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Keating, G. M.

Publications and source records attributed to Keating, G. M..

At least 55 records · Page 3
All sourcesNASA NTRSDOE OSTI
NASA NTRS1981

Global ozone - Solar activity relationship from satellite measurements

Global ozone variations are evaluated by analyzing satellite measurements, using the technique of integrating out dynamical effects causing large variations in total ozone at individual locations. Analysis of Nimbus 4 reprocessed BUV data was extended to cover the period from April 1970 through December 1975. Temporal and latitudinal variation of biases and yearly change in global biases between the satellite and ground based ozone measurements are indicated. The bias-corrected 6-month-running filtered global means are shown, and the correlation coefficient between ozone and the solar activity index remains high at 0.94. It is concluded that the results give a strong indication of an ozone-solar activity relationship that is caused by solar UV variability.

Keating, G. M.↗
NASA NTRS1980

Venus upper atmosphere structure

Atmospheric densities of Venus were measured from the orbital decay of the Pioneer Venus from Dec. 9, 1978 to Aug. 7, 1979 near the 16 deg latitude between 140 and 190 km during the entire day. Comparative atmospheric densities on earth at 150 km are higher by a factor of 3.5 with only a 1% diurnal variation; an atmospheric composition, temperature, and density model based on the orbiter atmospheric drag (OAD) vertical structure is presented. The model shows that atomic oxygen is the major component in the Venus atmosphere above 145 km at night and above 160 km during the day with mixing ratios over 0.1 near 140 km; drag measurements indicate O concentrations from 1 x 10 to the 9th/cu cm in daytime to 3 x 10 to the 7th/cu cm at night. It is concluded that the neutral upper atmosphere of Venus is surprisingly insensitive to solar extreme UV variations and changes in the solar wind.

Keating, G. M.↗
NASA NTRS1979

Short-term cyclic variations and diurnal variations of the Venus upper atmosphere

The vertical structure of the nighttime thermosphere and exosphere of Venus was discussed. A comparison of the day and nighttime profiles indicates, contrary to the model of Dickinson and Riley (1977), that densities (principally atomic oxygen) dropped sharply from day to night. It was suggested either that the lower estimates were related to cooler exospheric temperatures at night or that the atomic bulge was flatter than expected at lower altitudes. Large periodic oscillations, in both density and inferred exospheric temperatures, were detected with periods of 5 to 6 days. The possibility that cyclic variations in the thermosphere and stratosphere were caused by planetary-scale waves, propagated upward from the lower atmosphere, was investigated using simultaneous temperature measurements obtained by the Venus radiometric temperature experiment (VORTEX). Inferred exospheric temperatures in the morning were found to be lower than in the evening as if the atmosphere rotated in the direction of the planet's rotation, similar to that of earth. Superrotation of the thermosphere and exosphere was discussed as a possible extension of the 4-day cyclic atmospheric rotation near the cloud tops.

Keating, G. M.↗
NASA NTRS1979

Venus thermosphere and exosphere - First satellite drag measurements of an extraterrestrial atmosphere

Atmospheric drag measurements obtained from the study of the orbital decay of Pioneer Venus I indicate that atomic oxygen predominates in the Venus atmosphere above 160 kilometers. Drag measurements give evidence that conditions characteristic of a planetary thermosphere disappear near sundown, with inferred exospheric temperatures sharply dropping from approximately 300 K to less than 150 K. Observed densities are generally lower than given by theoretical models.

Keating, G. M.↗
NASA NTRS1978

Relation between monthly variations of global ozone and solar activity

Monthly averaged variations of global ozone determined from infrared interferometer spectrometer measurements aboard Nimbus 4 are shown to be consistently in agreement with monthly averaged variations of solar activity. The relationship between monthly changes of ozone and solar activity are found to be generally consistent with the longer-term variations of ozone over the last solar cycle and can be accounted for by assuming monthly solar flux variations near 0.2 micron of about 2%.

Keating, G. M.↗
NASA NTRS1978

Comparison of ozone concentrations obtained from Skylab eclipse and ozonesonde measurements

The satellite eclipse technique of ozone measurement is evaluated to determine its accuracy and resolution. The method of obtaining ozone concentrations from ground-based observations of eclipsing satellites is described, the theory of this method is outlined, and the data reduction procedure is summarized. It is shown that the satellite eclipse technique successfully measures the vertical distribution of ozone from 15 to 40 km with precisions ranging from + or - 12% between 20 and 35 km and + or - 25% at both 15 and 40 km. The ozone profile is found to be in good agreement with in situ measurements obtained from an ozonesonde launched near the eclipse tangent point at local sunset, the percent differences being less than 14% from 20 to 40 km.

Mcdougal, D. S.↗
NASA NTRS1977

Global exospheric temperatures from ESRO 4 scale height measurements

The scale height temperatures considered are based on molecular nitrogen measurements by the gas analyzer aboard the ESRO 4 in the altitude range from 280 to 310 km during the interval from December 1972 to April 1974, a period of low solar activity. At the altitude of measurement during the considered period, the scale height temperature is essentially the exospheric temperature. The mean scale height temperature derived from 1833 independent N2 scale heights is 708 K. It is concluded that the ESRO 4 data provides evidence of mean global temperatures of less than 800 K.

Keating, G. M.↗
NASA NTRS1977

Composition and structure of the atmosphere of Venus

Some of the main questions regarding the composition, structure, and origin of the atmosphere of Venus are posed. These questions are (1) the distribution of the constituents of the lower atmosphere, (2) cloud composition, (3) the planet's surface and interior as revealed by atmospheric data, (4) the state property profiles and their variation over the planet, (5) the reason for the high temperatures of the lower atmosphere, (6) composition and temperature profiles of the upper atmosphere and location of the homopause, (7) spatial and temporal variations in the upper atmosphere, (8) the cause of the stability of CO2 - global circulation or local turbulence, (9) influence of neutral composition on the thermal structure, (10) response of upper atmosphere to change in solar EUV and solar wind, (11) the source and destination of the atmosphere, and (12) the location of Venus's water. The main parameters to be measured which will aid in resolving these problems are enumerated.

Hoffman, J. H.↗
NASA NTRS1977

Comparison of drag and mass spectrometer measurements during small geomagnetic disturbances

During small geomagnetic disturbances, ESRO 4 and OGO 6 gas analyzer measurements at high altitudes suggest that helium and atomic oxygen concentrations in the lower thermosphere decrease, whereas satellite drag measurements indicate that density increases. This discrepancy is explained by the corresponding temperature increases maximizing at high latitudes. ESRO 4 data suggest that at altitudes where atomic oxygen or helium predominates, the temperature increase compensates for the decrease in lower thermospheric concentrations. This yields a net density increase with geomagnetic disturbances. The Explorer 39 drag satellite measurements verify this conclusion. It is felt that the composition variations associated with minor disturbances indicate the upwelling of the polar atmosphere, circulation towards the equator, and subsidence in the equatorial region. ESRO measurements show that at low latitudes the increases in helium concentrations with geomagnetic disturbances are chiefly caused by the circulation from high latitudes and the subsidence at lower latitudes.

Keating, G. M.↗
NASA NTRS1974

Helium in the Martian atmosphere - Thermal loss considerations

Helium concentrations in the Martian atmosphere are estimated assuming that the helium production on Mars (comparable to its production on earth) via the radioactive decay of uranium and thorium is in steady state equilibrium with its thermal escape. Although nonthermal losses would tend to reduce the estimated concentrations, these concentrations are not necessarily an upper limit since higher production rates and/or a possibly lower effective exospheric temperature over the solar activity cycle could increase them to even higher values. The computed helium concentration at the Martian exobase (200 km) is 8 million atoms/cu cm. Through the lower exosphere, the computed helium concentrations are 30-200 times greater than the Mariner-measured atomic hydrogen concentrations. It follows that helium may be the predominant constituent in the Martian lower exosphere and may well control the orbital lifetime of Mars-orbiting spacecraft.

Levine, J. S.↗
NASA NTRS1973

The Air Density Explorer Satellite Program

Since 1961, four satellites designed specifically for determination of the density and composition variations of the earth's neutral atmosphere at satellite altitudes have been launched: Explorer 9, Explorer 19, Explorer 24, and Explorer 39. Studies of the orbital decay of these satellites have resulted in major revisions in our conception of the upper atmosphere at satellite altitudes. These features include the winter helium bulge detected near 1000 km with its north-south asymmetry, the summer atomic oxygen bulge near 500 km, and the winter enhancement of atomic oxygen near 120 km. The Langley Research Center is now in the process of designing and fabricating the Dual Air Density Explorers. These will be two satellites launched by means of a single Scout rocket in 1975, and they are expected to remain in essentially the same orbital plane throughout the 2-year mission. Each satellite is drag sensitive and uses a mass spectrometer in a unique system which is insensitive to orientation, is highly sensitive to the upper atmosphere, and is capable of in-flight calibration.

Keating, G. M.↗
NASA NTRS1972

North-South asymmetry of the neutral exosphere.

A systematic asymmetry in the neutral exosphere between the Northern and Southern Hemispheres has been identified for the first time after correcting for all other known systematic variations. This phenomenon was clearly detected from recent measurements of helium drag effects near 1000 km on the low mass-to-area ratio Explorer 19 satellite. From a reanalysis of all four NASA Langley Air Density Explorer satellites (Explorers 9, 19, 24, and 39), this systematic asymmetry was traced over an entire solar activity cycle. It was found that helium concentrations in local summer at high latitudes are generally more than 50% lower in the Southern Hemisphere than in the Northern Hemisphere. In addition, the increase in helium concentrations from summer to winter was found to be approximately 80% greater in the Southern Hemisphere than in the Northern Hemisphere.

Keating, G. M.↗
NASA NTRS1971

Neutral upper atmosphere structure

Neutral thermosphere and exosphere structure, discussing density, temperature, composition and diurnal and seasonal variations

Keating, G. M.↗