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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 433 records · Page 24
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NASA NTRS1974

Acoustic-gravity waves in the upper atmosphere

In this paper we review the theory of acoustic-gravity waves, the interaction of such waves with the ionosphere, the experimental support for the existence of such waves in the upper atmosphere, and the role played by acoustic-gravity waves in thermospheric dynamics. After a thorough discussion on the properties of acoustic-gravity waves in an ideal isothermal atmosphere, the effects produced by horizontal winds, sharp boundary discontinuities, and dissipative processes are discussed. The generation of these waves by stationary or moving sources is then treated. It is shown that the atmospheric response to a stationary impulse source can be described by the emission of three waves: acoustic, buoyancy, and gravity. These discussions are then followed by reviewing propagation effects in a realistic atmosphere for both free waves and guided waves. Recent numerical results are given. When acoustic-gravity waves propagate through the ionosphere, interaction between the wave and the ionosphere will take place. The physical processes involved in such an interaction are examined.

Yeh, K. C.↗
NASA NTRS1982

A Shuttle Upper Atmosphere Mass Spectrometer /SUMS/ experiment

A magnetic mass spectrometer is currently being adapted to the Space Shuttle Orbiter to provide repeated high altitude atmosphere data to support in situ rarefied flow aerodynamics research, i.e., in the high velocity, low density flight regime. The experiment, called Shuttle Upper Atmosphere Mass Spectrometer (SUMS), is the first attempt to design mass spectrometer equipment for flight vehicle aerodynamic data extraction. The SUMS experiment will provide total freestream atmospheric quantitites, principally total mass density, above altitudes at which conventional pressure measurements are valid. Experiment concepts, the expected flight profile, tradeoffs in the design of the total system and flight data reduction plans are discussed. Development plans are based upon a SUMS first flight after the Orbiter initial development flights.

Blanchard, R. C.↗
NASA NTRS1980

Upper atmosphere modifications due to chronic discharges of water vapor from space launch vehicle exhausts

The influences of transport, photodissociation, and frequency of injection on the global redistribution of water deposited in the earth's upper atmosphere by repeated launches of large rockets are investigated. Measurable environmental effects of the injected water are found to occur when the mesospheric water vapor mixing ratio exceeds 100 ppmv, which occurs over areas of order 20,000 sq km in connection with possible future Satellite Power System activities. These effects include (1) a 50% reduction in D-region ionization due to screening of L alpha radiation by water; (2) a 50% reduction of D-region ionization as a result of converting NO(+) to water cluster ions which possess more rapid recombination rates; (3) a doubling of OH concentrations below 100 km; and (4) a global doubling of nighttime E-region ionization due to L alpha and L beta radiations geocoronally scattered by atomic hydrogen released by photolysis of H2O. Mixing ratios of 1,000 ppmv necessary for the maintenance of clouds at the mesopause are reached only over areas of order 200 sq km.

Forbes, J. M.↗
NASA NTRS1986

Comment on the paper 'On the influx of small comets into the earth's upper atmosphere. II - Interpretation' by L. A. Frank, J. B. Sigwarth and J. D. Craven

The proposal by Frank et al. (1986) that clouds of small comets periodically inject large amounts of H2O into the upper atmospheres of the earth, Venus, and Mars is examined critically, with a focus on transport and disposal mechanisms invoked to account for the large H2O masses involved. It is argued that observed parameter values (such as mixing ratios, vertical wind velocities, and H escape flows) prohibit transport by eddy, molecular diffusion, vertical avection, or coherent movement. In a reply by Frank et al., these objections are discussed in terms of an overall description of the decelerataion and penetration of a cometary water cloud, and H2O concentrations and mixing mechanisms consistent with observed values for the earth are proposed. It is suggested that an increase in cometary H2O influx could lead to concentrations attaining the frost point and to formation of a global mesospheric cloud with significant climate effects. A lower H2O influx rate for Venus (consistent with observed H loss and atmospheric H2O concentration) and relatively rapid loading of the Mars surface and atmosphere with H2O ice and vapor (followed by brief warming periods with increased exospheric H2O outflow and surface flow of liquid H2O) are considered.

Donahue, T. M.↗
NASA NTRS1972

Upper atmospheric probing by resonance fluorescence excited by tunable laser radiation.

Consideration of the application of the measurement of resonance fluorescence radiation excited by tunable laser radiation to the detection of atomic, molecular, and ionic species in the upper atmosphere. The species considered are N2, N2(+), NO, NO(+), O2(+), CO, CO(+), CH, Na, K, and Ca. Calculations of the resonance scattering cross sections, photon returns, and signal-to-noise ratios are given for these species for a range of conditions. Based on a probing altitude of 100 km, the detections of N2, NO, CO, CH, O2, and the trace metals appear feasible with state-of-the-art systems and within the concentration range present in the atmosphere.

Saunders, A. R.↗
NASA NTRS1974

Future monitoring of charged particle energy deposition into the upper atmosphere and comments on possible relationships between atmospheric phenomena and solar and/or geomagnetic activity

The charged particle observations proposed for the new low altitude weather satellites, TIROS-N, are described that will provide the capability of routine monitoring of the instantaneous total energy deposition into the upper atmosphere by the precipitation of charged particles from higher altitudes. Estimates are given to assess the potential importance of this type of energy deposition. Discussion and examples are presented illustrating the importance in distinguishing between solar and geomagnetic activity as possible causative sources.

Williams, D. J.↗
NASA NTRS1983

The structure of Neptune's upper atmosphere - The stellar occultation of 24 May 1981

Observations of the 24 May 1981 occulation of an uncatalogued star by Neptune made at the Cerro Tololo Inter-American Observatory have been analyzed to yield temperature profiles of Neptune's upper atmosphere for number densities near 5 x 10 to the 13th per cu cm. The mean temperatures at immersion (latitude - 56 deg) and emersion (latitude - 16 deg) obtained by numerical inversion were 140 + or - 10 K and 154 + or - 10 K, respectively. The immersion and emersion profiles are remarkably similar in overall shape, suggestive of global atmospheric layering. From the astrometry of the event, precise relative positions of Neptune and the occulted star were obtained.

French, R. G.↗
NASA NTRS1990

Upper atmosphere models and research; Proceedings of Workshops X and XI and the Topical Meeting of the 27th COSPAR Plenary Meeting, Espoo, Finland, July 18-29, 1988

Topics are presented on the updating of CIRA, the trace constituents of the middle and upper atmosphere, and the localized response of the lower thermosphere and ionosphere at high latitude. Papers are presented on mean temperature fields in the lower thermosphere, a comparison of the thermosphere total density model TD 88 with CIRA 86, improved reference models for the middle-atmosphere ozone, a reference model for CH4 and N2O and trends, reference models for thermospheric NO, and a simulation of odd nitrogen distribution in the thermosphere. Other papers are on the response of the ionosphere-thermosphere system to magnetospheric forcing, microinstabilities driven by nonthermal plasma in the high-latitude F-region, the characteristics of the high-latitude trough, the lower thermospheric coupling study of the CEDAR and WITS programs, and numerical simulations of the seasonal response of the thermosphere to propagating tides.

Rycroft, M. J.↗
NASA NTRS1993

Observations of the UARS Particle Environment Monitor and computation of ionization rates in the middle and upper atmosphere during a geomagnetic storm

In this paper we present observations made by the Particle Environment Monitor (PEM) instruments during the geomagnetic storm of 8-9 November, 1991. Ionization and energy deposition rates as functions of altitude in the middle and upper atmosphere by incident electrons and positive ions in the storm interval are computed. The suite of PEM instruments provides a systematic measurement of energetic particles and their associated X-rays over an energy range not fully covered by previous satellite missions.

Sharber, J. R.↗
NASA NTRS1972

Retrograde rotation of the upper atmosphere of Venus.

From June through September 1970, ultraviolet photographs of Venus were obtained by the International Planetary Patrol Program. A study of these photographs, together with some from other observatories, confirms previous reports that there is a retrograde circulation of the upper atmosphere of Venus. The sense of the rotation and its approximate period are determined from the motions of well-defined cloud features on five occasions over intervals of several hours. A distinctive feature similar to the 'Y' described by Boyer and Guerin (1969, 1971) is seen many times over a forty-day interval (June 21 to August 1) and allows a good determination of the rotation period: 4.41 plus or minus 0.02 days retrograde (synodic) or 4.50 days (sidereal). This value differs significantly from other estimates, but applies only to this particular forty-day interval.

Caldwell, J.↗
NASA NTRS2011

Wind and Temperature Spectrometry of the Upper Atmosphere in Low-Earth Orbit

Wind and Temperature Spectrometry (WATS) is a new approach to measure the full wind vector, temperature, and relative densities of major neutral species in the Earth's thermosphere. The method uses an energy-angle spectrometer moving through the tenuous upper atmosphere to measure directly the angular and energy distributions of the air stream that enters the spectrometer. The angular distribution gives the direction of the total velocity of the air entering the spectrometer, and the energy distribution gives the magnitude of the total velocity. The wind velocity vector is uniquely determined since the measured total velocity depends on the wind vector and the orbiting velocity vector. The orbiting spectrometer moves supersonically, Mach 8 or greater, through the air and must point within a few degrees of its orbital velocity vector (the ram direction). Pointing knowledge is critical; for example, pointing errors 0.1 lead to errors of about 10 m/s in the wind. The WATS method may also be applied without modification to measure the ion-drift vector, ion temperature, and relative ion densities of major ionic species in the ionosphere. In such an application it may be called IDTS: Ion-Drift Temperature Spectrometry. A spectrometer-based coordinate system with one axis instantaneously pointing along the ram direction makes it possible to transform the Maxwellian velocity distribution of the air molecules to a Maxwellian energy-angle distribution for the molecular flux entering the spectrometer. This implementation of WATS is called the gas kinetic method (GKM) because it is applied to the case of the Maxwellian distribution. The WATS method follows from the recognition that in a supersonic platform moving at 8,000 m/s, the measurement of small wind velocities in the air on the order of a few 100 m/s and less requires precise knowledge of the angle of incidence of the neutral atoms and molecules. The same is true for the case of ion-drift measurements. WATS also provides a general approach that can obtain non-equilibrium distributions as may exist in the upper regions of the thermosphere, above 500 km and into the exosphere. Finally, WATS serves as a mass spectrometer, with very low mass resolution of roughly 1 part in 3, but easily separating atomic oxygen from molecular nitrogen.

Herrero, Federico↗
NASA NTRS1989

A new means for observation of small comets and other water-laden bodies entering earth's upper atmosphere

This paper shows that the infrared radiance of comet-associated water vapor clouds described by Frank et al. (1986b) is large relative to natural background emissions. This IR emission arises from scattering of solar radiation and earth-shine and from excitation by upper atmospheric atomic oxygen. As a consequence, observations in space or from high-altitude platforms should provide an unambiguous signature of the entry of such objects into earth's atmosphere.

Banks, Peter M.↗
NASA NTRS1981

Satellite observations of upper atmosphere O3 and HNO3 from the Limb Infrared Monitor of the Stratosphere /LIMS/ experiment on Nimbus 7

The Limb Infrared Monitor of the Stratosphere (LIMS) experiment, launched on-board the Nimbus satellite, was designed to measure both day and night limb radiance which is used to infer upper atmosphere temperature profiles and chemical compound concentrations important in the study of ozone chemistry. The LIMS instrument is a six channel, limb scanning, thermal radiometer which uses HgCdTe detectors, cooled to approximately 64 K. Measurements include ozone, water vapor, nitrogen dioxide, and nitric acid. The ozone and nitric acid channels are centered at approximately 9.6 microns and 11.3 microns, respectively. Results from the channels are described with an emphasis on data validation. The O3 and HNO3 channels have demonstrated high measurement precision.

Russell, J. M., III↗
NASA NTRS1987

The precipitation of energetic heavy ions into the upper atmosphere of Jupiter

Evidence for auroral particle precipitation at Jupiter was provided by the ultraviolet spectrometers onboard the Voyagers 1 and 2 spacecraft and by the International Ultraviolet Explorer (IUE). Magnetospheric measurements made by instruments onboard the Voyager spacecraft show that energetic sulfur and oxygen ions are precipitating into the upper atmosphere of Jupiter. A theoretical model has been constructed describing the interaction of precipitating oxygen with the Jovian atmosphere. The auroral energy is deposited in the atmosphere by means of ionization, excitation, and dissociation and heating of the atmospheric gas. Energetic ion and electron precipitation are shown to have similar effects on the atmosphere and ionosphere of Jupiter.

Horanyi, M.↗
NASA NTRS1988

The precipitation of energetic heavy ions into the upper atmosphere of Jupiter

Evidence for auroral particle precipitation at Jupiter was provided by the ultraviolet spectrometers on board the Voyager 1 and 2 spacecraft and by the International Ultraviolet Explorer. Magnetospheric measurements made by instruments on board the Voyager spacecraft indicate that energetic sulfur and oxygen ions are precipitating into the upper atmosphere of Jupiter. A theoretical model describing the interaction of precipitating oxygen with the Jovian atmosphere was constructed. The auroral energy is deposited in the atmosphere by means of ionization, excitation, and dissociation and heating of the atmospheric gas. Energetic ion precipitation and electron precipitation are shown to have similar effects on the atmosphere and ionosphere of Jupiter.

Horanyi, M.↗
NASA NTRS1981

The rotation period of Neptune's upper atmosphere

The variations in the near-infrared brightness of Neptune observed during July and August 1980 show a well-defined, large-amplitude variation in Neptune's J-K color, with a period of 17.73 + or - 0.1 hour. These results are interpreted as diurnal variations resulting from the 17.73-hour rotation period of the Neptune upper atmosphere in the presence of inhomogeneous weather, and are found to qualitatively corroborate those of Cruikshank (1978). It is also noted that Smith and Slavsky (1980) report a 17.7-hour component as a secondary periodicity in their data. Variations were observed in the 5-0-micron spectral region which are in phase with the variations seen at shorter wavelengths.

Brown, R. H.↗