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Froidevaux, L.

Publications and source records attributed to Froidevaux, L..

105 records · Page 6
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NASA NTRS1993

The evolution of ozone observed by UARS MLS in the 1992 late winter southern polar vortex

The evolution of ozone (O3) observed by the Microwave Limb Sounder on board the Upper Atmosphere Research Satellite is described for 14 Aug through 20 Sep 1992, in relation to the polar vortex. The development of an ozone hole is observed in column O3, and a corresponding decrease is seen in O3 mixing ratio in the polar lower stratosphere, consistent with chemical destruction. The observations also suggest that poleward transport associated with episodes of strong planetary wave activity is important in increasing O3 in the mid-stratosphere.

Manney, G. L.↗
NASA NTRS1993

Microwave Limb Sounder measurement of stratospheric SO2 from the Mt. Pinatubo volcano

The Microwave Limb Sounder (MLS) experiment on the Upper Atmosphere Research Satellite (UARS) began atmospheric measurements on September 19, 1991. Residual SO2 from the Pinatubo eruption was detected immediately after instrument activation. The SO2 was 1ocated in a tropical band with peak mixing ratios of about 15 ppbv near 26 km altitude. The observed decay of SO2 has provided an estimate of the OH concentration in the plume.

Read, W. G.↗
NASA NTRS1993

Stratospheric ClO and ozone from the Microwave Limb Sounder on the Upper Atmosphere Research Satellite

Concentrations of atmospheric ozone and of ClO (the predominant form of reactive chlorine responsible for stratospheric ozone depletion) are reported for both the Arctic and Antarctic winters of the past 18 months. Chlorine in the lower stratosphere was almost completely converted to chemically reactive forms in both the northern and southern polar winter vortices. This occurred in the south long before the development of the Antarctic ozone hole, suggesting that ozone loss can be masked by influx of ozone-rich air.

Waters, J. W.↗
NASA NTRS1988

Measurements of odd nitrogen compounds in the stratosphere by the ATMOS experiment on Spacelab 3

Spacelab 3's Atmospheric Trace Molecule Spectroscopy (ATMOS) experiment has obtained 30 deg N and 48 deg S vertical profiles of reservoir gases, source gases, and other trace molecules that are important in the middle atmosphere's odd nitrogen, odd chlorine, and odd hydrogen chemical families. The abundances of individual gases and total odd nitrogen levels measured by ATMOS have been compared with prior results obtained from balloon and satellite platforms. The lower-limit profile agrees with ATMOS data to within 16 percent up to 42 km altitude.

Russell, J. M., III↗
NASA NTRS1985

A critical analysis of CLO and O3 in the mid-latitude stratosphere

The Caltech one-dimensional photochemical model is used to analyze important questions concerning the upper stratospheric O3 and the key HO(x), NO(x), and ClO(x) free radicals. The model is described and first order effects of the inclusion of diffuse radiation in a spherical rather than plane parallel atmosphere at solar zenith angles close to 90 deg are assessed. A comparison is made between photochemical theory and observations for upper stratospheric O3, where local photochemistry rather than dynamics should control the O3 abundance. The photochemical equilibrium relation for odd oxygen is studied, including the important radicals involves. It is concluded that a significant model ozone deficit exists in the upper stratosphere. Possible causes for such a discrepancy are investigated in light of current model and experimental uncertainties. In particular, the observational ratio of atomic oxygen to zone appears to disagree with the model results.

Froidevaux, L.↗
NASA NTRS1985

Oxygen species

The spatial distribution of ozone, as predicted by numerical models, is compared with observations. A set of reference ozone profiles was developed against which to compare current numerical calculations. Most of the analyses will focus on ozone between 30 and 70 km altitude.

Brasseur, G.↗
NASA NTRS1982

Radiation and chemistry in the stratosphere - Sensitivity to O2 absorption cross sections in the Herzberg continuum

It is suggested that the discrepancies between observed and modeled vertical profiles of such halocarbons as CFCl3, as well as the problem of simultaneously fitting N2O, CH4, CF2Cl2 and CFCl3 profiles with a single eddy diffusion model, are due to an overestimation of the molecular oxygen absorption cross sections in the 200-220 nm spectral region. The replacement of current O2 cross sections in this range with values that are in better agreement with results for the compounds cited leads to N2O, CF2Cl2 and CFCl3 concentration reductions of factors 0.70, 0.62 and 0.19, respectively. Profiles of CH4, H2 and CO remain unchanged, and the predicted concentration of HNO3 above 30 km is reduced by about 50% for yet another improved fit with observations. It is noted that the correction proposed produces a 30% ozone increase near the 20-25 km peak.

Froidevaux, L.↗
NASA NTRS1981

Saturn's rings - Infrared brightness variation with solar elevation

The main subject of the discussed investigation is the infrared brightness variation of the A, B, and C rings, as a function of solar elevation. Existing models for the B ring are not entirely satisfactory. A description is presented of a model applicable to all three rings. This model and other existing models are compared with the available data. Particular attention is given to the 20-micrometer observations of Saturn's rings. It is found that the brightness variation of the A and B rings with solar elevation angle can be well modeled by an optically thick monolayer of particles, or equivalently, a flat sheet, emitting on one side only. This points to a temperature contrast between the two sides of the ring plane. The infrared brightness of the C ring increases as the solar elevation angle with respect to the ring plane decreases.

Froidevaux, L.↗
NASA NTRS1981

Thermal response of Saturn's ring particles during and after eclipse

The investigation is based on data which were obtained on May 18, 1978, at the 5-m Hale telescope on Palomar Mountain. A Ge:Ga bolometer was used at the f/70 Gregorian focus; a cold interference filter limited the wavelength response to between 16 and 26 micrometers. A brightness asymmetry is observed between the ansae of all three rings; the largest asymmetry occurs in the C ring. The simplest explanation of such asymmetries is just the eclipse cooling and subsequent heating of similar particles at different radial distances from Saturn, coupled with the different travel times from eclipse exit to east ansa. The observed eclipse cooling and subsequent heating in Saturn's B ring support the idea that the uppermost surface of the particles is of low-conductivity water frost, similar to the uppermost surface of the Galilean satellites (omitting Io).

Froidevaux, L.↗
NASA NTRS1981

Scientific results from the Pioneer Saturn infrared radiometer

Data on Saturn and its rings are presented, obtained by the Pioneer 11 infrared radiometer in broadband channels, centered at 20 and 45 microns. Assuming symmetry about the equator and a constant flux poleward of 7.5 deg latitude, an average effective temperature of 96.5 + or - 2.5 K indicates a total emission which is 2.8 times that of the absorbed sunlight. Temperatures at the 1 bar level are 137 and 140 K, and a minimum temperature averaging 87 K is registered near the 0.06 bar level. Ring boundaries and optical depths are consistent with those at optical wavelengths. Ring temperatures are 54-86 K on the south side, approximately 54 K on the north side, and at least 67 K in Saturn's shadow.

Orton, G. S.↗
NASA NTRS1980

Radial diffusion in Io's torus - Some implications from Voyager I

Data from several Voyager 1 experiments are used to determine the magnitude and L dependence of the radial diffusion coefficient for low-energy charged particles outside of Io's orbit under steady-state conditions. The extreme ultraviolet observations near 685A are inverted to produce an ion density profile for L greater than 6. This normalized ion profile as well as the (equatorial) electron density profile estimated from the planetary radio astronomy (PRA) observations falls off as L to the -5th. Such a density gradient would make possible centrifugally driven cross-L diffusion outside of Io's orbit without ruling out the presence of an atmospherically driven mechanism. A lower limit for the radial diffusion coefficient DLL is 1.5 x 10 to the -10th L to the 5th (Jupiter radii squared per sec), yielding a characteristic diffusion time from 6RJ to 7RJ of less than 10 days, much shorter than previously anticipated. Steady-state diffusion is not a good assumption inside of Io's orbit, where the particle densities decrease sharply from 6 Jupiter radii to 5 Jupiter radii; the diffusion time in that region is probably longer than outside of Io's orbit.

Froidevaux, L.↗
NASA NTRS1978

A time dependent model of the Jovian current sheet

Analysis of vector helium magnetometer measurements during the Pioneer 10 outbound pass through the Jovian magnetosphere reveals that the average location of the near-equatorial current sheet is a surface whose shape is determined by the velocity at which the magnetic perturbations produced by a rotating tilted dipole propagate to large radial distances. A model is presented which is a surface encircling the planet and rotating rigidly with it. Based on a linear fit to the times of the current sheet crossings, a formula is derived for the surface representing the average position of the near-equatorial current sheet in the Jovian magnetosphere.

Kivelson, M. G.↗