Introduction

The Solar System dust bands are features of the zodiacal cloud emission which have been unambiguously related to the comminution of main-belt asteroids [1], As such, they offer an important insight into the replenishment of the zodiacal cloud, and an opportunity to cast light upon a fundamental question which has yet to be answered satisfactorily: is the zodiacal cloud predominantly asteroidal or cometary?

The approach of the Solar System Dynamics group at the University of Florida towards zodiacal cloud modeling [2] differs in a fundamental way to methods found elsewhere in the literature. This is perhaps due in most part to motivation: many authors are interested in zodiacal emission only as a source of noise, which needs to be modeled only to be subtracted from a given dataset to facilitate other investiagtions. To achieve this, empirical formulations of the various components of the foreground zodiacal emission are produced from observations [3]. This is in contrast to our physically motivated approach, which follows the orbital evolution of a set of dust particles numerically from source to sink, allowing us to place constraints on the origin of the various emission signatures.

Our previous attempts to model the dust bands have been based on the dynamical history of 10 micron astronomical silicate particles [4]. This is because the numerical approach is extremely numerically intensive, and until recently the dynamics of larger parti-

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