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Search indexed NASA NTRS and DOE OSTI research on propulsion, heat transfer, battery materials and energy systems. Follow report and document links to the original sources.

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At least 811 records · Page 45
All sourcesNASA NTRSDOE OSTI
NASA NTRS1989

Improved performance in NASTRAN (R)

Three areas of improvement in COSMIC/NASTRAN, 1989 release, were incorporated recently that make the analysis program run faster on large problems. Actual log files and actual timings on a few test samples that were run on IBM, CDC, VAX, and CRAY computers were compiled. The speed improvement is proportional to the problem size and number of continuation cards. Vectorizing certain operations in BANDIT, makes BANDIT run twice as fast in some large problems using structural elements with many node points. BANDIT is a built-in NASTRAN processor that optimizes the structural matrix bandwidth. The VAX matrix packing routine BLDPK was modified so that it is now packing a column of a matrix 3 to 9 times faster. The denser and bigger the matrix, the greater is the speed improvement. This improvement makes a host of routines and modules that involve matrix operation run significantly faster, and saves disc space for dense matrices. A UNIX version, converted from 1988 COSMIC/NASTRAN, was tested successfully on a Silicon Graphics computer using the UNIX V Operating System, with Berkeley 4.3 Extensions. The Utility Modules INPUTT5 and OUTPUT5 were expanded to handle table data, as well as matrices. Both INPUTT5 and OUTPUT5 are general input/output modules that read and write FORTRAN files with or without format. More user informative messages are echoed from PARAMR, PARAMD, and SCALAR modules to ensure proper data values and data types being handled. Two new Utility Modules, GINOFILE and DATABASE, were written for the 1989 release. Seven rigid elements are added to COSMIC/NASTRAN. They are: CRROD, CRBAR, CRTRPLT, CRBE1, CRBE2, CRBE3, and CRSPLINE.

Chan, Gordon C.↗
NASA NTRS1989

NASA space communications R and D (Research and Development): Issues, derived benefits, and future directions

Space communication is making immense strides since ECHO was launched in 1962. It was a simple passive reflector of signals that demonstrated the concept. Today, satellites incorporating transponders, sophisticated high-gain antennas, and stabilization systems provide voice, video, and data communications to millions of people nationally and worldwide. Applications of emerging technology, typified by NASA's Advanced Communications Technology Satellite (ACTS) to be launched in 1992, will use newer portions of the frequency spectrum (the Ka-band at 30/20 GHz), along with antennas and signal-processing that could open yet new markets and services. Government programs, directly or indirectly, are responsible for many space communications accomplishments. They are sponsored and funded in part by NASA and the U.S. Department of Defense since the early 1950s. The industry is growing rapidly and is achieving international preeminence under joint private and government sponsorship. Now, however, the U.S. space communications industry - satellite manufacturers and users, launch services providers, and communications services companies - are being forced to adapt to a different environment. International competition is growing, and terrestrial technologies such as fiber optics are claiming markets until recently dominated by satellites. At the same time, advancing technology is opening up opportunities for new applications and new markets in space exploration, for defense, and for commercial applications of several types. Space communications research, development, and applications (RD and A) programs need to adjust to these realities, be better coordinated and more efficient, and be more closely attuned to commercial markets. The programs must take advantage of RD and A results in other agencies - and in other nations.

Source record↗
NASA NTRS1989

The evolution of space mechanisms in the ESA R and D program

The status of recently completed and already ongoing technology developments, as well as some of the most important future developments of the European Space Agency are discussed. Among the subjects considered are Scientific Satellites, Columbus space station development, applications spacecraft for communications, Earth observation and meteorology, and the Ariane V and Hermes space transportation systems.

Wyn-Roberts, D.↗
NASA NTRS1988

HD 38452 - J. R. Hind's star that changed colour

In 1851, John Russell Hind announced that a star previously observed by him to be very red had become bluish white in color. It is shown that this star, HD 38451, is a ninth magnitude shell star which presumably was ejecting a shell when Hind first observed it. From high dispersion coude spectra, low dispersion IUE spectra, and ground-based photometry, HD 38451 is found to be a normal A21V shell star. Its current values of E(B-V) of about 0.14 is probably caused by interstellar rather than circumstellar reddening. There remains a problem to reconcile the large amount of reddening present when Hind first observed the star with its evidently small diminution in visual brightness at that time.

Warner, Brian↗
NASA NTRS1988

The three R's of training: Recording, Retaining, and Reporting - The training management system that synergizes

NASA's Kennedy Space Center employs a Training and Certification Record System (TCRS) which tracks and maintains records for each of its employees, encompassing all aspects of training history: training courses, physical examinations, proficiency tests, on-the-job training, standboards, and certifications with completions and expiration dates. TCRS, which is fully automated, includes an expiration-alert notification capability to project recurring expirations, thereby functioning as a forecasting tool for training budgets.

Ingram, Dick D.↗
NASA NTRS1988

The support constraints for orbital systems - How to measure the R&M effects

The loss of the space shuttle Challenger cast doubt on many issues of Space Station support. Modeling alternatives runs into theoretical difficulties. This paper reports on a modeling approach that accounts for a fixed resupply cycle in reliability estimates for a single orbital system. The emphasis in the single-system model is on ground-based support, rather than on orbital activities and constraints. The paper also provides a scheme in outline for a multi-system model that similarly reflects Space Station restorability concepts, but accounts for cross-system competition for on-orbit resources and access to launch vehicle space.

Weisman, Carl S.↗
NASA NTRS1989

Magnetospheric plasma pressures in the midnight meridian - Observations from 2.5 to 35 R(E)

Plasma pressure data from the ISEE 2 fast plasma experiment (FPE) are statistically analyzed to determine the plasma sheet pressure versus distance in the midnight local time sector of the near-earth (12-35 earth radii) magnetotail plasma sheet. In regions where the bulk of the plasma pressure is contributed by particles in the energy range of the FPE (70 eV to 40 keV for ions), the statistically determined peak plasma pressures vary with distance similarly to previously determined lobe magnetic pressures. Estimates of plasma pressures in the 'transition' region (7-12 earth radii), where the magnetic field topology changes rapidly from a dipolar to a taillike configuration, are compared with the observed pressure profiles. Quiet time observations and estimates are combined to provide profiles of the equatorial plasma pressure along the midnight meridian between 2.5 and 35 earth radii.

Spence, Harlan E.↗
NASA NTRS1989

Radial diffusion and losses of energetic protons in the 5 to 12 R(S) region of Saturn's magnetosphere

Phase space density profiles for nearly equatorial mirroring energetic protons, derived from Pioneer 11 measurements during the 1979 Saturn encounter, were analyzed using solutions of the time-averaged radial diffusion equation in a dipolar planetary magnetic field. Then, several loss models were considered, ranging from a model that takes into account satellite absorption only to the one that accounts for satellite plus ring-E absorption plus added distributed losses, and the corresponding form of the time-averaged radial diffusion coefficient was determined for each case by a minimum-variance fit to the data-derived phase space densiy profiles. The model comparisons clearly indicated the need for distributed losses, in addition to satellite absorption, in order to explain the smooth decline of the experimental energetic proton phase space density profiles in the 5-12-Saturn radius region of Saturn's magnetosphere.

Hood, L. L.↗
NASA NTRS1989

Comment on 'Observations of Low-Latitude Electron Precipitation' by R. Lieu, J. Watermann, K. Wilhelm, J. J. Quenby, and W. I. Axford

Observations made by an electron spectrometer aboard Spacelab 1 and presented by Lieu et al. (1988) are examined critically. The precipitation of electrons in the energy range of 0.1-12.5 keV was measured on December 6 and 7, 1983. Data for 16 passes near 240 km altitude, between + and - 30 deg geographic latitude, outside the South Atlantic Anomaly were included. It is argued that there is no geophysical confirmation of the large electron fluxes reported by Lieu et al. In their response, Lieu et al. discuss the sampling bias in the Spacelab 1 data and the magnetic shielding deficiencies of the calibration facility below about 500 eV.

Rassoul, H. K.↗
NASA NTRS1989

Space Station Freedom - Accommodation for technology R&D

The paper examines the features of the accommodation equipment designed for the candidate technology payloads of the Space Station, which include magnetic plasma thruster systems and a hypothetical advanced electromagnetic propulsion system utilizing high-temperature superconductivity materials. The review of the accommodation-equipment concepts supports the assumption that some propulsion technologies can be tested on the Space Station while being attached externally to the station's truss structure. For testing technologies with inherent operation or performance hazards, space platforms and smaller free-flyers coordinated with the Space Station can be used. Diagrams illustrating typical accommodation equipment configurations are included.

Holt, Alan C.↗
NASA NTRS1989

An upfront R&M approach for aerospace systems

NASA has recently established a maintainability and maintenance planning program. This paper presents an overview of the program and discusses the specific application of the maintainability requirements as contained in NASA handbook (NHB) 5300.4 (1E), 'Maintainability Program Requirements for Space Systems'. Suggestions regarding the extent to which these requirements should be applied during each phase of program development also are presented.

Lisk, Ronald C.↗
NASA NTRS1990

Eighteenth NASTRAN (R) Users' Colloquium

This publication is the proceedings of the Eighteenth NASTRAN Users' Colloquium held in Portland, Oregon, April 23-27, 1990. It provides some comprehensive general papers on the application of finite elements in engineering, comparisons with other approaches, unique applications, pre- and post-processing or auxiliary programs, and new methods of analysis with NASTRAN.

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NASA NTRS1990

A generic interface between COSMIC/NASTRAN and PATRAN (R)

Despite its powerful analytical capabilities, COSMIC/NASTRAN lacks adequate post-processing adroitness. PATRAN, on the other hand is widely accepted for its graphical capabilities. A nonproprietary, public domain code mnemonically titled CPI (for COSMIC/NASTRAN-PATRAN Interface) is designed to manipulate a large number of files rapidly and efficiently between the two parent codes. In addition to PATRAN's results file preparation, CPI also prepares PATRAN's P/PLOT data files for xy plotting. The user is prompted for necessary information during an interactive session. Current implementation supports NASTRAN's displacement approach including the following rigid formats: (1) static analysis, (2) normal modal analysis, (3) direct transient response, and (4) modal transient response. A wide variety of data blocks are also supported. Error trapping is given special consideration. A sample session with CPI illustrates its simplicity and ease of use.

Roschke, Paul N.↗
NASA NTRS1989

Analysis of an extended period of earthward plasma sheet flow at about 220 R(E) - CDAW 8

The interpretation of the ISEE 3 earthward flow events observed during an extended period on January 29, 1983 is addressed in terms of a neutral line moving beyond roughly 220 earth radii. This concept was tested for consistency with current magnetospheric and solar wind observations. A broad range of additional data including Dynamics Explorer auroral imaging and a wide variety of ground-based measurements from the eighth Coordinated Data Analysis Workshop (CDAW 8) was available. The distant neutral line location within the context of the distant tail, geostationary orbit, auroral zone, and associated solar wind data is analyzed, based on an extended version of the Coraniti and Kennel (1972) flaring tail theory. It is concluded, from known solar wind conditions that, for a typical neutral line location at about 135 earth radii, an increase of about 30 percent of the near-earth lobe field strength would be required to cause the distant neutral line to move tailward beyond 220 earth radii. The question of why substorms did not terminate the growth phase earlier is also addressed.

Schindler, K.↗
NASA NTRS1990

On the apparent positions of T Tauri stars in the H-R diagram

The spread in apparent luminosities of T Tauri stars caused by occultation and emission from protostellar disks is investigated. A random distribution of disk inclination angles, coupled with a plausible range of accretion rates, introduces a significant scatter in apparent luminosities for intrinsically identical stars. The observed dispersion of luminosities for K7-M1 Hayashi track stars thought to have disks in Taurus-Auriga is similar to predictions of the simple accretion disk model, which suggets that age determinations form many pre-main-sequence stars are uncertain. The results also suggest that Stahler's 'birthline' for convective track pre-main-sequence stars may be located at slightly lower luminosities than previously thought.

Kenyon, Scott J.↗
NASA NTRS1991

Nineteenth NASTRAN (R) Users' Colloquium

The proceedings of the the Nineteenth NASTRAN Users' Colloquium held April 22 to 26, 1991 are presented. Topics covered include the application of finite elements in engineering, comparisons with other approaches, unique applications, pre- and postprocessing or auxiliary programs, and new methods of analysis with NASTRAN.

Source record↗
NASA NTRS1991

Experiences in porting NASTRAN (R) to non-traditional platforms

The 1990 UNIX version of NASTRAN was ported to two new platforms that are not supported by COSMIC: the Sun SPARC workstation and the Apple Macintosh using the A/UX version of UNIX. The experiences of the authers in porting NASTRAN is summarized here. Suggestions for users who might attempt similar ports are given.

Davis, Gregory L.↗
NASA NTRS1991

Spectra of comet P/Halley at R = 4 - 8 AU

Spectra of Comet Halley (lambda lambda = 3400-6500 A) were acquired at pre- and post-perihelion distances of 4.8 AU on 1985 Feb. 17 (Coma V equals 18.9 mag) and 1987 Feb. 1 (coma V = 15.9 mag) using the 4.5-m Multiple-Mirror Telescope (MMT) and the CTIO 4.0-m telescope, respectively. The CN(0,0) violet system band flux at 4.8 AU was approx. 15 times greater at the post-perhelion phase compared to pre-perihelion. Additional post-perihelion spectra, obtained on 1986 Nov. 28 to 30 with the MTT, showed CN(0,0) and very weak C3 4040 A emission. The MMT data are one-dimensional spectra (aperture: 5 arc sec diameter) obtained with an intensified Reticon while the CTIO data are two-dimensional spectra (slit length = 280 arc sec) obtained with a 2D-Frutti photon counting system. Extended CN(0,0) emission was detected in the 1987 Feb. 1 (at 4.8 AU) spectra to a distance of at least 70 arc sec in the solar and anti-solar directions. Additional CCD spectra obtained with the KPNO 2.2-meter telescope on 1988 Feb. 20 (at 7.9 AU) show scattered solar continuum approx. 32 arc sec diameter. However, no emission features were detected at 7.9 AU.

Wehinger, Peter A.↗