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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 973 records · Page 54
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NASA NTRS1985

Anomalous low level of cosmic ray intensity decreases observed during 1980

Past studies have revealed solar cycle changes in the sunspot activity, as well as in many other solar parameters, such as, solar flares and solar coronal holes. These solar features in turn produce the observed cyclic variations in the interplanetary plasma and fields. Both the cosmic ray intensity as well as the intensity of geomagnetic disturbances are affected by the interplanetary changes and produce 11/22 year periodicity. An anomalous situation has been noticed during the year 1980 (period of high sunspot activity), when both the geomagnetic disturbance index Ap, as well as the magnitude and number of Forbush decreases as small. Such an anomaly occurs, in spite of the fact that both the sunspot numbers and the energetic solar flares are almost maximum during the present solar cycle.

Jain, A. K.↗
NASA NTRS1984

Rotation and the internal structures of the major planets and their inner satellites

Measurements of the rotational periods coupled with those of the masses, the mean radii, and the shapes or the gravitational moments (J2 and J4) enable important constraints to be placed on the internal structures of some remote bodies. Values of J2 for Uranus and Neptune have been calculated from the observed precession rates of the narrow eccentric and inclined Uranian rings and of the orbit of Triton, Neptune's massive satellite. Recent observations of the motions of spots have yielded reliable rotational periods for these planets. These observations are used to show that Uranus and Neptune may have quite different internal structures. The shapes of satellites that are close to their primaries may yield information on the degree of internal differentiation of these bodies. Io, Mimas, Enceladus, and Miranda are of interest in this respect. Residuals in the observed precession rates of the Uranian rings, about 0.005 deg/day, that cannot be accounted for by the best-fit model of J2 and J4 may be related directly to observed irregular variations in ring width of magnitude over 2 km and may indicate the existence of shepherding satellites with mass ratios of over 10 to the -10th. If this is the case, then the effects of these satellites on the precession rates of the rings will result in an appreciable uncertainty in the value of J4 for Uranus.

Dermott, S. F.↗
NASA NTRS1985

Magnetopause merging site asymmetries

Regions where a draped model magnetosheath magnetic field is nearly antiparallel to a model geomagnetic field are shown to be asymmetric for an interplanetary magnetic field (IMF) at the garden hose angle, as suggested by Heelis. When the IMF has a southward component, the asymmetry favors the dawn region for both IMF polarities. The dusk region is favored when the IMF has a northward component. If the regions of antiparallel fields are assumed to be sites of maximum magnetic merging, then the asymmetry is consistent with observed seasonal variations of geomagnetic activity and with dawn-displaced magnetospheric phenomena. In the alternate merging geometry of a line passing through the subsolar region, the asymmetry is predominantly north-south rather than dawn-dusk. Merging line geometry is consistent with the seasonal variations but not with the dawn-displaced phenomena.

Crooker, N. U.↗
NASA NTRS1985

Radio and infrared observations of OH/IR stars at the tangential point and near the galactic center

Unambiguous infrared identifications of a sample of OH/IR stars in the galactic disk and in the vicinity of the galactic center are presented. Simultaneous OH and broadband infrared photometric measurements are used to derive quantitative relations between the infrared and OH fluxes and the properties of the circumstellar shells, providing observational evidence that these stars represent an evolutionary sequence of increasing mass loss rate. These relations are used to explain the observed time variations of the silicate absorption feature with changing bolometric luminosity in OH/IR stars. It appears that the ratio of the OH flux to the number of pump photons is not constant, but is also a function of the mass loss rate.

Baud, B.↗
NASA NTRS1985

The importance of improved facular observations in understanding solar constant variations

A new study of solar irradiance modeling has been undertaken to improve the previous modeling efforts and perhaps to resolve the energy-balance question. In the present study, the daily sunspot and facular areas (using plages as a proxy measure of faculae) have been utilized, as well as a plage intensity index to examine brightness variations. It is noted that the reported plage areas changed by a factor of 2 near the end of 1979. Although this can be partially modeled because a commensurate change in plage brightness occurs, it leads to the conclusion that facular areas and brightness uncertainties prevent a definitive answer to the energy-balance question with this technique.

Schatten, K. H.↗
NASA NTRS1985

Power spectra of mesospheric velocities in polar regions

The mobile SOUSY radar was operated on Andoya in Northern Norway during the MAP/WINE campaign from November 1983 to February 1984 and for about two weeks in June 1984 to study the seasonal dependence of mesospheric structures and dynamics at polar latitudes. During the winter period, measurements were carried out on 57 days, primarily in coordination with the schedule of the rocket experiments. Echoes were detected in the troposphere and stratosphere up to 30 km and at mesospheric heights from about 50 to 90 km with a distinct maximum around noon. In summer, the radar system was operated continuously from 19th to the 28th of June 1984. Echoes occurred almost for 24 hours in the height range from 70 to 95 km showing no recognizable diurnal variation. Similar observations in polar latitudes were carried out for several years with the Poker Flat Radar in Alaska.

Czechowsky, P.↗
NASA NTRS1986

The distribution of dust in the inner coma of comet IRAS-Araki-Alcock (1983d)

The behavior and characteristics of the inner coma of the Comet IRAS-Araki-Alcock (IAA) were examined for five nights in May 1983 using a ground-based 2.2 m CCD telescope. A highly variable, asymmetric sunward emission was detected, along with a long filamentary structure. The brightness was highest in the sunward direction, with radial brightnesses diminishing more slowly than predicted with a 1/r model. The slow fall-off is attributed to the emission of conglomerate dust grains which fragment while traveling through the inner coma and increase the effective surface area of the dust. Significant day-to-day variations were observed, and the filamentary features were indicative of a centralized region on a mantled nucleus which rotated. The nucleus is estimated to be no more than 17 km in diameter.

Storrs, A. D.↗
NASA NTRS1985

Electron density in the equatorial topside

Ionospheric electron content studies have revealed severe discrepancies between Faraday measurements and model predictions at low latitudes. In this investigation, satellite data of AE-C and Aeros and incoherent scatter data from Jicamarca, Peru and Arecibo, Puerto Rico are used to examine the latitudinal and diurnal extent of this disagreement. It is found that in the modified dip range -30 deg to +30 deg the present IRI relative layer shape underestimates the thickness of the topside electron density during both, day and night. The Bent model which was used as a source for the IRI description performs somewhat better in this critical dip range, though it does not reach the observed values. Also it does not show the observed diurnal variation. A correction to the IRI formula is proposed that guarantees better agreement with the satellite and incoherent scatter data.

Bilitza, D.↗
NASA NTRS1985

Stress assessment and spectral characterization of suspected acid deposition damage in red spruce (Picea Rubens) from Vermont

The effects of acid deposition on Picea rubens are studied. The Picea rubens located at Camels Hump Mt., Mt. Ascutney, and Ripton, VT were analyzed using stress level evaluations, in situ spectral data, pressure bomb analysis, and aircraft sensors. Spruce stress per circular plot and percent spruce mortality are calculated. The relation between stress levels and elevation and exposure and weather patterns is examined. It is observed that variations in the reflectance curves of the foliage and branches are related to cellular health, the type of cellular arrangement, and the degree of leaf tissue hydration; the leaf and twig specimens from high stress sites are more reflective in the red portion of the visible and less reflective in the NIR portion of the spectrum. The pressure bomb data reveal that the xylem water tension is higher in specimens from high stress sites. It is noted that remote sensing permits discrimination and mapping of suspected acid deposition damage.

Rock, B. N.↗
NASA NTRS1987

Middle atmosphere density and models

The 80 to 130 km altitude region is our old ignorosphere, the region of the atmosphere that no one seems to be interested in and yet the critical region for shuttle entry and atmospheric braking. Comparison between the Air Force reference atmosphere and Shuttle Inertial Measurement Units data shows large fluctuations at high latitudes. New data sources are available now, such as the Arecibo and Millstone Hill ionospheric scatter radars. In the 20 to 80 km altitude range there is a reasonable quantity of data on the mean atmosphere, however, infomation on diurnal variability is needed. In the 20 to 80 km altitude range data is needed to identify systematic variations and models for the regions are preliminary. Unpredictable variations are observed: turbulence, storm effects, gravity waves.

Champion, K.↗
NASA NTRS1986

Rapid spectral and flux time variations in a solar burst observed at various dm-mm wavelengths and at hard X-rays

A solar burst was observed with high sensitivity and time resolution at cm-mm wavelengths by two different radio observatories (Itapetinga and Algonquin), with high spectral time resolution at dm-mm wavelengths by patrol instruments (Sagamore Hill), and at hard X-rays (HXM Hinotori). At the onset of the major burst time structure there was a rapid rise in the spectral turnover frequency (from 5 to 15 GHz), in about 10s, coincident to a reduction of the spectral index in the optically thin part of the spectrum. The burst maxima were not time coincident at the optically thin radio frequencies and at the different hard X-ray energy ranges. The profiles at higher radio frequencies exhibited better time coincidence to the high energy X-rays. The hardest X-ray spectrum (-3) coincided with peak radio emission at the higher frequency (44 GHz). The event appeared to be built up by a first major injection of softer particles followed by other injections of harder particles. Ultrafast time structures were identified as superimposed on the burst emission at the cm-mm high sensitivity data at X-rays, with predominant repetition rates ranging from 2.0 to 3.5 Hz.

Zodivaz, A. M.↗
NASA NTRS1987

Electrodynamics of the middle atmosphere: Superpressure balloon program

In this experiment a comprehensive set of electrical parameters were measured during eight long duration flights in the southern hemisphere stratosphere. These flight resulted in the largest data set ever collected from the stratosphere. The stratosphere has never been electrodynamically sampled in the systematic manner before. New discoveries include short term variability in the planetary scale electric current system, the unexpected observation of stratospheric conductivity variations over thunderstorms and the observation of direct stratospheric conductivity variations following a relatively small solar flare. Major statistical studies were conducted of the large scale current systems, the stratospheric conductivity and the neutral gravity waves (from pressure and temperature data) using the entire data set.

Holzworth, Robert H.↗
NASA NTRS1987

Experiments on dynamic stiffness and damping of tapered bore seals

Stiffness and damping were measured in tapered bore ring seals with air as the sealed fluid. Excitation was provided by a known unbalance in the shaft which rotated in the test seals. Results were obtained for various seal supply pressures, clearances, unbalance amounts, and shaft speeds. Stiffness and damping varied little with unbalance level, indicating linearity of the seal. Greater variation was observed with speed and particularly supply pressure. A one-dimensional analysis predicted stiffness fairly well, but considerably overestimated damping.

Fleming, David P.↗
NASA NTRS1986

Heat transfer in the stagnation region of the junction of a circular cylinder perpendicular to a flat plate

The heat transfer rate in the stagnation region of the junction of a circular cylinder perpendicular to a flat plate was measured for a range of Reynolds numbers varying from 3.0 x 10 to the 4th to 7.0 x 10 to the 5th and a flow Mach number of 0.14. The measurements were performed in a shock-tube facility using a reflected shockwave technique and thin-film platinum heat gages. The heat flux was measured for both the plate and the circular cylinder. A substantial increase in the heat transfer rate in the junction region was observed. The influence of the cylinder over the flat plate extended beyond 3/4 cylinder diameter for low Reynolds numbers. For high Reynolds numbers the maximum increase in the heat transfer rate was observed to be approximately 100 percent, but for very low Reynolds numbers a maximum increase in the heat flux to the plate by a factor of 5 was observed. The variations in the heat transfer rate to the stagnation point of the cylinder was very small.

Hinckel, J. N.↗
NASA NTRS1986

A study of the damping capacity of graphite epoxy composites in a vacuum

The damping properties of a graphite epoxy composite material (used in the construction of the Hubble Space Telescope) are measured under a variety of conditions in a vacuum chamber to simulate conditions in space. An improved method is proposed which utilizes several points of the response curve near a resonance to estimate the damping ratio and the undamped resonance frequency. The damping of a graphite epoxy tube is monitored for four weeks to study moisture desorption and temperature effects. A significant variation is observed in the damping ratio with temperature.

Rao, Mohan D.↗
NASA NTRS1987

Voyager observations of the azimuthal brightness variations in Saturn's rings

The present Voyagers I and II measurements of Saturn A ring azimuthal brightness variations in reflected light are noted to be in general agreement with earth-based measurements. Voyager images of the rings in light transmitted through them also indicate the presence of these brightness variations, but with greater amplitude and an about 65-deg phase discrepancy with those seen in reflection. These differences in photometric behavior are qualitatively accounted for in terms of the widespread presence of particle wakes in the A ring.

Franklin, F. A.↗
NASA NTRS1987

Evidence for turbulence in H II regions

The results of extensive velocity mapping across the face of Galactic H II regions are used to make an accurate determination of velocity dispersions and structure functions for a number of nebulae. A dependence of random velocities upon scale, indicating the presence of turbulence, is found. These relationships are compared with the predictions of models for Kolmogorov turbulence in H II regions, and poor agreement is found. A more general formulation shows that there is no single power law for the velocity-distance relation that fits the observations. From the variations in the shape of the observed structure function, it is concluded that the turbulent energy enters the nebulae at several different scales. It is also found that velocity broadening of the observed lines is significantly greater than would be inferred from the velocity scatter across the face of the nebulae.

O'Dell, C. R.↗