(Grant NAG2-480) (NASA-CR-185388; NAS 1.26:185388; PCS-TR88-136) Avail: NTIS HC A03/MF A01 CSCL 05B The question of sharing of rights and information in the Take-Grant Protection Model is examined by concentrating on the similarities between the two; in order to do this, new theorems are stated and proven for each that specifically show the similarities. The proof for one of the original theorems is also provided. These statements of necessary and sufficient conditions are contrasted to illustrate the proposition that transferring rights and transferring information are fundamentally the same, as one would expect in a capability-based system. Directions are then discussed for future Author research in light of these results. N89-28447# Lawrence Livermore National Lab., CA. PROBLEMS AND SOLUTIONS IN ONLINE DOCUMENTATION SYSTEMS Jun. 1989 6 p Presented at the Cray User's Jean Shuler Group Conference, Los Angeles, CA, 24 Apr. 1989 (Contract W-7405-eng-48) (DE89-014092; UCRL-101237; CONF-8904210-7) Avail: NTIS HC A02/MF A01 Pogo says we are surrounded by insurmountable opportunities. DOCUMENT, the online document system at NMFECC, has been continually enhanced and modified in the past 12 years to meet customer needs by analyzing the insurmountable opportunities (commonly called problems) that have arisen. We have analyzed where these documentation retrieval problems exist and solved these problems. The greatest challenge was to provide the customer with a stable system using the existing database of documents while adding new features and programs to retrieve information. Listed are four of the problems we have encountered, solutions are given and some indicators of success are shown. DOE N89-27930 ANT Nachrichtentechnik, Backnang (Germany, F.R.). N89-28448*# Washington, DC. Management Information Services, Inc., THE PRIVATE SECTOR ECONOMIC AND EMPLOYMENT BENEFITS TO THE NATION AND TO EACH STATE OF PROPOSED FY 1990 NASA PROCUREMENT EXPENDITURES Apr. 1989 77 p Prepared for NASA Alumni League, Washington, DC (NASA-CR-185894; NAS 1.26:185894) Avail: NTIS HC A05/MF A01 CSCL 05C The private sector economic and employment benefits (disaggregated among 80 industries and 475 occupations) of the proposed FY 1990 NASA procurement expenditures to the nation and to each state are estimated. Nationwide, it is found that FY 1990 NASA procurement expenditures of $11.3 billion will have an economic multiplier of 2.1 and will create, directly and indirectly, 237,000 jobs, $23.2 billion in total industry sales, $2.4 billion in corporate profits, and $7.4 billion in Federal, state, and local government tax revenues. These benefits are widely dispersed throughout the United States and are significant in many states not normally considered to be major beneficiaries of NASA spending. The indirect economic benefits are identified for each state resulting from the second-, third-, and fourth rounds of industry purchases generated by NASA procurement expenditures. Each state is ranked on the basis of several criteria, including the total benefits, indirect benefits, and per capita benefits received from NASA spending. The estimates developed are important for maintaining a viable U.S. Space Program through the remainder of this century. 84 LAW, POLITICAL SCIENCE AND SPACE POLICY B.G. Includes NASA appropriation hearings; aviation law; space law and policy; international law; international cooperation; and patent policy. N89-28449# Army War Coll., Carlisle Barracks, PA. Raymond J. Dolan 7 Mar. 1989 45 p (AD-A207334) Avail: NTIS HC A03/MF A01 CSCL 22/2 Technological advances will have a significant impact on future crises. Decision making will become more difficult and complex as the amount of information available to decision makers and the public increases substantially. Photos from commercial satellites have just begun to have an effect on governments and their policies. The rapid increase in technology will provide capabilities to the news media that will profoundly affect the relationship among the media, military and national leaders. The old ways of doing business have changed. The launching of a media satellite is certain to raise many issues that must be addressed and solved. The media's use of their own satellite will generate conflicts between first amendment rights and U.S. national security and foreign policy interests. A mediasat will also affect military strategy and tactics. These issues are addressed in a hypothetical scenario in a generate awareness of potential problems and postulate some GRA solutions. N89-28450# (U.S. House). Committee on Science, Space and Technology 88 SPACE SCIENCES (GENERAL) THE 1990 NATIONAL AERONAUTICS AND SPACE 1989 69 p Hearing before the Subcommittee on Transportation, Aviation and Materials of the Committee on Science, Space and Technology, 100th Congress, 1st Session, no. 17, 26 Apr. 1989, volume 1 (GPO-99-550) Avail: Subcommittee on Transportation, Aviation and Materials, House of Representatives, Washington, D.C. 20515 SOD HC $2.25 Hearings before a subcommittee on transportation, aviation, and materials of the U.S. House of Representatives are presented for the fiscal year 1990 NASA aeronautics research and technology program are presented. All written testimony and submittals for the record are included. Justifications for research and development of high-speed air transportation are provided. B.G. Committee on Science and Technology (U.S. N89-28451# House). N89-28452# Army War Coll., Carlisle Barracks, PA. Neil W. Grotegut 28 Mar. 1989 39 p (AD-A207347) Avail: NTIS HC A03/MF A01 CSCL 05/1 The United States relies on the superior technology of its defense systems as a competitive edge against overwhelming Soviet numerical advantages. There is strong evidence to suggest that the U.S.S.R. is rapidly reducing the U.S. technology lead through the transfer and assimilation of technology gained from the West. The relevant issues of West to East technology transfer is examined in order to provide awareness and appreciation of its importance to the security of the U.S. GRA N89-28453# Lawrence Livermore National Lab., CA. E. Lafranchi Jun. 1988 313 p (DE89-014320; UCRL-53868-88) Avail: NTIS HC A14/MF A01 This annual report describes the accomplishments of the Engineering Research Program for fiscal year 1988. Sixty-seven research and development projects are covered. For each project, goal(s), technical description, and an overview of future work are provided. DOE INTERPLANETARY PARTICLE ENVIRONMENT. PROCEEDINGS OF A CONFERENCE 15 Apr. 1988 Joan Feynman, ed. and Stephen Gabriel, ed. (NASA-CR-185461; JPL-Publ-88-28; NAS 1.26:185461) Avail: A workshop entitled the Interplanetary Charged Particle Environment was held at the Jet Propulsion Laboratory (JPL) on March 16 and 17, 1987. The purpose of the Workshop was to define the environment that will be seen by spacecraft operating in the 1990s. It focused on those particles that are involved in single event upset, latch-up, total dose and displacement damage in spacecraft microelectronic parts. Several problems specific to Magellan were also discussed because of the sensitivity of some electronic parts to single-event phenomena. Scientists and engineers representing over a dozen institutions took part in the meeting. The workshop consisted of two major activities, reviews of the current state of knowledge and the formation of working groups and the drafting of their reports. For individual titles, see N89-28455 through N89-28470. TOWARD A DESCRIPTIVE MODEL OF GALACTIC COSMIC RAYS IN THE HELIOSPHERE C93 R. A. Mewaldt, A. C. Cummings, James H. Adams, Jr., Paul Researchers review the elements that enter into phenomenological models of the composition, energy spectra, and the spatial and temporal variations of galactic cosmic rays, including the so-called anomalous cosmic ray component. Starting from an existing model, designed to describe the behavior of cosmic rays in the near-Earth environment, researchers suggest possible updates and improvements to this model, and then propose a quantitative approach for extending such a model into other regions Author of the heliosphere. THE EFFECTS OF HIGH ENERGY PARTICLES ON Paul A. Robinson, Jr. In its Interplanetary Particle Environment. 15 Apr. 1988 CSCL 03B p 35-47 (For primary document see N89-28454 22-90) Avail: NTIS HC A08/MF A01 Researchers review the background and motivation for the detailed study of the variability and uncertainty of the particle environment from a space systems planning perspective. The engineering concern raised by each environment is emphasized rather than the underlying physics of the magnetosphere or the sun. Missions now being planned span the short term range of one to three years to periods over ten years. Thus the engineering interest is beginning to stretch over periods of several solar cycles. Coincidentally, detailed measurements of the environment are now becoming available over that period of time. Both short term and long term environmental predictions are needed for proper mission planning. Short term predictions, perhaps based on solar indices, real time observations, or short term systematics, are very useful in near term planning -- launches, EVAS (extravehicular activities), coordinated observations, and experiments which require the magnetosphere to be in a certain state. Long term predictions of both average and extreme conditions are essential to mission design. Engineering considerations are many times driven by the worst case environment. Knowledge of the average conditions and their variability allows trade-off studies to be made, implementation of designs which degrade gracefully under multi-stress environments. Author Avail: NTIS HC A08/MF A01 CSCL 03B The Cosmic Ray Effects on MicroElectronics (CREME) model that is currently in use to estimate single event effect rates in spacecraft is described. The CREME model provides a description of the radiation environment in interplanetary space near the orbit of the earth that contains no major deficiencies. The accuracy of the galactic cosmic ray model is limited by the uncertainties in solar modulation. The model for solar energetic particles could be improved by making use of all the data that has been collected on solar energetic particle events. There remain major uncertainties about the environment within the earth's magnetosphere, because of the uncertainties over the charge states of the heavy ions in the anomalous component and solar flares, and because of trapped heavy ions. The present CREME model is valid only at 1 AU, but it could be extended to other parts of the heliosphere. There is considerable data on the radiation environment from 0.2 to 35 AU in the ecliptic plane. This data could be used to extend the Author CREME model. N89-28459*# Pasadena. Jet Propulsion Lab., California Inst. of Tech., A NEW PROTON FLUENCE MODEL FOR E GREATER THAN 10 MeV c93 Joan Feynman, T. P. Armstrong, L. Dao-Gibner, and S. Silverman (Boston Coll., Chestnut Hill, MA.) In its Interplanetary Particle Environment. Proceedings of a Conference 15 Apr. 1988 p 58-71 (For primary document see N89-28454 22-90) (Grant NSF ATM-83-05537) Avail: NTIS HC A08/MF A01 CSCL 03B Researchers describe a new engineering model for the fluence of protons with energies greater than 10 MeV. The data set used is a combination of observations made primarily from the Earth's surface between 1956 and 1963 and observations made from spacecraft in the vicinity of Earth between 1963 and 1985. With this data set we find that the distinction between ordinary proton events and anomalously large proton events made in earlier work disappears. The greater than 10 MeV fluences at 1 AU calculated with the new model are about twice those expected on the basis of models now in use. In contrast to earlier models, results do Author not depend critically on the fluence from any one event. N89-28460*# Air Force Geophysics Lab., Hanscom AFB, MA. INTENSITY/TIME PROFILES OF SOLAR PARTICLE EVENTS AT ONE ASTRONOMICAL UNIT c92 M. A. Shea In Jet Propulsion Lab., California Inst. of Tech., Interplanetary Particle Environment. Proceedings of a Conference 15 Apr. 1988 p 75-84 (For primary document see N89-28454 22-90) Avail: NTIS HC A08/MF A01 CSCL 03B A description of the intensity-time profiles of solar proton events observed at the orbit of the earth is presented. The discussion, which includes descriptive figures, presents a general overview of the subject without the detailed mathematical description of the physical processes which usually accompany most reviews. Author N89-28462*# National Oceanic and Atmospheric Administration, Boulder, CO. SOLAR PROTON EVENT FORECASTS c92 G. R. Heckman In Jet Propulsion Lab., California Inst. of Tech., Interplanetary Particle Environment. Proceedings of a Conference 15 Apr. 1988 p 91-100 (For primary document see N89-28454 22-90) Avail: NTIS HC A08/MF A01 CSCL 03B The United States operates a space weather service to provide information on space hazards including solar proton events to Federal government agencies and other users who operate systems that are affected by disturbances in the upper atmosphere and interplanetary environment. The observation and prediction of solar proton events has been continuous through solar cycle 21 (1976 to 1986), establishing a base of experience that can be used in providing similar support to space operations in the 1990's. The observations, indices, alerts, and forecasts used in the service D. F. Smart In Jet Propulsion Lab., California Inst. of Tech., Interplanetary Particle Environment. Proceedings of a Conference 15 Apr. 1988 p 101-110 (For primary document see N89-28454 22-90) Avail: NTIS HC A08/MF A01 CSCL 03B A procedure has been developed to generate a computerized time-intensity profile of the solar proton intensity expected at the earth after the occurrence of a significant solar flare on the sun. This procedure is a combination of many pieces of independent research and theoretical results. Many of the concepts used were first reported by Smart and Shea (1979) and are summarized by Smart and Shea (1985). Extracts from the general procedure that relate to predicting the expected onset time and time of maximum at the earth after the occurrence of a solar flare are presented. HIGH-ENERGY PARTICLES VERY NEAR THE SUN Abstract Only c92 B. E. Goldstein In its Interplanetary Particle Environment. Proceedings of a Conference 15 Apr. 1988 p 117 (For primary document see N89-28454 22-90) Avail: NTIS HC A08/MF A01 CSCL 03B NASA's long range plans include a Solar Probe (Star Probe) mission in which a spacecraft is placed in an eccentric orbit with perihelion at four solar radii. As part of the study effort for this mission, a Solar Probe Environment Workshop was sponsored by JPL. The report of this committee was issued in September 1978 as JPL Publication 78-64. A brief abstract of this document is given. There are considerable uncertainties in the models of solar energetic particle release and transport. The committee addressed this problem by using different modelling techniques when possible to provide a cross-check on the estimates. These models were used to extrapolate observation at 1 AU to the vicinity of the Sun. Additionally, the occurrence of a flare of a given magnitude must be estimated on a statistical basis. Therefore, it is possible to state a likelihood that the fluxes and fluences will be less than a certain magnitude, but in the event of an extremely large solar flare (occurrence of perhaps once a decade, e.g., August 4, 1972) it is likely that the hazard would be insurmountable. A brief first look indicates that the near-solar particle environment is not a worse hazard than Jupiter. Author A. C. Cummings and E. C. Stone In Jet Propulsion Lab., California Inst. of Tech., Interplanetary Particle Environment. Proceedings of a Conference 15 Apr. 1988 p 133-134 (For primary document see N89-28454 22-90) (Contract NAS7-918; NGR-05-002-160) Avail: NTIS HC A08/MF A01 CSCL 03B This brief report is intended to update the anomalous component section of the summary report of the galactic cosmic-ray working group (Mewaldt et al., 1987), which was drafted at the March 1987 Workshop on the Interplanetary Charged Particle Environment at the Jet Propulsion Laboratory. The description of the spectrum of the anomalous cosmic-ray component is contained in section 3.3 of that report. That description is based on data analyzed through day 310 of 1986, and in it we proposed that the energy spectrum of the various species of the anomalous component could be derived by scaling from two generic spectra. Two generic spectra were required because the energy spectrum of the anomalous component changed shape near the time of the solar magnetic field reversal in 1980. These two generic spectra are shown in Figure 2 of the summary report. N89-28468*# Chicago Univ., IL. Author GRADIENTS OF GALACTIC COSMIC RAYS AND ANOMALOUS COMPONENTS c93 R. B. McKibben In Jet Propulsion Lab., California Inst. of Tech., Interplanetary Particle Environment. Proceedings of a Conference 15 Apr. 1988 p 135-148 (For primary document see N89-28454 22-90) Avail: NTIS HC A08/MF A01 CSCL 03B Measurements of radial and latitudinal gradients of galactic cosmic rays and anomalous components now cover radii from 0.3 to 40 AU from the sun and latitudes up to 30 deg above the ecliptic plane for particle energies from approx. 10 MeV/n up to relativistic energies. The most accurate measurements cover the period 1972 through 1987, which includes more than one full 11 year cycle of solar activity. Radial gradients for glactic cosmic rays of all energies and species are small (similar to less than 10 percent AU), and variable in time, reaching a minimum of near O percent AU out to 30 AU for some species at solar maximum. Gradients for anomalous components are larger, of order 15 percent AU, may show similar time variability, and are relatively independent of particle species and energy. For the period 1985 through 1986 the intensity decreased away from the ecliptic for all species and energies. For galactic cosmic rays, the measured gradients are approx. 0.5 percent/degree near 20 AU, while for anomalous components the gradients are larger, ranging from 3 to 6 percent/degree. Comparison with a similar measurement for anomalous helium in 1975 through 1976 suggests that the latitude gradients for anomalous components have changed sign between 1975 and 1985. For galactic cosmic rays, the available evidence suggests no change in sign of the latitudinal gradient for relativistic particles. Author C93 N89-28469*# Delaware Univ., Newark. TIME VARIATION OF GALACTIC COSMIC RAYS Paul Evenson In Jet Propulsion Lab., California Inst. of Tech., Interplanetary Particle Environment. Proceedings of a Conference 15 Apr. 1988 p 149-161 (For primary document see N89-28454 22-90) (Grants NAG5-374; NSF ATM-86-03192) Avail: NTIS HC A08/MF A01 CSCL 03B Time variations in the flux of galactic cosmic rays are the result of changing conditions in the solar wind. Maximum cosmic N89-28470*# Arizona Univ., Tucson. GALACTIC COSMIC RAYS IN THREE DIMENSIONS Abstract Only c93 J. R. Jokipii In Jet Propulsion Lab., California Inst. of Tech., Interplanetary Particle Environment. Proceedings of a Conference 15 Apr. 1988 p 162-163 (For primary document see N89-28454 22-90) Avail: NTIS HC A08/MF A01 CSCL 03B A general conclusion is that the cosmic rays increase with increasing distance from the Sun at approximately 2 percent a.u. There is a strong correlation of the cosmic ray intensity with distance with the tilt of the heliospheric current sheet. Moreover, researchers find that the variation of the cosmic rays with time changes in alternate sun spot cycles. Finally, it seems that during alternate sun spot minima (1965 and 1985) the cosmic rays access to the inner solar system was along the equatorial current sheet, wheras in 1975 the cosmic rays came in over the poles. The recently discovered anomalous component of cosmic rays is very much related to this whole problem, and probably corresponds to particles being accelerated at the termination of the solar wind at some 50 to 100 astonomical units from the sun. In summary, many predictions of the models remain controversial in detail. Nonetheless, it appears now that we can expect more cosmic rays over the poles in the next sunspot cycle, and the intensity will continue to increase with heliocentric radius out to the interstellar medium. Author (Grant NAGw-630) (NASA-CR-185862; NAS 1.26:185862) Avail: NTIS HC A03/MF A01 CSCL 03B Interstellar SiO was discovered shortly after CO but it has been detected mainly in high density and high temperature regions associated with outflow sources. A new model of interstellar silicon chemistry that explains the lack of SiO detections in cold clouds an exponential temperature is presented which contains dependence for the SiO abundance. A key aspect of the model is the sensitivity of SiO production by neutral silicon reactions to density and temperature, which arises from the dependence of the rate coefficients on the population of the excited fine structure levels of the silicon atom. This effect was originally pointed out in the context of neutral reactions of carbon and oxygen by Graff, who noted that the leading term in neutral atom-molecule interactions involves the quadrupole moment of the atom. Similar to the case of carbon, the requirement that Si has a quadrupole moment requires population of the J = 1 level, which lies 111K above the J = O ground state and has a critical density n(cr) equal to or greater than 10(6)/cu cm. The SiO abundance then has a temperature dependence proportional to exp(-111/T) and a quadratic density dependence for n less than n(cr). As part of the explanation of the lack of SiO detections at low temperatures and densities, this model also emphasizes the small efficiencies of the production routes and the correspondingly long times needed o reach equilibrium. Measurements of the abundance of SiO, in conjunction with theory, can provide information on the physical properties of interstellar clouds such as the abundances of oxygen bearing molecules and the depletion of interstellar silicon. Author (DE89-612518; IFT-P-03/87) Avail: NTIS (US Sales Only) HC A03/MF A01 A study of amounts of information necessary to localize the trajectory of a dynamical system known as the Mixmaster universe is presented. The main result is that less information is necessary near the cosmological singularity of the system than far away. This conclusion is obtained by evolving probability distributions towards the singularity and comparing the associated information functions. Qualitative methods of dynamical systems theory present a phenomenon that might be related to this loss of information. DOE N89-28473# Hiroshima Univ., Takehara (Japan). Research Inst. for Theoretical Physics. STOCHASTIC APPROACH TO CHAOTIC INFLATION AND THE DISTRIBUTION OF UNIVERSES Yasusada Nambu and Masao Sasaki Nov. 1988 15 p (DE89-778051; RRK-88-35) Avail: NTIS (US Sales Only) HC A03/MF A01 Using the Fokker-Planck equation derived from stochastic approach to inflation, the dynamics and global structure of the chaotic inflationary universe are investigated. Full account was taken of the difference in the physical volume of each horizon size region in the Fokker-Planck equation. It was found that the modified Fokker-Planck equation admits a normalizable stationary solution, contrary to the original equation. The approximate form of the solution was evaluatedand it describes both the distribution of quantum universes out of which the universes was born and that of large classical (grow-up) universes like ours. In particular, for lambda phi sup 4 theory, the distribution of classical universes has a power law spectrum. Thus there appears no characteristic scale and the distribution of classical universes has a fractal DOE structure. 91 LUNAR AND PLANETARY EXPLORATION Includes planetology; and manned and unmanned flights. For spacecraft design or space stations see 18 Spacecraft Design, Testing and Performance. N89-28474*# National Aeronautics and Space Administration, Workshop held in Flagstaff, AZ, 25-27 Aug. 1987 Original contains color illustrations (NASA-SP-494; NAS 1.21:494; LC-88-25450) Avail: NTIS HC A18/MF A01 CSCL 03B The current state of knowledge of dynamic processes in the Jovian system is assessed and summaries are provided of both theoretical and observational foundations upon which future research might be based. There are three sections: satellite phenomena and rings; magnetospheric phenomena, lo's torus, and aurorae; and atmospheric phenomena. Each chapter discusses time dependent theoretical framework for understanding and interpreting what is observed; others describe the evidence and nature of observed changes or their absence. A few chapters provide historical perspective and attempt to present a comprehensive synthesis of the current state of knowledge. Author N89-28475*# Hampton Inst., VA. Dept. of Computer Science. PARALLEL ARCHITECTURES FOR PLANETARY EXPLORATION REQUIREMENTS (PAPER) Interim Report Ruknet Cezzar and Ranjan K. Sen 25 Jun. 1989 57 p |