Other
Scientific paper
May 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006sptz.prop30235m&link_type=abstract
Spitzer Proposal ID #30235
Other
Scientific paper
We propose to observe a combined eclipse- and occultation event of the binary asteroid system (617) Patroclus, a member of the intriguing population of Jupiter Trojans. This will be the first thermal-IR observation of such a rare event. Patroclus, the only known Trojan binary, is a particularly well-suited target because its orbital parameters are well known (Marchis et al. 2006) and both components are of roughly equal size, which maximizes the observable effects of the eclipse event. Observing a nearly total eclipse allows the surface thermal inertia, which depends on key physical properties such as the surface porosity, to be determined in a uniquely direct way. Also, occultations allow one component to be studied without significant contamination from the other, thereby facilitating the determination of possible differences between their surface compositions. Note that the angular distance between the components does not exceed 0.15". The proposed Spitzer IRS observations will allow us to clarify the physical nature of the Patroclus system and constrain its mineralogy by providing measurements of the thermal inertia, size and albedo of each component, and the spectral silicate features around 10microns. From spatially resolved Keck imaging Marchis et al. (2006) have recently determined the orbital parameters of the Patroclus system. From these they determined the total mass of the system which, combined with a previous estimate of Patroclus' size, implies a bulk mass density of only 0.8 g cm-3, indicative of a composition dominated by water ice. This supports the idea that large Jupiter Trojans, such as Patroclus, are among the most primordial bodies in the solar system accessible to observations, and that they are basically collisionally unaltered since their formation.
Berthier Jerome
Descamps Pascal
Emery Josh
Harris Alan
Hestroffer Daniel
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