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Simultaneous Thomson scatter measurements for middle and low latitudes, comparing electron density and temperature and exospheric and global temperature distributions
Maximum to minimum exospheric temperature ratio determination, concluding solar wind dependence of diurnal variation in thermosphere
Modified expression for exospheric temperature in Jacchia static diffusion models of upper atmosphere in polar regions
Radar based values of neutral night exospheric temperature, discussing dominant effect of annual variation
Thermospheric hydrogen density and temporal variations from Explorer 32 measurements, discussing dependence on exospheric temperature
Neutral thermosphere and exosphere structure, discussing density, temperature, composition and diurnal and seasonal variations
Exospheric evening temperature behavior data, using Fabry-Perot interferometer measurements of atomic oxygen line Doppler broadening
Atomic hydrogen dayglow Lyman alpha structure of Mars exosphere from Mariner 6 and 7 UV spectrometric observations
Fabry-Perot interferometer measurements of atomic oxygen 6300 A and 5577 A line profiles from twilight and nightglow are used to determine the neutral temperatures in F2 and E regions of the earth's ionosphere. The exospheric temperatures T sub n (infinity) determined from the 6300 A profiles are usually somewhat higher than those calculated from Jacchia's model, with differences as large as approximately 300 K noted when T sub n (infinity) = 1500 to 1600 K. The post-sunset and pre-dawn rate of change of T sub n (infinity) is often substantially larger than the Jacchia prediction. The 5577 A (E-region) measured temperatures range from 200 to 220 K on quiet nights to 500 to 600 K during geomagnetic storms.
The analysis of composition measurements made with the neutral mass spectrometer aboard the OGO-6 satellite leads to the following conclusions. The measured atomic oxygen densities are generally in good agreement with those deduced from drag. The molecular nitrogen densities in the annual and semiannual variations depart significantly from those predicted by drag models and suggest similar departures for exospheric temperatures. The helium densities generally tend to vary in an inverse manner to the nitrogen densities. These composition changes are consistent with dynamical processes associated with the global circulation in the thermosphere.
Discussion of the implications of low concentration of Martian nitrogen as reflected in the apparent failure of the ultraviolet spectrometers on Mariner 6 and Mariner 7 to detect molecular nitrogen. If eddy mixing is about as effective on Mars as it is on earth, then there seems to be less nitrogen present on Mars than would be expected if terrestrial-type outgassing were operating. It is shown that, in this case, a nonthermal escape mechanism involving the predissociation of exospheric nitrogen can be used to explain the low nitrogen concentration.
The Mariner 6 and 7 UV spectrometer experiments observed intense emissions from CO, O, and CO2(+) in the Martian airglow. Analysis shows that they are excited predominantly by the absorption of solar EUV photons by CO2 and constitute a major energy-loss mechanism for the thermosphere. Models of the thermospheric temperature profile and the airglow layer that demonstrate the effects of neutral chemistry and ionospheric composition are developed. With their aid, the observed CO Cameron-band emission scale height of 19 (plus or minus 4.5) km is shown to suggest an exospheric temperature of 315 (plus or minus 75) K. Consideration of other data suggests a 'best' value of about 350 K. Within the uncertainties in the excitation efficiencies and in the thermospheric cooling mechanisms, the observations are consistent with the measured electron density. There is no indication in the data that the ionosphere is modified by the solar wind below 200 km.
Simultaneous airglow and electron content measurements made at Hawaii are used to infer the number of 6300 and 6364 A quanta produced per electron lost in the nighttime F layer of the ionosphere. The equation of continuity of electrons is then solved numerically to obtain the electron density profile, and the amount of quenching is estimated. This leads to the number of excitations of O(super-1 D) per O2(+) recombination (epsilon). We find, for an exospheric temperature of 1100 K, epsilon is equal to 1.1 plus or minus 0.6, in good agreement with Zipf's laboratory measurement at 300 K.
Densities derived from the drag of five artificial satellites and covering the time interval from 1958 to 1971 have been used to study the variations in the thermosphere arising from changes in solar activity. Exospheric temperatures derived from the densities by means of atmospheric models have been related to the 10.7-cm solar flux, in which the active-area component had been separated from the slow-varying clear-disk component by means of a relation between the flux and sunspot areas. When the day-to-day (27-day) variation is suppressed, the remaining slow temperature variation appears to be linearly related to the clear-disk flux component. If we also relate linearly the day-to-day temperature variations with the day-to-day variations of the flux, we find that the regression coefficient changes from 1 K at sunspot maximum to 2 K at low solar activity; a nearly constant coefficient is obtained by relating the temperature variations to the ratio of the active-area component to the clear-disk component of the flux.
This paper reports some preliminary results from the suprathermal ion detectors deployed on the lunar surface by the Apollo 12 and 14 astronauts. Salient features of these results include: the possible observation of sporadic venting of gas from the lunar surface; evidence for a prompt ionization and acceleration mechanism operating in the lunar exosphere; and a preliminary measurement yielding approximately 1 month for the e-folding decay time for the heavier components of the exhaust gases from the Apollo lunar landing systems. Prominent phenomena from which these results have been derived are: (1) ion bursts of low to moderate energy seen in conjunction with lunar sunrise and sunset; (2) solar wind energy ions detected on the night side of the moon; (3) ions of several keV energy seen during the lunar sunset to midnight quadrant of the moon's orbit; (4) magnetosheath ion flux enhancements; (5) ion bursts generated by the lunar impact of the Apollo 13 Saturn upper stage; and (6) geomagnetic storm associated ion flux variations in the earth's magnetotail.
Analysis of the O I 1304- and 1356-A data from Mariner 6 and 7, and estimation of the atomic oxygen concentration of the Martian atmosphere. Derived values of the parameters describing the sources of excitation differ considerably from previous estimates. A detailed statistical treatment is used in the analysis. At an exospheric temperature of 350 K the atomic oxygen concentration at 135 km is estimated to be between 0.5 and 1%. The likely source of the 1304-A intensity is resonance scattering of solar 1304-A photons. For the 1356-A emission, the likely source is photodissociation of CO2. There is an indication of a diurnal variation of the Martian upper atmosphere.
Energy and diffusive mass transport associated with the thermospheric circulation are considered in a self-consistent, though mathematically relatively simple form to describe in a three-dimensional two-constituent model magnetic storm characteristics in composition (N2, O, and He), temperature and mass-density. It is shown that during disturbed conditions the latitudinal variations of composition and gas temperature T sub g reflect the local nature of the magnetic storm heat input assumed to be primarily confined to the auroral zones. Thereby T sub g and N2 increase, He decreases and O remains constant through the auroral zones at exospheric heights (due to the superposition of temperature and diffusion effects) in agreement with OGO-6 mass spectrometer measurements. In contrast, the magnetic storm response in the total mass density is characterized by a strong world-wide component and a relatively insignificant increase toward the poles with the density peak occurring between two (poles) and eight (equator) hours after the maximum energy input, in substantial agreement with satellite drag data.
An empirical global model for magnetically quiet conditions has been derived from longitudinally averaged N2, O, and He densities by means of an expansion in spherical harmonics. The data were obtained by the OGO-6 neutral mass spectrometer and cover the altitude range 400 to 600 km for the period 27 June 1969 to 13 May 1971. The accuracy of the analytical description is of the order of the experimental error for He and O and about three times experimental error for N2, thus providing a reasonable overall representation of the satellite observations. Two model schemes are used: one representing densities extrapolated to 450 km and one representing densities extrapolated to 120 km with exospheric temperatures inferred from N2 densities. Using the best fit model parameters the global thermospheric structure is presented in the form of a number of contour plots.