A. D. Dolgov (Institute for Theoretical and Experimental Physics, Rencontres de Moriond: Electroweak Interactions and Unified (DE89-013150; FNAL/C-89/112-A; CONF-8903132-2) Avail: NTIS HC A03/MF A01 A review of the cosmological term problem is presented. Baby universe model and the compensating field model are discussed. The importance of more accurate data on the Hubble constant and the Universe age is stressed. N89-27615# Astronomicky Ustav. DOE Ceskoslovenska Akademie Ved, Ondrejov. DYNAMICS OF THE SOLAR SYSTEM: PROCEEDINGS, 1987 Milos Sidlichovsky, ed. 211 p Proceedings of the 10th European Regional Astronomy Meeting of the IAU, Prague, Czechoslovakia, 24-29 Aug. 1987 (DE89-609828; INIS-mf-11400-Vol-3; CONF-8708269-Vol-3; Publ-68-Vol-3) Avail: NTIS HC A10/MF A01 The conference proceedings contains a total of 31 papers of which 7 were not incoporated in INIS. The mathematical methods of calculating the movements of the planets, their satellites and asteroids in the solar system, and the mathematical modeling of the past development of the solar system are discussed. Great attention is also devoted to resonance in the solar system and to the study of many celestial bodies. Four papers are devoted to DOE planetary rings and three to modern astrometry. N89-27616# Astronomicky Ustav. Ceskoslovenska Akademie Ved, Ondrejov. EVOLUTION OF GALAXIES. PROCEEDINGS, VOLUME 4 (DE89-609850; INIS-mf-11401-Vol-4; CONF-8708269-Vol-4; The proceedings contain 87 papers divided into 8 chapters. The chapter Bipolar outflows and star formations contains papers on optical and infrared observations of young bipolar outflow objects and the theory thereof, and observations of cometary nebulae. The chapter Masers and early stellar evolution discusses molecular masers and star forming regions. The following chapter contains papers on initial mass function and star formation rates in galaxies. The chapter Clusters and star formation contains data on OB associations and open star clusters, their development, and observations, CO and H sub 2 in the galaxy, the four vector model of radio emission and an atlas of the wavelength dependence of ultraviolet extinction in the Galaxy. The most voluminous is the chapter Evolution of galaxies. It contains papers on the theories of the physical and chemocynamic development of galaxies of different types, rotation research and rotation velocities of galaxies and their arms, and mathematical and laboratory models of morphological development. Chapter seven contains papers dealing with active extragalactic objects, quasars, and active galactic nuclei. The last chapter discusses cosmological models, the theory of the inflationary universe, and presents an interpretation of the central void and X-ray background. DOE N89-27617# Rome Univ. (Italy). Dipartimento di Fisica. Prepared in cooperation with Academy of Sciences (USSR), (Preprint-598; ETN-89-94687) Avail: NTIS HC A02/MF A01 It is argued that magnetic moment of electron neutrino mu=10 to the minus 11th power muB is most likely to induce adiabatic resonant (i.e., complete) helicity flip of neutrino in the layer of the supernova core with density 10 to the 12th power g/cc. Therefore such a value of mu does not lead to an inconsistency with the observed neutrino events from the supernova SN1987a. The process proposed gives rise to a rapid energy transfer from the inner core to the outer layers which can explain the mechanism of blowing of the supernova's envelope. 91 LUNAR AND PLANETARY EXPLORATION ESA Includes planetology; and manned and unmanned flights. For spacecraft design or space stations see 18 Spacecraft Design, Testing and Performance. N89-27618# Los Alamos National Lab., NM. Earth and Space Sciences Div. CHARACTERIZATION OF LUNAR ILMENITE RESOURCES Grant Heiken and David T. Vaniman 1989 30 p Presented at the Lunar Planetary Science Conference, Houston, TX, 12 Mar. 1989 (Contract W-7405-eng-36) (DE89-013455; LA-UR-89-1793; CONF-8903111-3) Avail: NTIS HC A03/MF A01 Ilmenite will be an important lunar resource, to be used mainly for oxygen production but also as a source of iron. Ilmenite abundances in high-Ti basaltic lavas are higher (10 to 20 percent) than in high-Ti mare soils (mostly less than 10 percent). This factor alone may make crushed high-Ti basaltic lavas most attractive as a target for ilmenite extraction. Concentration of ilmenite from either a crushed basalt or regolith requires sizing to avoid polycrystalline fragments. In coarse-grained high-Ti basaltic lavas, about 60 to 80 percent of the ilmenite will consist of relatively clean single crystals if the rocks are crushed to a size of 0.2 mm. Fine-grained high-Ti basalts, with thin skeletal or hopper-shaped ilmenites, would produce essentially no free or clean ilmenite grains unless crushed to sizes of less than 0.15 mm, and only approximately 7 percent free ilmenite if crushed to sizes smaller than 0.05 mm. Data from the 2.8 m-thick regolith sampled by coring at the Apollo 17 site show that in even the most basalt-clast-rich and least mature stratigraphic intervals, free ilmenite grains make up less than 2 percent of the 0.02- to 0.2-mm size fraction and a mere 0.3 percent of the 0.2- to 2-mm size DOE fraction. N89-27619*# National Aeronautics and Space Administration. Lewis Research Center, Cleveland, OH. LUNAR PRODUCTION OF SOLAR CELLS Geoffrey A. Landis and Maria Antonietta Perino (Aeritalia S.p.A., Turin, Italy) May 1989 18 P Presented at the 9th Biennial SSI/Princeton Conference on Space Manufacturing, Princeton, NJ, 10-13 May 1989; sponsored by the Space Studies Inst. (NASA-TM-102102; E-4866; NAS 1.15:102102) Avail: NTIS HC A03/MF A01 CSCL 03B The feasibility of manufacturing of solar cells on the moon for spacecraft applications is examined. Because of the much lower escape velocity, there is a great advantage in lunar manufacture of solar cells compared to Earth manufacture. Silicon is abundant on the moon, and new refining methods allow it to be reduced and purified without extensive reliance on materials unavailable on the moon. Silicon and amorphous silicon solar cells could be manufactured on the moon for use in space. Concepts for the production of a baseline amorphous silicon cell are discussed, and specific power levels are calculated for cells designed for both lunar and Earth manufacture. N89-27620# Rome Univ. (Italy). Dipartimento di Fisica. 18 p Author In ITALIAN; ENGLISH SOLAR MICROWAVE RADIATION MAPS MEASURED AT 1988 (PB89-154876; SER-A-3; ISSN-0783-8751; ISBN-951-754-677-7) Avail: NTIS HC A05/MF A01 CSCL 03B The Metsaehovi Radio Research Station operates a 14 m diameter radio telescope. Annually the telescope has been reserved for solar measurements for 4 to 10 weeks, typically during summer months. Measurements include maps of the whole or part of the Sun, tracking of active regions and solar oscillation monitoring. Most of the solar maps have been measured using receivers operating at 22.2 GHz or at 36.8 GHz. The sensitivity of receivers is good enough for 0.2 sfu resolution. In the temperature scale the resolution is better than 100 K and it is limited by the changes of the atmospheric attenuation. The purpose of the report is to publish at least one map for each of the days when measurements were performed. For some of these days there exist several measured maps. The volume contains selected maps measured in 1982 and 1983. A list of all measured maps during this period is included. GRA Prepared in John M. Finn (Science Applications International Corp., McLean, VA.) and James Chen 27 Mar. 1989 70 P cooperation with Maryland Univ., College Park (AD-A207311; NRL-MR-6402) Avail: NTIS HC A04/MF A01 CSCL 03/2 Properties of two-dimensional straight (symmetric in z) magnetic arcade equilibria in the solar corona are studied within the framework of magnetohydrodynamics. Sequences of MHD equilibria are obtained by solving the Grad-Shafranov equation with the footprint displacement and the entropy prescribed. It is shown that no multiple solutions, or bifurcations, result. This is to be contrasted with the approach of prescribing the axial magnetic field Bz(psi) or pressure p(psi), in which bifurcations do occur. The physical conditions for which the footprint displacement or entropy, as opposed to Bz or p, must be specified are discussed. It is argued that these conditions are more likely to occur in the corona than those conditions under which Bz and p may be prescribed. The lack of bifurcations indicates that equilibrium will not be lost as the footprint displacement or entropy is increased. The limiting configurations for infinite footprint displacement and infinite entropy are also discussed. It is shown that although the current density does become somewhat peaked, the total current in the peak region decreases as the system is sheared (or heated). In fact, the current in this peak region contains a rapidly decreasing fraction of the total current so that the limiting configuration is not one in which the current is concentrated into a current sheet. GRA N89-27623* # National Aeronautics and Space Administration. Lewis Research Center, Cleveland, OH. SOLAR RADIATION ON MARS Aug. 1989 33 P Joseph Appelbaum and Dennis J. Flood Detailed information on solar radiation characteristics on Mars are necessary for effective design of future planned solar energy systems operating on the surface of Mars. Presented here is a procedure and solar radiation related data from which the diurnally, hourly and daily variation of the global, direct beam and diffuse insolation on Mars are calculated. The radiation data are based on measured optical depth of the Martian atmosphere derived from images taken of the sun with a special diode on the Viking cameras; and computation based on multiple wavelength and multiple scattering of the solar radiation. Author N89-27624# National Geophysical Data Center, Boulder, CO. SOLAR-GEOPHYSICAL DATA NUMBER 535, PART 1. DATA FOR FEBRUARY, JANUARY 1989, AND LATE DATA Prompt Reports, March 1989 Helen E. Coffey, ed. Mar. 1989 143 P (PB89-185987; SGD-535-Pt-1; LC-79-640375; ISSN-0038-0911) Avail: NTIS HC A07/MF A01 CSCL 03B Solar-geophysical information is presented in tabular and graphic form. Categories include detailed index for 1988 and 1989; data for February 1989 (advance and world-wide IUWDS alert periods, solar activity indices, solar flares, solar radio emission, Stanford mean solar magnetic field); data for January 1989 (solar active regions, sudden ionospheric disturbances, solar radio spectral observations, cosmic ray measurements by neutron monitor, geomagnetic indices, radio propagation indices); and late data (solar active regions -- H-alpha synoptic charts 1806 to 1808 (September-November 1988), cosmic ray measurements by neutron monitor Thule, December 1988, geomagnetic indices commencements/solar flare effects December 1988). sudden GRA N89-27625# National Geophysical Data Center, Boulder, CO. SOLAR-GEOPHYSICAL DATA NUMBER 535, PART 2. DATA FOR SEPTEMBER 1988, AND MISCELLANEOUS Comprehensive Reports, March 1989 Helen E. Coffey, ed. Mar. 1989 77 p (PB89-185995; SGD-535-Pt-2; LC-79-640375; ISSN-0038-0911) Avail: NTIS HC A05/MF A01 CSCL 03B Solar-geophysical information is presented in tabular and graphic form. Categories include a detailed index for 1988 and 1989; data for September 1988 (solar flares, solar radio bursts at fixed frequencies, solar X-ray radiation from GOES satellite, mass ejections from the sun, active prominences and filaments); and miscellaneous data (interplanetary solar wind data, IMP-8, February-November 1988. GRA 93 SPACE RADIATION Includes cosmic radiation; and inner and outer earth's radiation belts. For biological effects of radiation see 52 Aerospace Medicine. For theory see 73 Nuclear and High-Energy Physics. N89-27627# Sandia National Labs., Albuquerque, NM. DETECTION OF VERY HIGH ENERGY GAMMA-RAYS FROM THE CRAB NEBULA C. Akerlof, J. DiMarco, H. Levy, D. Meyer, P. Radusewicz, R. Tschirhart, Z. Yama, and C. MacCallum 28 Apr. 1989 9 p (Contracts DE-AC04-76DP-00789; DE-AC02-76ER-01112) During the period October 1988 through December 1988, a search was made for very high energy gamma rays from the direction of the Crab nebula using the atmospheric Cerenkov technique. The detector consisted of seven-fold arrays of photomultiplier tubes at the focii of two 11-meter diameter solar concentrators situated in Albuquerque, New Mexico. A dc signal was detected from the Crab nebula with a statistical significance of 5.8 sigma after the application of various cuts designed to suppress the background of hadronic showers. A search for a pulsed component failed to identify a significant signal in phase with the radio pulse from the Crab pulsar. These results, with a threshold energy of 200 GeV, are in substantial agreement with high energy results recently reported by the Mt. Hopkins group. DOE N89-27628# Los Alamos National Lab., NM. Space Astronomy and Astrophysics Group. SPECTRA OF CRAB-LIKE PULSARS: A GRO PERSPECTIVE Cheng Ho 1989 9 p Presented at the Gamma Ray Observatory Science Workshop, Greenbelt, MD, 10-13 Apr. 1989 (Contract W-31-109-eng-38) (DE89-013461; LA-UR-89-1760; CONF-8904216-2) Avail: NTIS HC A02/MF A01 A single-parameter model has been constructed to calculate the continuum spectrum of energetic pulsed radiation resulting from the formation of a Crab-type charge depletion region (gap) in the outer magnetosphere of rapidly spinning pulsars (Ho 1989). We discuss the characteristics of the theoretical predictions for the Crab pulsar and the specific features expected in the energy bands of the Gamma-Ray Observatory (GRO). These features include a possible spectral dip in the 0.3 to 30 MeV range, a change in polarization behavior below and above the dip, if polarization can be discerned, and most importantly, an exponential roll-over in the energy range necessary to detect the exponential roll-over. This model predicts that the 50 ms pulsar in the Large Magellanic Cloud (PSR0540-693) will be marginally detectable by GRO with a nominal two-week integration. Furthermore, we discuss the spectrum and detectability of a pulsar with 0.5 ms period and a surface magnetic field of 10(9) G. Such a pulsar may exist in SN 1987A. Since the 50 ms pulsar and SN 1987A are within the same field of view of GRO, it will be of great importance to take an extra long integration of this region to search for gamma-ray emission from these sources. DOE N89-27629*# Stanford Univ., CA. Center for Space Science and Astrophysics. Maximum Mission (SMM) during the maximum of the 21st solar cycle (circa 1980) are analyzed in order to study their statistical correlation with type 3 bursts. The earlier finding by Kane (1981) are confirmed qualitatively that flares with stronger hard X-ray emission, especially those with harder spectra, are more likely to produce a type 3 burst. The observed distribution of hard X-ray and type 3 events and their correlations are shown to be satisfactorily described by a bivariate distribution consistent with the assumption of statistical linear dependence of X-ray and radio burst intensities. From this analysis it was determined that the distribution of the ratio of X-ray intensity (in counts/s) to type 3 intensity (in solar flux units) which has a wide range and a typical value for this ratio of about 10. The implications of the results for impulsive phase models are discussed. N89-27630# Dept. Author Lawrence Livermore National Lab., CA. Physics USE OF THE EGRET (ENERGETIC GAMMA-RAY EXPERIMENT TELESCOPE) IN STUDIES OF THE ORIGIN OF THE COSMIC RADIATION Charles D. Dermer 19 May 1989 9 p Presented at the Gamma Ray Observatory Science Workshop, Greenbelt, MD, 10-12 Apr. 1989 (Contract W-7405-eng-48) (DE89-013785; UCRL-101129; CONF-8904216-4) Avail: NTIS HC A02/MF A01 The Energetic Gamma-Ray Telescope (EGRET) onboard the Gamma Ray Observatory will provide the first detailed map of the galaxy showing both intensity and spectral variations at greater than 20 MeV gamma-ray energies. Possible reasons for gamma-ray spectral variations are considered under the hypothesis that point sources of cosmic rays exist. We show how the spectrum and intensity of cosmic rays in the vicinity of such objects can depend on propagation effects, injection conditions and model geometry DOE in a number of special cases. A01 In the framework of calibrating and monitoring the energy response of a high resolution electromagnetic calorimeter the different role played by electrons and muons is discussed. A set of relations between the signal amplitudes measured in cosmic ray events and the physical quantities entering in the energy determination is derived. The absolute light yield of the detector can be monitored by the ionization loss of muons of known momentum or by the average ionization of muons with the cosmic ray energy distribution. A method to determine this average ionization in a precise way, using noninteracting pions of known momentum is given. A system to correct the calibration constants for the effect of the variation of the optical properties of each detector element is outlined. It is stressed that precise knowledge of the ionization loss is crucial. This consideration led the L3 collaboration to measure the Bi4Ge3012 (BGO) ionization loss and verify the agreement with theoretical formulas at the percent level. 99 GENERAL ESA STATISTICAL STUDY OF THE CORRELATION OF HARD X-RAY AND TYPE 3 RADIO BURSTS IN SOLAR FLARES Russell J. Hamilton and Vahe Petrosian May 1989 Submitted for publication 39 p (Grants NSG-7092; NSF ATM-87-05084) (NASA-CR-185833; NAS 1.26:185833; CSSA-ASTRO-89-03) Avail: NTIS HC A03/MF A01 CSCL 03B A large number of hard X-ray events which were recorded by the Hard X-Ray Burst Spectrometer (HXRBS) on the Solar No abstracts in this category. WHAT YOU CAN DO FOR STAR All users of this abstract service are urged to forward reports to be considered for announcement in STAR. This will aid NASA in its efforts to provide the fullest possible coverage of all scientific and technical publications that might support aeronautics and space research and development. If you have prepared relevant reports (other than those that you will transmit to NASA, DOD, or DOE through the usual contract- or grant-reporting channels), please send them for consideration to the NASA Scientific and Technical Information Facility, P.O. Box 8757, BWI Airport, Maryland 21240. 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