Modelling the IRAS Zodiacal Emission

Details Modelling the IRAS Zodiacal Emission Modelling the IRAS Zodiacal Emission

Sep 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990mnras.246..273r&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Vol. 246, NO.2/SEP15, P. 273, 1990

Astronomy and Astrophysics

Astronomy

33

Scientific paper

Using Version 3 of the IRAS Zodiacal History File, we investigate the spatial distribution of zodiacal dust at distances greater than 0.9 AU from the Sun. After investigating several hundred models for the density distribution of the interplanetary dust, the best fit to the data at |β|>15° was found to be a simple fan model with α=4.9. The inclination of the symmetry plane of the dust to the ecliptic plane was found to be i = 1.1°, and the longitude of its ascending node was Ω=79°. An isotropic 100 μm component was included in the model, but its magnitude, 2.2 MJy sr-1, is not considered to be statistically significant in the light of the ±1.6 MJy sr-1 uncertainty in the absolute IRAS calibration at 100 μm.

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