Jupiter's Ring Plane Crossing of 2002-2003

Details Jupiter's Ring Plane Crossing of 2002-2003 Jupiter's Ring Plane Crossing of 2002-2003

Jul 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002hst..prop.9426s&link_type=abstract

HST Proposal ID #9426

Computer Science

Hst Proposal Id #9426

Scientific paper

Jupiter's ring system consists of three components: the main band, the vertically-extended inner halo and the exterior gossamer rings. Each component illustrates aspects of dust dynamics within Jupiter's inclined magnetic field and its strong plasma environment. We will image all three components with ACS during an unusual, extended period of edge-on viewing, December 2002 through February 2003. For faint planetary rings, this geometry improves the signal-to-noise ratio considerably and permits an unambiguous decoupling of radial and vertical structure. Although the Jovian rings have been examined by four spacecraft and from the ground, we are still lacking in a systematic set of data that can distinguish between the ring's prominent dust population and its embedded macroscopic source bodies. We also do not know the size distribution of dust with sufficient accuracy to test rival theories of ring origin. Observations of the system at a range of wavelengths and phase angles with ACS will finally make this determination possible. Coordinated observations at the W. M. Keck Telescope will extend our wavelength coverage well into the IR.

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