Astronomy and Astrophysics – Astronomy
Scientific paper
Sep 1996
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996dps....28.1602g&link_type=abstract
American Astronomical Society, DPS meeting #28, #16.02; Bulletin of the American Astronomical Society, Vol. 28, p.1120
Astronomy and Astrophysics
Astronomy
Scientific paper
The Solar System dust bands discovered by IRAS are toroidal distributions of dust particles with common proper inclinations. It is impossible for particles with high eccentricity (approximately 0.2 or greater) to maintain a near constant proper inclination as they precess, and therefore the dust bands must be composed of material having a low eccentricity, pointing to an asteroidal origin. The mechanism of dust band production could involve either a continual communution of material associated with the major Hirayama asteroid families (Dermott et al, Nature, 312, 505-509, 1984), the equilibrium model, or random disruptions in the asteroid belt of small, single asteroids (Sykes and Greenberg, Icarus, 65, 51-69, 1986). The IRAS observations of the zodiacal cloud from which we isolate the dust band profiles have excellent resolution, and the manner in which these profiles change around the sky should allow us to determine the origin of the bands, their radial extent, the size-frequency distribution of the material and the optical properites of the dust itself. The equilibrium model of the dust bands suggests Eos as the parent of the 10deg band pair. In this paper we present results from detailed numerical modeling of the 10deg band pair. We demonstrate that a model composed of dust particles having mean semi-major axis, proper eccentricity and proper inclination equal to those of the Eos family member asteroids, but with a dispersion in proper inclination of 2.5deg , produces a convincing match with observations. Indeed, it is impossible to reproduce the observed profiles of the 10deg band pair without imposing such a dispersion on the dust band material. This result is strong evidence in favor of the equilibrium model.
Dermott Stanley F.
Grogan Keith
Jayaraman Sumita
Xu Yu-Liang
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