A physical model for the IRAS zodiacal dust bands

We present a model, based on justifiable physical assumptions, of the zodiacal cloud and asteroidal dust bands which gives a good representation of the thermal IR emission from interplanetary dust observed using IRAS. In addition to the narrow asteroidal bands that have been previously reported, we find a broad double-band component with peak intensities at $$\beta \approx \pm9^\circ$$, which shows significant emission at latitudes $$\left|\beta \right| \sim 20^\circ$$. The physical significance of this feature within the Solar system and its relationship to the zodiacal cloud are discussed.