Other
Scientific paper
Sep 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006dps....38.7206s&link_type=abstract
American Astronomical Society, DPS meeting #38, #72.06; Bulletin of the American Astronomical Society, Vol. 38, p.629
Other
Scientific paper
The existence of atomic hydrogen in the Saturnian system has been known for over three decades. Despite extensive observations and modeling over this period of time, the spatial morphology and kinetic nature of the circumplanetary hydrogen are still not well understood. The reasons for this lack of understanding are that the basic physical nature of the sources of hydrogen is poorly characterized and that the only detailed spatial measurements of hydrogen are from remote Lyman-α emissions acquired by the Voyager mission, with recent Cassini mission measurements not yet available. The Voyager 1 and 2 UVS observations of Shemansky and Hall (JGR 97, 4143-4161, 1992) have therefore been modeled by combining the numerically efficient approach of Smyth and Marconi (Icarus 101, 18-32, 1993) for the calculation of orbits with the Saturnian plasma model of Richardson (GRL 22, 1177-1180, 1995). Although the model-data comparison is limited by the quality of the Voyager data, H source rates for a Titan source of 3.3 - 4.8 x 1027 atoms s-1 and, for the first time, H source rates larger by about a factor of four for an overall interior icy-satellite source of 1.4 - 1.9 x 1028 atoms s-1 are obtained. These source rates for Titanogenic hydrogen are consistent with previous estimates. These rates for the overall interior icy-satellite source are consistent with recent estimates of those for other water-group species based on observational considerations but are substantially higher than source strengths based on estimated sputtering rates. The larger interior icy-satellite source rate is now recognized from Cassini mission data as likely supplied by the newly discovered gas jet escaping from the south pole of Enceladus. In addition to the H source rates, some broad constraints on the energy and spatial distribution of hydrogen in the Saturnian system will also be presented.
Marconi Max L.
Smyth William H.
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