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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 145 records · Page 8
All sourcesNASA NTRSDOE OSTI
DOE OSTI2026

Ice-nucleating particles (INPs) concentrations from SAIL-Net

This data set contains ice-nucleating particle (INP) concentration spectra collected during the SAIL-Net sampling period, which complemented the Surface Atmosphere Integrated Field Laboratory (SAIL) campaign in the East River watershed near Crested Butte, Colorado. SAIL-Net was a distributed aerosol measurement network designed to investigate aerosol variability across complex mountainous terrain. The data set includes samples from multiple SAIL-Net sites, including AOS, Gothic, Snodgrass, Pumphouse, Irwin, and Top. INP concentrations are reported as a function of freezing temperature, together with confidence limits, sampling times, site location, elevation, sampled air volume, and treatment information. These data provide an analysis-ready record of the INPs across the SAIL-Net network.

activation temperature↗
NASA NTRS1969

On the shell equations in complex form.

Linear thin shell theory in complex dependent variable form for determining fourth order partial differential equations, considering elastic shells with edge loads

Sanders, J. L., Jr.↗
NASA NTRS1974

Measurement of cosmic ray positron and negatron spectra between 50 and 800 MeV

A balloon-borne magnetic spectrometer was used to measure the spectra of cosmic ray positrons and negatrons at energies between 50 and 800 MeV. Comparisons of the separate positron and negatron spectra observed near the earth with their expected intensities in interstellar space can be used to investigate the complex (and variable) interaction of galactic cosmic rays with the expanding solar wind. The present measurements, which have established finite values or upper limits for the positron and negatron spectral between 50 and 800 MeV, have confirmed earlier evidence for the existence of a dominant component of negatrons from primary sources in the galaxy. The present results are shown to be consistent with the hypothesis that the positron component is in fact mainly attributable to collisions between cosmic ray nuclei and the interstellar gas. The estimate of the absolute intensities confirm the indications from neutron monitors that in 1972 the interplanetary cosmic ray intensities were already recovering toward their high levels observed in 1965.

Daugherty, J. K.↗
NASA NTRS1973

Total carbon contents of Apollo 15 and 16 lunar samples

The total carbon contents in Apollo 15 fines range from 29 to 170 micrograms/g. Fines from Apollo 16 range from 65 to 280 micrograms/g. These samples are similar to those from Apollo 11, 12, and 14, with dark colored fines generally containing more carbon than lighter fines. Sample 61221 (light colored fines) is anomalously high with 100 micrograms/g total carbon. Correlations between total carbon content and sample collection station for each mission are evident. Basalts from Apollo 15 have less than 27 micrograms/g total carbon. Anorthositic rocks from Apollo 15 and 16 have less than 20 micrograms/g total carbon. Breccias show complex and variable carbon distributions.

Moore, C. B.↗
NASA NTRS1976

Structure of the neutral upper atmosphere of Mars - Results from Viking 1 and Viking 2

Neutral mass spectrometers carried on the aeroshells of Viking 1 and Viking 2 indicate that carbon dioxide is the major constituent of the Martian atmosphere over the height range 120 to 200 kilometers. The atmosphere contains detectable concentrations of nitrogen, argon, carbon monoxide, molecular oxygen, atomic oxygen, and nitric oxide. The upper atmosphere exhibits a complex and variable thermal structure and is well mixed to heights in excess of 120 kilometers.

Nier, A. O.↗
NASA NTRS1978

Structure of the Magnetopause: Observations and Implications for Reconnection

The earth's magnetopause is the boundary between a hot tenuous plasma in the magnetosphere and a cooler denser plasma in the magnetosheath. Both of these plasmas contain magnetic fields whose directions are usually different but whose magnitudes are often comparable. Efforts to understand the structure of the magnetosphere were hampered by the variability and complexity of this boundary. Although conclusive direct evidence for a field component, B sub n across the magnetopause was not found, this lack of evidence may reflect the difficulty in determining B sub n in the presence of magnetopause waves rather than the real absence of this component. Considerable indirect evidence exists for an open magnetosphere, but the importance of the reconnection process thought to produce open field lines was questioned.

Fairfield, D. H.↗
NASA NTRS1977

Composition and structure of Mars' upper atmosphere - Results from the neutral mass spectrometers on Viking 1 and 2

The upper atmospheric mass spectrometers flown on Viking 1 and 2 are described, and results obtained for the composition and structure of Mars' upper atmosphere are summarized. Carbon dioxide is the major constituent of the atmosphere at all heights below 180 km. The thermal structure of the upper atmosphere is complex and variable with average temperatures below 200 K for both Viking 1 and 2. The atmosphere is mixed to heights in excess of 120 km. The isotopic composition of carbon and oxygen in the Martian atmosphere is similar to that in the terrestrial atmosphere: N-15 is enriched in Mars' atmosphere by a factor of 1.62 + or - 0.16.

Nier, A. O.↗
NASA NTRS1979

Structure of the magnetopause - Observations and implications for reconnection

The earth's magnetopause is the boundary between a hot tenuous plasma in the magnetosphere and a cooler denser plasma in the magnetosheath. Both of these plasmas contain magnetic fields whose directions are usually different but whose magnitudes are often comparable. Efforts to understand the structure of the magnetosphere have been hampered by the variability and complexity of this boundary. Waves on the magnetopause surface propagate toward the magnetotail and produce the multiple boundary crossings frequently seen by spacecraft. Boundary velocities are poorly known and range anywhere within an order of magnitude of 10 km/s. Typical thicknesses are probably of the order of a few hundred km, which is a few times the gyroradius of a thermal proton. Although conclusive direct evidence for a field component, Bn, across the magnetopause has not been found; this lack of evidence may reflect the difficulty in determining Bn in the presence of magnetopause waves rather than the real absence of this component. Considerable indirect evidence exists for an open magnetosphere, but the importance of the reconnection process thought to produce open field lines has recently been questioned.

Fairfield, D. H.↗
NASA NTRS1979

Observations of pulsating X-ray binaries 4U0900-40 and 4U1223-62

A sounding-rocket observation of the pulsating X-ray binaries 4U 0900-40 (Vela X-1) and 4U 1223-62 (GX301-2, Wray 977) over the energy range from 0.5 to 27 keV is reported. No short-time-scale periodicities in the range from 2 msec to 20 sec are found for either source, although both exhibit some minor flaring activity on time scales of a few seconds. The data for Vela X-1 suggest that the time-averaged spectra are complex and that the pulse-resolved spectra are also complex and variable, with significant fluctuations above 10 keV. When compared with other observations at different epochs, the spectral data for 4U 1223-62 confirm large variability in both intensity and spectral characteristics. It is concluded that the intrapulse changes observed in the spectral behavior of Vela X-1 must reflect changes in the surface magnetic fields and the plasma flows near the neutron star.

Ku, W. H.-M.↗
NASA NTRS1980

Shockless airfoils for wings, compressors, and turbines

The major aspects of a code for the design of shockless airfoils in two-dimensional transonic flow are reviewed. The code is based on a method of analytic continuation into the domain of two complex characteristic variables, which makes it possible to associate a shockless airfoil with a given pressure distribution. This procedure is compared with another more direct method based on a two-dimensional analysis code that has had wide acceptance by the aircraft industry.

Garabedian, P. R.↗
NASA NTRS1981

Energetic particle events /greater than or equal to 30 keV/ of Jovian origin observed by Voyager 1 and 2 in interplanetary space

Detailed observations of ion events of Jovian origin as observed by the low energy charge particle (LECP) instrumentation on Voyager 1 and 2 during the inbound and outbound pass for both spacecraft are reported. The general characteristics of these events are examined, and a comparison is made with similar observations at earth. Careful attention is given to the compositional signature of the Jovian ion events. Two of the specific events discussed in detail are selected to display the range of variability and complexity of the Jovian-produced interplanetary ion events. The observations are seen as strongly implying that the Jovian magnetosphere is the source of a significant fraction of the particles.

Zwickl, R. D.↗