Properties of interplanetary dust from infrared and optical observations. II. Brightness, polarization, temperature, albedo and their dependence on the elevation above the ecliptic.

Details Properties of interplanetary dust from infrared and optical observations. II. Brightness, polarization, temperature, albedo and their dependence on the elevation above the ecliptic. Properties of interplanetary dust from infrared and optical observations. II. Brightness, polarization, temperature, albedo and their dependence on the elevation above the ecliptic.

Dec 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995a%26a...304..602r&link_type=abstract

Astronomy and Astrophysics, v.304, p.602

Astronomy and Astrophysics

Astrophysics

15

Interplanetary Medium, Polarization, Infrared: Solar System, Comets: General, Minor Planets, Asteroids

Scientific paper

In the first paper, by using the "node of lesser uncertainty" method, Dumont & Levasseur-Regourd (1988) have obtained the heliocentric gradients of the local temperature, the local volume intensity (i.e. local brightness) and the local albedo in the symmetry plane of the zodiacal cloud (close to ecliptic plane). In the present work, by a new treatment applied to the IRAS data, the values of the gradients are derived more precisely. The method is also applied out of the ecliptic, to retrieve the local values of brightness, polarization, temperature and albedo out of the symmetry plane, first towards the ecliptic pole, and then in the so-called tangential plane (i.e. plane tangent to the Earth orbit and perpendicular to the ecliptic). Maps showing the changes of these local values (normalized at a solar distance of 1AU and a phase angle of 90deg) with elevation above the ecliptic up to 0.4AU, are drawn in this plane. The brightness, the polarization and the temperature decrease, while the albedo increases, with increasing elevation. The decrease of the temperature is also established at a solar distance of 1.5AU and up to 1AU above the ecliptic. These results can be interpreted in terms of at least two populations of dust with different average orbital inclinations, originating from periodic comets and asteroidal dust bands, and from new comets.

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