Engineering topics

Fox, J. L.

Publications and source records attributed to Fox, J. L..

45 records · Page 3

NASA NTRS1985

The vibrational distribution of N2(+) in the terrestrial ionosphere

The densities and vibrational distributions of N2(+) in the X2sigma g +, A2Pi u and B2sigma u + states in the daytime terrestrial ionosphere are computed for both low and high solar activity. Altitude profiles of the relative populations of the vibrational levels of N2(+) X2sigma g + are presented. The fraction of vibrationally excited N2(+) varies from 5 percent at 100 km to 50 percent at 450 km. Several models are examined in which loss of N2(+)(v) is enhanced for v greater than 0 and in which various assumptions are made about the vibrational distributions produced in charge transfer reactions. The N2(+) densities are significantly reduced if N2(+)(v) reacts with O at rates which are near gas-kinetic. Vibrational distributions of the A2pi u and B2sigma u + states are also presented, as well as volume emission rates and integrated overhead intensities of the major bands of the Meinel and first negative systems.

Fox, J. L.↗

NASA NTRS1985

The O2(+) vibrational distribution in the Venusian ionosphere

The vibrational distribution of O2(+) in the ionosphere of Venus was calculated for a model atmosphere (similar to one discribed by Fox, 1982), based on data from the Pioneer Venus neutral mass spectrometer. The calculation of the ion densities includes both chemistry and diffusion. At 100 km, quenching precludes survival of vibrationally excited 02(+). At the exobase, near 200 km, more than half of O2(+) molecules are vibrationally excited. The effects of vibrationally excited O2(+) on the hot oxygen coronas and the airglow are discussed.

Fox, J. L.↗

NASA NTRS1984

Studies of the chemistry of vibrationally and electronically excited species in planetary upper atmospheres

The vibrational distribution of O2(+) in the atmospheres of Venus and Mars was investigated to compare with analogous values in the Earth's atmosphere. The dipole moment of the Z(2) Pi sub u - X(2) Pi sub g transition of O2(+) is calculated as a function of internuclear distance. The band absorption oscillator strengths and band transition probabilities of the second negative system are derived. The vibrational distribution of O2(+) in the ionosphere of Venus is calculated for a model based on data from the Pioneer Venus neutral mass spectrometer.

Fox, J. L.↗

NASA NTRS1984

Radiative lifetimes of the second negative system of O2(+)

The dipole moment of the A2Pi(u)-X2Pi(g) transition of O2(+) is calculated as a function of internuclear distance using ab initio methods. The band absorption oscillator strengths and band transition probabilities of the second negative system are derived and the resulting lifetimes are compared with experimental data. The high-lying v double prime levels of the ground state may decay into low-lying v prime levels of the excited state. The corresponding radiative lifetimes are calculated.

Wetmore, R. W.↗

NASA NTRS1983

Nitrogen escape from Mars

The escape rate of nitrogen from Mars is calculated to be 2.3 x 10 to the 5th per sec for low solar flux conditions and 8.9 x 10 to the 5th per sec for high solar flux conditions. The major source of energetic atoms is dissociative recombination of ground state and vibrationally excited N2(+) ions. The measured N-15/N-14 isotope ratio can be reproduced by postulating an early dense atmosphere during which little differentiation occurred.

Fox, J. L.↗

NASA NTRS1982

A stratospheric chemical instability

The equations which determine partitioning of Cl(x) in steady state have multiple (three) solutions under conditions which might arise in the high-latitude winter stratosphere. Two of these solutions are stable, one is unstable, to infinitesimal perturbations. The relative stability of solutions is examined by subjecting the system to finite perturbations. The more stable solution is found to eliminate the less stable when semi-infinite volumes of the two solutions are placed in contact. The high-ClO, low NO2 solution is more stable under most conditions. Transitions from less to more stable states are slow in winter but may occur more rapidly when the seasonal variation of insolation is taken into account.

Fox, J. L.↗

NASA NTRS1982

Atomic carbon in the atmosphere of Venus

The densities of atomic carbon in the Venusian thermosphere are computed for a model which includes both chemistry and transport. The maximum density of C is 2.8 x 10 to the 7th per cu cm near 150 km for an assumed O2 mixing ratio of 0.0001. Photoionization of atomic carbon is found to be the major source of C(+) above 200 km, and resonance scattering of sunlight by atomic carbon may be the major source of the C I emissions at 1561 A, 1657 A, and 1931 A. The computed C(+) densities are found to be in substantial agreement with those measured by Pioneer Venus.

Fox, J. L.↗

NASA NTRS1982

The chemistry of metastable species in the Venusian ionosphere

Reactions of metastable species are important in determining the densities of minor ions in the Venusian ionosphere. Calculations are carried out in which the coupled continuity and momentum equations are solved for twelve ions and four neutral species in the dayside ionosphere, including O(+)(2D), O(2P), N(2D), and N(2P). Altitude profiles of these metastable species are presented. Their reactions are shown to be a significant source of several minor ions, especially N2(+), CO(+), and N(+). The discrepancies which existed between model and measured densities of these ions are resolved.

Fox, J. L.↗

NASA NTRS1981

Studies of the role of metastables and doubly ionized species in the chemical and thermal structure of the Venusian and Martian ionospheres

Models of the upper atmospheres of Mars and Venus were constructed using Viking and Pioneer Venus data. The neutral densities, with the exception of NO, N(4S), N(2D) and N(2P) were taken from the measured values, along with the neutral, ion, and electron temperatures. Using solar fluxes and relevant cross sections, the production rates of ions and neutral fragments by photo and electron impact processes were computed. These production rates were combined with chemical production rates and loss along with one dimensional transport eddy diffusion, molecular and ambi polar diffusion, and thermal diffusion, to determine the densities of ions and odd nitrogen species. Preliminary calculations show that the chemistry of metastables and doubly ionized species is important in the ionospheres of Mars and Venus. Production of N(+) in metastable reactions is particularly important, and it explains the discrepancy between the measurements of earlier models. Production of CO(+) is also affected. Reactions of O(++) and O(+)(2D) with N2 have important consequences for the escape rate of atomic nitrogen from the Martian atmosphere.

Fox, J. L.↗