B.,Fowler, P. H., Redfern, R. M., andProc. Ind. Acad. Sci., Vol. 90 , 1 981 , p. 33 7.Ap. J. (Let ters) , Vol . 190, 1 974, p. L35.

McKibben, R. B., Pyle, K. R., and Simpson, J. A.: Ap. J. , Vol. 227 , 1979, p. L14 7. Hov estadt,D., Klecker, B., Gloeckler, G., Ipavich, F. M., Fan, C. Y ., and Fisk, L. A. : Proc. 16 th Int . CosmicRay Conf., Kyoto, Vol. 3, 1979 , p. 255.Fleischer, R. L., Price, P. B., and W alker, R. M.: Nu clear Tra cks in Solids: Principles an d Ap pli-cations. Univ. of California Press, 197 5. Henke, R. P., and Benton, E. V.: Nuclear Inst. andMethod s, Vol. 97 , 19 71, p. 483.

ACKNOWLEDGMENTSWe are extremely thankful to Indian Space Research Organization Satellite Centre (ISAC),Bangalore, for their excellent support in conducting various integrations and testings of IONS; to BhabhaAtomic Research Centre (BARC), Bombay, for fabrication of the flight and flight spare IONS structure;Laser Laboratory of BARC for providing laser operations; and Variable Energy Cyclotron Centre (VEC),

Calcu tta, for providing support for the alpha beam exposures. We are grateful to NASA for providingus with the Spacelab-3 flight aboard the Shuttle Challenger and the Mission Specialists, Dr. Don Lind andDr. Norman Thaggard, for inflight replacement of a faulty cable, as well as NASA ground engineers forground support and help in reactivation of IONS during the flight.

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Figure 1. IONS payload flown in Space Shuttle Spacelab-3. In actual flight the payload waswrapped o n i ts side by a thermal blan ket for maintaining appropriate thermal environmentand was placed on the open cargo bay on a special ly mounted experiment supportstructure. Th e pressure inside the payload was maintained a t 0.1 atm. dur ing thefl ight with th e help of pressure senitive venting valves fixed on the wall of the

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N 8 7 - 22112ANIMA L STUDIES ON SPACELAB-3

C. Schatte, R. Grindeland, P. Callahan, and W . BerryNASA Ames R esearch Center, Moffett Field, California 94035G. Funk and W. Lencki

MATSCO, Valley Forge, Pennsylvania

ABSTRACTThe flight of the two squirrel monkeys and 24 rats on Spacelab-3 was the first mission to providehands-on mainte nance of animals in a laboratory environment. With few exceptions, the animals grewand behaved normally, were free of ch ronic stress, and differed from groun d con trols only for gravity-depen dent parameters. One of th e monkey s exhibited symp toms of space sickness similar to thoseobserved in hum ans, which suggests squirrel monkeys m ay be good m odels fo r studying the space-adaptat ion syndrome. Among the wide variety of parameters measured in the rats, most notable was the

dram atic loss of muscle mass and increased fragility of long bones. Oth er interesting rat findings werethose of suppressed interferom produc tion by spleen cells, defective release of grow th normo ne by soma-trophs, possible dissociation of circadian pacemakers, changes in hepatic lipid and carb ohy drate metabo-lism, and hypersensitivity of marrow cells to erythropoietin. These results portend a strong role foranimals in identifying and elucidating the physiological and anatomical responses of mammals to micro-gravity.

INTRODUCTIONWith the flight of two squirrel monkeys and 24 rats on Spacelab-3 (SL-3), NASA under took th efirst of several missions using animals in a role for which they have long been used in research on Earth

- as a model mammalian system with which to delineate the fundamental mechanisms of physiologicalresponse to an env ironm ent; i.e., microgravity. The prima ry objective of SL-3 was to evaluate the abilityof the Research Animal Holding Facility (RAHF) to maintain animals in a normal, laboratory environ-men t in space. It is impo rtant to use an anima l that grows normally, behaves normally, and is free fromchronic stress because most of the experimental measurements of interest in space are compromised bya subject w hich doe s not meet these requirements. Onc e these criteria are met, a high-quality experi-mental animal can then be provided for doing high-quality experiments on fut ure missions. Beyond thisprimary objective, SL-3 did provide the opportunity to obtain preliminary data on animal health andwell being in flight as well as to sample selected physiological parameters which might be the focus offuture f l ight experiments.

FLIG HT OPERATIONSThe RAHF is a controlled-environment animal-housing facility, the physical specification andoperation of which has been previously described [ 1 3 . The RAHF has two interchangeable modules ofseparate cages that can house up to four squirrel monkeys or 24 rats. Food and water consumption,activi ty, and interm ittent photographic records are obtained automatically. Temperature, humidity, andlight cycles can be controlled or varied as desired.

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Two adult male squirrel monkeys, free of antibodies to Herpes saimiri, were flown unrestrained.The ra ts comprised two group s of 12 males each. One group was adults abo ut 12 weeks old; theselarge rats represented the more ma ture, slower-growing organism. Th e other group was juveniles ab out8 weeks ol d; these small rats represented t he younge r, faster-growing organism. Fo ur of the large ratswere implanted with a transmitter w hich permitted the c ontinuous monitoring of heat ra te and deepbodytempe rature. Both mo nke ys and rats were free of several specific pathogens, but were not gnotob ioticor axenic.

The flight animals spent 1 day in the Spacelab prior to launch and 7 days in microgravity and,because of an altered landing site, 6 hours in a jet flight during the return to Kennedy Space Center.Apart from a brief physical examination at 3 hours postflight, data collection could not begin until about12 hours af ter landing. The squirrel mon keys were not tested postflight, whereas the rats were sacrificedfor a thorough examination, Ground-control rats in cages similar to those in the R AH F (simulationcontrols) and ground con trols in stand ard vivarium cages were also processed postflight. The ground-control groups could no t be subjected to th e postlanding jet f l ight , but w ere otherwise handled in exactlythe same manner as were the flight rats.

RESULTSUpon completion of the examination of the animals, the following results were recorded.

Squirrel MonkeysBoth squirrel monkeys ate less food, and were less active in space than on the ground (Table 1).Weight loss during the flight was within normal limits (


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of vivarium control animals at the end of the mission. The w eights of various organs (brain, hea rt,kidney, liver, adrenals, pituitary, spleen, prostate, thymus, parotid, and testes) in flight animals wereeithe r no t differ ent from simulation-cage control animals or w ithin normal limitts of variat ion [3 ]. Inparticular, indications of chronic stress (adrenal hypertrophy, thymic involution, parotid hyperplasia,and liver atro phy ) were no t observed in eithr group (data not shown). We conclud ed tha t the flightanimals grew at a normal rate and that growth-related symptoms of chronic stress were not evident.Hematology, Immunology, and Blood Chemistry

Hematological indices (Table 3) showed increased hematocrit, red-cell count, and hemoglobin inbot h groups. Because plasma volume could not be measured, it is unclear wheth er these changes resultedfrom increased erythropoiesis or hemoconc entration. How ever, postflight studies with cultured bone-marrow cells showed that marrow sensitivity to erythropoietin was heightened in the flight animals(Table 4). Prod uctio n of interferon-y by spleen cells cultured postflight was dramatically reduced inflight animals (Table 4). Among several plasma-hormones and blood-cell parameters measured postflight,only plasma co nce ntratio ns of osteocalcin were significantly lower in flight rats (Tab le 5 ) . However, itis likely th at mea surem ent of these relatively labile parameters was compromised by the 12-hour hiatusbetween landing and sample acquisition. We believe tha t these m easurements, more than the others, areless reflective of any changes which might have occurred during flight.Heart Rate and Body Temperature

The composite 24-hr heart rate for four rats over the 7-day flight was compared to their heartrate for a similar preflight period. Heart rate was lower in flight at all times of the day, and in particu-lar did not show the increase normally observed during the active period [9]. The period of the rhythmin flight was unchanged from that of preflight (23.9 k 0.02 hours).Mean body temperature was not affected by the flight, but the period of its rhythm was increasedto 24 .4 k 0.3 hours. The finding suggests the possibility tha t microgravity might cause the body-tem pera-

ture rhy thm to become free-running. If so, it might then dissociate from that of heart rate, which didnot show an indication of becoming free-running.Muscle

Both large and small flight rats had reduced mass of selected hind-limb extensor and flexormuscles postflight (Table 6) when compared to similar con trol rats. The two groups differed in tha t thelarge c ontro l rats lost muscle mass from their preflight values, w hereas most of the muscles in the smallcon trol animals showed som e grow th despite the obvious cage effect. In view of this, the muscle massloss in flight was more pronounced for the small, faster-growing rats than for the more mature, slower-growing ones. The antigravity s oleus muscle was the mo st sensitive to micrograv ity, with th e less-gravity-dependent tibialis anterior the least.

Histochemical and morphological analyses [ l o ] showed that loss of mass was apparently due tocell shrinkage rathe r tha n necrosis. However, about 1 percent of flight fibers were necrotic and u p to70 percen t of solei fibers had core lesions. Diaminopeptidase activity was unchanged, but b oth tri-aminopeptidase and Ca-activated protease activity were substantially increased in flight muscles. A decreasein mitochondrial NADH dehydrogenase activity, a marker of aerobic metabolism, coupled with increasedglycerophosphate dehydrogenase, a marker of glycolysis, suggested a shift from aerobic to glycolyticmetabolism in flight muscles. Fast fiber type s appeared more num erous in flight than in control soleiand fast myofibrilliar ATPase activity was elevated in flight muscles.

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Biochemical analyses of muscles (Table 7) f rom small animals showed tha t loss of protein, proba-bly from myofibrils, corresponded to loss of muscle mass. Tyrosine con tent, an indicator of proteincatabolism, was elevated only in small solei while the ratio of glutamine to glutamate, another suchindic ator w as increased in mo st of th e flight muscles. Glyc ogen dep ositio n was observed in all flightmuscles, suggesting a system ic effect apa rt from differences in muscle mass changes or me tabolic changesspecific to the individual muscles.Bone

Growth of tibial plates from small rats was reduced in flight (Table 8) and the effect wasconsistent in all three zones of the plates. Using two injections of calcein as a marker, the rate of perio-steal bone formation in the tibial diaphyses of large rats was 66 percent of preflight values for flight ratswhen com pared to simulation cage control rats [1 4] . There were no differences between fl ight andcon trol proxima l humerus of large rats for the following parameters: percent trabecular bone volume,percent osteoclast surface, percent osteoblast surface, number of osteoblasts for osteoclasts per millime-ter, and longitudinal bone growth [ 141. There was a substantial increase in fragility based on biome-chanical measurem ents (Table 9). This increased fragility occurre d despite the fact that the re were nodifferences in calcium, phosphorus, o r hydroxy proline co nten t of either trabecular or cort ical bone [8 ,151. But in the absence of gross demineralization of long bones, gradient-density analysis show ed tha tthere was a shift in mineral con centration from lower specific-gravity fra ctions (1.3-1.7, 1.8-1.9) towa rdhigher-density fractions (2.0-2.1, 2.2-2.9 ) in th e flight bon es [ 151. Histochemical analyses of osteoblastsand osteoclasts showed no difference between flight and control animals for the following parameters:alkaline and acid phosphatases, golgi activity, secretory granule size, dipeptidal peptidase, and lysosomalactivities [ 161 .

Vertebral bone differed somewhat from long bones in that mass was decreased in the absence ofdemineralization (Table 10). Of particular interest was the fa ct tha t bon e osteocalcin conc entra tion waslower in flight animals. There was no differenc e betw een flight and con trol vertebrae of small or largerats for the following parameters: percen t trabecular bone volume, percen t osteoblast or osteoclastsurface, osteoblasts or osteoclasts per millimeter of bone , and longitudinal bone grow th.Growth Hormone

Culture of pi tui tary soma totrophs [ 171 showed that the number of somatotrophs was increasedand that their growth hormone content was higher in flight rats (Table 11). However, when growthhormones are implanted into hypophysectomized rats, release of hormone from flight cells was decreasedas indicated by tibial grow th. This appare nt defect in the release of growth horm one thu s caused totalsynthesis by somatotrophs from flight rats t o be substantial ly lower than tha t in co ntrol rats. There wasno difference in hormone species between flight and con trol animals. If grow th horm one release wasreduced during flight, it might have caused some of the changes in muscle and bone previously observed.Liver Metabolism

Flight animals apparently had an increase in carbohydrate-based metabolism, suggested by the20-fold increas e in glycogen con ten t, and a decrease in lipid-based metab olism , as suggested by thedecreased cholesterol con tent (Table 12). The latte r may have resulted from the decrease in activity ofHM GC oA reductase, which is the rate-limiting ste p in cholesterol synthesis. While sphingomyelin conte ntwas no t different, the rate-limiting enzym e f or sphingolipid synthesis, serine palmitoyl transferase , waslower in flight animals. The absence of any differences for the amin o transferases suggests tha t theabsence of whole-body catabolic activity and that protein catabolism which occurred in specific organs

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(e.g., m uscle) was isolated t o tho se organs.lating glycocorticoids.stress in the flight animals.Tyrosine am inotransferas e is particularly sensitive to circu-

The lack of an increase in its activity is a further indication of mininal chronic

Other ObservationsElectron microscopic analysis of otoconia showed no degeneration of macular cells or demineral-

ization of otoconia1 masses in flight rats [201. Neurohistochemistry indicated no increase in cytoch romeoxidase activity in the paraven tricular nucleus, the site of co ntrol of fluid balance [2 13. An extensiveanalysis of receptor binding in various parts of the brain (hippocampus, prefrontal cortex, lateral f rontalcortex, posterior cortex, amygdala, pons-medulla, and cerebellum) showed only an increase in hippocam-pal binding for 5-hydroxytryptamine (5HT) [221. However, me mb rane Mg-dependent NA-K ATPaseactivity was lower in flight rats.

There was no change in kidney receptor aff ini ty for 1, 25-0H)2 Vitamin D3, suggest ing that thekidney was no t th e si te of con trol of any changes in calcium ex cret ion [2 3] . Histomorphological analysisof cardiac muscle showed increased glycogen and lipid deposition in flight rats and loss of microtubulesas compared to controls [ 241. Histoch em ical and mo rpho logical analyses of parotid salivary glandshowed no hyperplasia or major enzyme changes indicative of chronic discharge of the sympathet icnervous system [25 .

CONCLUSIONSThe data presented in th e previous sect ions indicate tha t the R AHF was able to maintain bo thrats and mo nke ys in a relatively norm al condition suitable for their use as expe rimen tal animals. Gro wth

parameters and several indices of chronic stress suggested that changes in bone and muscle were a resultof exposure to microgravity per se and no t an artifact resulting from adverse housing conditions. Fo r themost par t , changes in hematology, muscle, and bone were qualitatively similar to those reported inhumans and in animals from th e Kosmos f l ights of the Soviet Union. However, i t is apparent that micro-gravity induces a wide range of physiological changes, some of which have not been measured heretofore.Fu rth er evaluation of th ese parameters will require m ore flight experim ents, including collection ofsamples in flight to eliminate the complications resulting from delayed p ostflight sampling.

REFERENCES1.

2.

3.

4.

5.

Callahan, P. X., e t al.,: Am es Research Center Life Sciences Pay load Project for Spacela b Mission3, SAE Technical Paper No. 831094, 1983.Fuller, C. A. :Physiologist, Vol. 28, No. 6, in press, 1985.

Early Adaptation to Altered Gravitational Environments in the Squirrel Monkey.

Grindeland, R. E., et al.:Microg ravity. Physiologist, Vol. 28 , No. 6, in press, 1985.Rodent Body, Organ and Muscle Weight Responses to Seven Days of

Lange, R. D., et al.:N o. 6, in press, 1985.Hem atologic Parameters of Astro rats Flow n on SL-3. Physiologist, Vol. 28,

Gould, C. L., et al.: Effect of Flight in Mission SL-3 on Interferon-Gamm a Production by Rats.Physiologist, Vol. 2 8, No. 6, in press, 1985.79


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6.

7 .

8.

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12.13.

14.

15.

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20.

21.

22.

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Inge, W. H. and Hartle, D. K.:NASA Spacelab (SL-3) for Seven Days. Phy siologist, Vol. 28, No. 6, in press, 1985.Hartle, D. K. and Inge, W. H.:Days Aboard NASA Spacelab 8. Physiologist, Vol. 28 , No. 6, in press, 1985 .Patterson-Buckendahl, R. E., et al.: Osteocalcin as an Indicator of Bone Metabolism DuringSpaceflight. Physiologist, Vol. 28, No. 6, in press, 1985 .Fuller, C. A. :Vol. 28, No. 6, in press, 1985.Riley, D. A., et al.: Morphological and B iochemical Changes in So leus and Exten sor DigitorumLongus Muscles of Rats Orbited in Spacelab 3. Physiologist, Vol. 28, No. 6, in press, 1985.Tischler, M. E., et al.: Responses of Am ino Acids in Hindl imb Muscles to Recovery from Hypo-gravity and Unloading by Tail-Cast Suspension. Physiologist, Vol. 28, No. 6, in press, 1985.

Henriksen, E. J., et al .: Muscle Protein and Glycogen Responses to Recovery from Hypogravi tyand U nloading by Tail-Cast Suspension. Physiologist, Vol. 28 , No. 6, in press, 1985 .Duke, J. , et al. : Microprobe Analysis of Epiphyseal Plates from Spacelab 3 Rats. Physiologist,Vol. 28, No. 6, in press, 1985.Wronski, T. J. , et al . :No. 6, in press, 1985.Russell, J. E. and Simmons, D. J. : Bone Maturat ion in Rats Flown on the Spacelab 3 Mission.Physiologist, Vol. 28, No. 6, in press, 1985.D ot y , S. B.: Morphologic and Histochemical Studies of Bone Cells from SL-3 Rats. Physiologist,Vol. 28, No. 6, in press, 1985.Hymer, W. C. , et al . :Prepared from R ats Flown o n Spacelab 3. Physiologist, Vol. 28, No. 6, in press, 1985.Hargrove, J. L. and Jones, D. P. : Hepat ic Enzym e Adaptat ion in Rats After Spaceflight. Physio-logist, Vol. 28, No. 6, in press, 1985.Merrill, A. H., et al . :from Spacelab 3. Physiologist, Vol. 28, No. 6 , in press, 1 985.Ross, M. D., et al.:in press, 1985.Murakam i, D. M., et al.: Changes in Fun ctional M etabolism in the Rat Ce ntral Nervous SystemFollow ing Spaceflight. Physiologist, Vol. 28, No. 6, in press, 1985.Miller, J. D., et al.: Effe cts of Weightlessness in Neurotransmitter Receptors in Selected BrainAreas. Physiologist, Vol. 28, No. 6, in press, 19 85 .

Atr iopept in (AP-3) in A tr ia and Plasma of Rats Orbi ted Aboard

Plasma Renin Concentrations (PRC) of Rats Orbited for Seven

Homeostasis and Biological Rhythms in the Rat During Spaceflight. Physiologist,

Histomorphometr ic Analysis of the Rat Skeleton. Physiologist, Vol. 28,

Microgravity Associated Changes in Pituitary Growth Hormone (GH) Cells

Hep atic Enzym es of Sp hingolipid and Glycerolipid Biosynthesis in Rats

Otoconia1 Morphology in Space-Flown Rats. Physiologist, Vol. 28, No. 6,


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23. Manglesdorf, D. J . , et a l . :Control R at Kidneys. Physiologist, Vol. 28, No. 6, in press, 1985.1,25-dihydroxy-vitamin D 3 Rec eptors in Space-Flown Versus Grou nded

24. Philp ott, D. E., e t al.: Microgravity Changes in Heart Str uctu re and Cyclic-AM P Metabolism.Physiologist, Vol. 28, No. 6, in press, 1985.25 . Mednieks, M. 1. and Hand, A. R.: Biochemical and Morphological Evaluation of the Effects of

Spaceflight on R at Salivary Glands. Physiologist, Vol. 28, No. 6, in press, 1985.

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Table 1 . Food consumptsquirrel monkeys.ion and weight change Of Table 4. Interferon-gamma production by culturedspleen cells (Ref. 5) and sensltivity of bone-narrow cultures to erythropoietin (Ref. 4) in

FOOD CONSUMPIION A C T I V I T Y rats.-m311 Yd2 618z YO2 20 I 1

44 !mUL w110. SPLEENS PRODUCING I N l t H F L R O N - I 1 7 1 1 0 1110*

NO . SANPLES

EONE E R I I H R O I D C O L O N I E S 1 1 U 5 C E L L SDAY 3 , .0 2 U E P / M L 2 . 6 7 f. 2 . 1 3 ' 2 2 . 7 z 2 . 5 4 '

1 . 61 f. 2.89 32 .8 L 7 . 3 2 '.583 f ,319 4.06 1 1 . 6 8 '1 .83 f . 4 3 d.67 f. 3.U4'

1.0 U EPIMLDAY 6, .02 U E P 1 M L

1.0 u E P m

Table 2. Ueight change of rats (Ref. 3 ) .BbIz

'LA"P H E F L I G H T 200.1 : .5" 3 n 2 . 3 2 6. 5F L 1 6 H T 2 4 2 . 9 f. 3 . 1 3 8 5 . 9 :.6'C O N TR O L ( S I MU LA I IO U C AGE) 258 .2 : .1 4 0 0 . 8 t. 7. 8C O N I Y O L ( V I V A R I U n C A G E ) 301.d f. 5.0' 433.0 f .0 '

Table 3. Hematology of rats (Ref. 4 )

H EMAIO C R I I , 1R e t . I O % Lne. G ~ O L

J K V . FLMH. PGMCHC. 6 IOLYYC. 1 0 9 1 ~D IF F ER EN T IAL , I

L w n o c Y T E sMONOCYTESEO S N OPH l LSYEU lR O Pn lLS

40.7 I .50'5.85 f zn1 3 . 5 f .5

b9.lO f 2 . N23.10 f 1.02

7 . 8 9 f 2. 033.10 : 55

8 Y . 5 f 2.01.2 f 0. 90.9 f. 0. 78.2 f. 4.3

43.6 f . 3 U '6.46 : 40814 .7 f. .60n

6 7 . 8 0 f 3 . 5 02 2 . 8 : .227 . 8 8 f 1.833 . 6 f. 1 .51

77.8 f (1.4'

19.1 f 7.Y'1.6 f. 1.10.9 f 1.0

10 DIFFERENCE F O R SPLEEN CELL OR BONE MARROW DIF FER ENT IAL COUNTS" i s . r . 1 . m - 12' . O U l

Table 5. Plasma measuremenand 6-8).P

C AL CIU M, W D L 1 2PHOSPHORUS, MG/DL 12C R E A I I I NE, MG/nL I2ALKAL IN E PH O SPH AT ASE. I U I L 12O ST EO C ALC IY, N G IML 6I , 25 - DIHYDROXY V I I . D 3, P G I n L 6C O R T IC O ST ER O N E. U G lO L 6I H I R O X I N , U G ID L I 2I R I D D O T H I R O Y I N E , N G l D L I2GROWTH H O R M O N E , UGIML 12PR O LAC T IN . U G I M L 12ER YT H R O PO IET IN , N MIR L 6A I R I O P E P T I U , U G / N L 6R E N I N , NG/I(L b

' f S.E.".P [ . U 1 O R L E S S

t3 in rats

i.lLmlm9 . 9 8 f. .64'10.9 f. .4 41 . 1 2 t. .I6

191 f. I 23 4 7 t. 12

64 2 6 . 21 7 . 0 f. 3.07 9 . 1 f 8 . 8

7. 5 : . 92. 8 t. U.Y

19.0 f 3. 72.80 f .4 84 4 . 2 f. 7 .3

8. n f 0.9

(Ref. 3, 4,ELuu

3.00 f. . I 610.1 t. .2 61.02 f .04212 f. 1 92 7 1 f 25 '

9 4 f. I71 7 . 7 f. 4.49. 1 f 1. 0

7 2 . 6 f 6.17 . 2 t 5.15. 5 f 6. 1

1 6 . 5 f. 4.62.00 f .6 73 5 . 6 f. 6.b

Table 6.rats expressed a3 percentage of preflight Values(Ref. 3 ) .

Muscle weights (C/lOO C body weight) Of

lpdlLBpl EuGn[SEML

SOLEUS 0.0" -32.5'GASTROCNEll lUS * 1 . 9 - 9. 7. .7 -10.6'L A N T A R I ST I B I A L I S A Y I E R I O R * 1.u - 4.6EXTENSOR DIGITORUM LONGUS * 4. 5 - b.8'ADDUCIOR LONGUS - 4 . 3 0.08SOLEUS - 2 . 2 -2u.u 'P L A N T A H I S - 6. 0 -IZ.OB

wGASTROCUEMIUS - 4. 4 -13 . ' ) 'TISI A t S A N T E R I O R - 6 . 0 -11.uEXTENSOR D IG I IO R U M LO N G U S - 4. 2 -10.6'AOUUCTOR LONGUS' - 1 5 . 3 -15.3

A M E A 8 r E l G l 1 l ~ U G B O O T * E I G H l E XP R E S S ED A S P E R C E N l A G C H A M G E F U O RP R E F L I G n l , M-IYP .0 5 on L E S SP n e r L i t M r V A L U E S u * u s u * L L . ~ H I G H


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Table 7. Biochemical measurements in muscles ofsmall rats expressed as percentage of control(Refs. 1 1 and 12).saEK

P R O T E I N - 34*GI. I C 0 6 t N .I44I Y R O h l N E + 37; L U lR I I I NE - 2 u;LuT anA iE - 26H b I I O i L N / S L U 19RSPAI( IA1E t - 77PSPAI I I A I I I NEH A L A I L - b 041 RNINE - 21

liAs.wL-. 95- 206I S '

* 46NS

- 34NS

F l A n u l U+ 617

YS- 24- 4 2* 2 9- I 1

YSYS

- I ?+ 63

NS- 21- 2 6

YSISNSNS

- 6f 53

NSNS- 4 2f 39

YSNSNS

Table 10. Analyses on vertebra L3 of s d l ats(Ref. 8).rpdlIBpL ELlGiiI

DR Y I E I G H I , RG/G BODY WEIGHTCALCIUM. UGIRG BONE 110 f 3 I79 f 3. 7OSTEOCALCIY. UG/RG BUY 2 . 4 3 f I 1 2 .19 f 22 '

,354 f ,009. .3I8 f O M '

Table 1 1 . Analyses of cultured pituitarysomatotrophs (Ref. 17).

Table 8.plates of small rats (magnification inparentheses) (Ref. 13).Height in millimeters of tibial-grouth

TOTAL R E S I I W 6 PR O LIF ER AT IVE H YPER T R O PH IC 1U U w L A -

- 1.30 f .67 f 82 f 1 . 2 2CUNTHGl 59.15" 10.08 16.76 33.19i i l G H : 5 0 . 5 9 ' 9.04' 1 5 . 4 2 ' 2s . a2 '

-1 .55 f .60 f .78 f 1.47

Table 9. Biomechanical measurements on humeri ofsmall rats (Ref. 8 ) .i.k.uuu w

~L~IUAIE L OAD , N E W T O N S 41.5 f 1.54' 2 9 . 8 : .76'U L T I M A T E U t F O R M A T I O N , 114 , 6 7 7 f .017 . 5 7 5 2 . 0 3 9WORK IO U L I I I I A I E L O A D , Y/MR 16.1 f .d 1 8.86 2 1.18'I N I I I A L S T IF F NE S S , N l l l l l 95.4 f 5.57 1 0 . 5 2 4.08'

' i 5 S . E . l . . M - 6' F t l G M l O I F F E I I L M I FnOM CONIROL AT P ' ,001 O n L I S 5

mLLI S O I I A T O T R O P H S / P I T U I T A RYI P Y L C E L L S / P I l U l l A W YW6 STH/103 SO R AIO T R O PH SWG S I H R ELEASED 11O 3 SO MAIO T R O PH SNET S Y W l H E S I S / 6 DAYS. Y G / S T H / I 0 3

SORAIOTROPHSu

I S O R A l O l R O P H S / P I U I T A R YI P R L C E L L S / P I I U I T A R YNG S l H / 1 U 3 SU MAIO T R O PH SNG S I H R E L E A S E W l U ' S O I I A I O I R O P H SNET S Y N T H E S I S 1 6 D A Y S , N6/103

S O N A I O I R O P H S

: NLY. M - (1a P ' .05 on L E S S

42.533 .521.690.0108.6

36.13 7 . 636.9126.454.6

44.03 1 . 8

60 .7 '3 3 . 3 0IS. 3'

4 1 . 7 '

94.5'41.9'

33.467 .1 '

Table 12. Biochemical analyses of liver fromsmall rats (Refs. 18 and 19) .LlwtQL u

LIVER U E I G H l . 6 11.1 f 0.3' 9.Y : .5n i c n o s o n A L PnorEin. n c i G LIVER 5.6 : . 3 '4.2 :.3'

24.5 :.8'L I C U G E Y , % IC L I V E RP H U S P I ( O L IP ID S . U R O L16 L IV tH 35.8 f 1. 5 12.3 2 1.7SP H I N6OL I I S, UMOLIG L I V E R 2.3 :.2P Y S U . N M L I I I 6 P(I0IEIN 1.38 : .23 1.11 : . J S "85 U.II f .IO U.62 f .32E w n E s

1.24 : Y8LHULtSTEROL, UIIOLlG LIVE R Y . 1 f 1.0 b.9 : .Y'

2. 6 :.2

L IG ASE, Y M L / I I l N l l G P l O l E l N 39.Y I 2 . U 5'4., :.b'SEMIYE r i L m i l o v L I R A W E R A S E . 29.0 f 2.1 17-4 12.1'P n o L m i n m PnoiEii

i n o L i n i i i t t G PROTEINP n o L m i w n r , Pnorc IN

G LIC ElU L- 3 - PH O SPH AlE A C I L I R A Y S F E I A S E . 1.06 f .IY 1.00 1 .2'4

HIIG-COA REDUCTASE, 8.6 : .1 1 . I f 0.3'l Y R U S I N E A M IN O lRANSFEllASE, ,021 : 007 ,026: OO Sl S P A R T A I E AIIINOIRAYSFERASE. I .5U : 24 1.49 : l YUUOLIIII N/RG PYO lE II

u n o L / I ( i w n G PRUIEINI I L U T A IW IU N E - S - IR A N S F E R A S E , 11.5 f 0 . 8 1 1 . 1 : . n

UIIULI I I INIMG PWO lE lNA i 2 I . L . ~ . . M - 6 8 P .us OR L E S S

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N 8 1 - 2 2 1 1 3AUTOGENIC-FEEDBACK TRAINING: A PREVENTIVE METHODFOR SPACE ADAPTATION SYNDROME

Patricia S . Cowings and Joseph C. SharpNASA Ames Research Center

William B . Toscano and Joe KamiyaUniversity of California at San FranciscoNeal E. MillerYale University

Th is is a report o n the progress made to date on the reduction of data for Space lab 3 Shuttle expe rime nt, No.3A FT 23. Four astronauts participated as subjects in this experime nt. Crewmen A and B served as treatment subjects(i .e ., received preflight training for control of their own motion sickness symptoms) and Crewm en C and D servedas controls (i .e., did not receive training). A preliminary evaluation of Autogenic Feedback Training (AFT) wasmade from visual inspections of graphs that were generated from the p reflight and inflight physiological data w hichincluded:a) Baseline rotating chair tests for all crewmen.b) Posttraining rotating chair tests of treatment groups subjects.c) Preflight data from Joint Integrated Simulations for all crewmen.d) Flight data for all crewmen during m ission days 0 through 4, nd mission day 6 for treatment subjectsonly.Skin temperature and acceleration data collected during the JIS and the SL-3 mission have not yet beenreduced and will be included in a later report.A summary of the findings suggested by these data is outlined below: The preflight training schedule givento treatmen t group subjects was, on av erage , 90 days longer than planned because of delays in the launch date. Thischange in th

spacelab 3 mission science review

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