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## Abstract

During two flights of a balloon-borne coronagraph to a maximum altitude of 25 km, observations of the wavelength distribution of skylight from 0.37 μ to 0.79 μ at a scattering angle of 2°4 as well as the angular distribution at γ=0.44 μ from scattering angles 1°7 to 58° were secured.

At 25 km the daytime sky radiance at a scattering angle of 2°4 is still nearly twice that expected from the Rayleigh sky. At a scattering angle of 10° the observed radiance exceeds the Rayleigh value by only about 10 per cent. At 20° and beyond the two are nearly indistinguishable. The angular and wavelength distributions of the light scattered by the aerosols are used to determine the parameters of the size distribution and the number of contaminating particles above the apparatus. Comparison of calculated angular distributions with the observations shows that between *r*=0.3 μ and 3.0 μ the particle size distribution is fairly well determined, varying as the −3.5 power of the radius in the stratosphere. An investigation is also made of how uniquely the observations are able to determine the parameters of the size distribution of the scattering particles.

Differentiation with respect to height of the inferred concentrations per cm^{2} column above a particular altitude yields the local particle concentration at any altitude. A broad relative maximum in particle concentration or “dust layer” exists at 20 km. The distribution of particle sizes at this altitude as determined by the scattered skylight compares favorably with the distributions determined by direct sampling. We conclude that many of these particles are of stratospheric origin. The observations also demonstrate the existence of extremely thin laminae of scattering particles in the stratosphere. The data allow determination of the optical depth caused by large particles in the atmosphere. At 25 km the optical depth for the non-molecular component is approximately 2×10^{−4}.

The variation of particle concentration with height above 20 km is interpreted on the assumption that two mechanisms transport particles–eddy diffusion, which carries particles upwards, and sedimentation, which transports meteoric debris downwards. The eddy diffusion coefficient in the altitude range 20 to 25 km is found to he approximately 5000 cm^{2} sec^{−1}. The observations also allow the influx of meteoric particles to be determined. The meteoric influxes inferred in this manner are compared with those determined from rocket and satellite experiments, estimates of meteoric dust settling in the air or deposited on the ground, and from the analysis of the zodiacal light. This comparison leads to the conclusions that: 1) a geocentric condensation of the interplanetary dust of approximately a factor of 10^{3} exists in the neighborhood of the earth; 2) this geocentric concentration is most effective for particles in the size range 0.3 μ to 10 μ; 3) a majority of the particles in the earth's dust cloud are in geocentric, quasi-closed orbits. It is also demonstrated that meteoric dust represents a negligible fraction of the particulate matter below 20 km in the earth's atmosphere.

## Abstract

During two flights of a balloon-borne coronagraph to a maximum altitude of 25 km, observations of the wavelength distribution of skylight from 0.37 μ to 0.79 μ at a scattering angle of 2°4 as well as the angular distribution at γ=0.44 μ from scattering angles 1°7 to 58° were secured.

At 25 km the daytime sky radiance at a scattering angle of 2°4 is still nearly twice that expected from the Rayleigh sky. At a scattering angle of 10° the observed radiance exceeds the Rayleigh value by only about 10 per cent. At 20° and beyond the two are nearly indistinguishable. The angular and wavelength distributions of the light scattered by the aerosols are used to determine the parameters of the size distribution and the number of contaminating particles above the apparatus. Comparison of calculated angular distributions with the observations shows that between *r*=0.3 μ and 3.0 μ the particle size distribution is fairly well determined, varying as the −3.5 power of the radius in the stratosphere. An investigation is also made of how uniquely the observations are able to determine the parameters of the size distribution of the scattering particles.

Differentiation with respect to height of the inferred concentrations per cm^{2} column above a particular altitude yields the local particle concentration at any altitude. A broad relative maximum in particle concentration or “dust layer” exists at 20 km. The distribution of particle sizes at this altitude as determined by the scattered skylight compares favorably with the distributions determined by direct sampling. We conclude that many of these particles are of stratospheric origin. The observations also demonstrate the existence of extremely thin laminae of scattering particles in the stratosphere. The data allow determination of the optical depth caused by large particles in the atmosphere. At 25 km the optical depth for the non-molecular component is approximately 2×10^{−4}.

The variation of particle concentration with height above 20 km is interpreted on the assumption that two mechanisms transport particles–eddy diffusion, which carries particles upwards, and sedimentation, which transports meteoric debris downwards. The eddy diffusion coefficient in the altitude range 20 to 25 km is found to he approximately 5000 cm^{2} sec^{−1}. The observations also allow the influx of meteoric particles to be determined. The meteoric influxes inferred in this manner are compared with those determined from rocket and satellite experiments, estimates of meteoric dust settling in the air or deposited on the ground, and from the analysis of the zodiacal light. This comparison leads to the conclusions that: 1) a geocentric condensation of the interplanetary dust of approximately a factor of 10^{3} exists in the neighborhood of the earth; 2) this geocentric concentration is most effective for particles in the size range 0.3 μ to 10 μ; 3) a majority of the particles in the earth's dust cloud are in geocentric, quasi-closed orbits. It is also demonstrated that meteoric dust represents a negligible fraction of the particulate matter below 20 km in the earth's atmosphere.

## Abstract

We combine calculated effects of short- and long-period orbital perturbations with modeled effects of recorded sunspot and facular activity to examine patterns of terrestrial insulation at selected latitudes in the Northern Hemisphere for the period 1874–1981. Here we consider systematic insulation effects at times of equinox and solstice and as annual means over the 108-year period. Solar activity is the more dominant term; it modulates global insulation at the period of the solar activity cycle with a maximum depletion, in years of maximum sunspot area, of about 0.1%. At high latitudes, where their effect is greatest, long-period orbital perturbations have driven annual mean insulation downward at a rate of about 0.05%/century. At middle and low latitudes this orbitally-induced, Milankovitch trend in annual mean insulation is positive and about 100 times smaller. Nutation of Earth's rotational axis induced by the gravitational pull of the moon adds a distinct modulation of 18.6-year period that significantly influences insolation at polar latitudes. Orbital perturbations by Jupiter and the inner planets add weaker modulation at shorter periods. The influence of orbital effects is to product secular trends in combined insulation patterns that vary in amplitude, phase, and sign with latitude and time of year.

## Abstract

We combine calculated effects of short- and long-period orbital perturbations with modeled effects of recorded sunspot and facular activity to examine patterns of terrestrial insulation at selected latitudes in the Northern Hemisphere for the period 1874–1981. Here we consider systematic insulation effects at times of equinox and solstice and as annual means over the 108-year period. Solar activity is the more dominant term; it modulates global insulation at the period of the solar activity cycle with a maximum depletion, in years of maximum sunspot area, of about 0.1%. At high latitudes, where their effect is greatest, long-period orbital perturbations have driven annual mean insulation downward at a rate of about 0.05%/century. At middle and low latitudes this orbitally-induced, Milankovitch trend in annual mean insulation is positive and about 100 times smaller. Nutation of Earth's rotational axis induced by the gravitational pull of the moon adds a distinct modulation of 18.6-year period that significantly influences insolation at polar latitudes. Orbital perturbations by Jupiter and the inner planets add weaker modulation at shorter periods. The influence of orbital effects is to product secular trends in combined insulation patterns that vary in amplitude, phase, and sign with latitude and time of year.