A Dynamical Model of a Still-Forming Zodiacal Dust Band, as Constrained by IRAS Data

Details A Dynamical Model of a Still-Forming Zodiacal Dust Band, as Constrained by IRAS Data A Dynamical Model of a Still-Forming Zodiacal Dust Band, as Constrained by IRAS Data

May 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009dda....40.1206e&link_type=abstract

American Astronomical Society, DDA meeting #40, #12.06; Bulletin of the American Astronomical Society, Vol. 41, p.906

Astronomy and Astrophysics

Astronomy

Scientific paper

When an asteroid is disrupted, the larger pieces remain on similar orbits and constitute an asteroid family. The smaller products of the disruption (10 microns- a few cm) decay into the inner solar system under the effect of Poynting-Roberston drag. Before these particles encounter the secular and mean-motion resonances at the inner edge of the main belt, they retain their proper orbital elements and share common forced elements, allowing for the existence of the dust band structure discovered by IRAS (Low et al., 1984). There are currently known to be at least three dust band pairs associated with relatively young (≤ 107 yr old) asteroidal disruptions (Grogan et al., 2001; Dermott et al., 2002; Nesvorny et al., 2003; 2008). A method of coadding the IRAS data set, revealed the existence of an additional solar system dust band at 17 degrees inclination, likely a confirmation of the M/N pair originally suggested by Sykes (1988). We see this new dust band at some but not all ecliptic longitudes, providing strong evidence for a very young dust band in the process of formation. In order to determine the parent body of this band, we create a full dynamical model of the formation of this dust band to constrain the parameters of a source body capable of producing the structure. The model is based on the dynamical evolution of the 10-1000 micron diameter dust particles from the disruption event. Comparison of the model to our co-added IRAS observations allows us to put bounds on the parameters of the parent body, including the node location and dispersion, which gives an age to the disruption that produced the partial band. We also investigate the effects that varying the orbital parameters has on the timescale and formation of a band pair.

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