Comparison of the tail region of Venus and Titan

Details Comparison of the tail region of Venus and Titan Comparison of the tail region of Venus and Titan

Dec 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agufm.p34b..05s&link_type=abstract

American Geophysical Union, Fall Meeting 2008, abstract #P34B-05

Physics

2451 Particle Acceleration, 2459 Planetary Ionospheres (5435, 5729, 6026), 2744 Magnetotail, 2748 Magnetotail Boundary Layers

Scientific paper

The Venus Express mission of ESA is exploring the tail formation region of Venus, the Cassini mission flew by Titan along similar orbits that allows to study the tail of Titan. Here we use the data of ASPERA-4 and CAPS charged particles analyzers, the magnetometer data, and the Langmuir probe data of CASSINI, flying onboard of these missions, to compare the tail structure of Venus and Titan. Whereas at Venus the plasma tail exhibits well ordered boundaries below the plasma mantle or its tailward extension (tail boundary, plasma surrounding the current sheet, etc.), at Titan these boundaries are less evident. The common boundary structure is one of the focal issues we study. At Venus the tail is dominated by planetary O+ ions, the ion composition of Titan's tail is more complex. Both at Venus and Titan the origin of the tail might be connected with the nightside ionospheric holes and with a centrifugal acceleration mechanism.

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