Observations in Jupiter's Vicinity with the Magnetospheric Imaging Instrument (MIMI) During Cassini/Huygens Flyby (October 2000-March 2001)

Details Observations in Jupiter's Vicinity with the Magnetospheric Imaging Instrument (MIMI) During Cassini/Huygens Flyby (October 2000-March 2001) Observations in Jupiter's Vicinity with the Magnetospheric Imaging Instrument (MIMI) During Cassini/Huygens Flyby (October 2000-March 2001)

May 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agusm...p51a11k&link_type=abstract

American Geophysical Union, Spring Meeting 2001, abstract #P51A-11 INVITED

Statistics

2756 Planetary Magnetospheres (5443, 5737, 6030)

Scientific paper

The MIMI investigation comprises three sensors, the Ion and Neutral Camera (INCA), Charge-Energy-Mass-Spectrometer (CHEMS), and Low Energy Magnetospheric Measurement System (LEMMS) covering the energy ranges 7 keV/nuc 3 Mev) and protons (1.6 < E < 160 Mev) from the back end of the dual field-of-view telescope. MIMI obtained data intermittently from October 2000 to March 2001 corresponding to distances of ~ 103RJ upstream to ~ 103RJ downstream of the planet. The first unambiguous image of Energetic Neutral Atoms (ENA) was seen at ~ 1155RJ upstream and occupied one pixel in INCA at ~ 3% statistics. The observed intensity in the range ~ 15 to 55 keV (hydrogen) corresponds to ~ 0.08 (cm2 s keV)-1 when scaled to 100 RJ., i.e. similar to expectations based on Voyager 1 observations some 21 years earlier. Many images were obtained through, and past, closest approach (140 RJ; Mitchell et al, this AGU). In addition to ENA's, the CHEMS sensor detected several ion species of Jovian (O+, S+, SO2+, etc) and interstellar (He+) origin in the upstream medium that manifested themselves as pick-up and accelerated components, suggesting that cis-Jovian space is dominated by a nebula populated by volcanic gases from Io (Hamilton, et al, this AGU). Energetic electrons and ion events (LEMMS) were also present upstream and marked each crossing of the extended bow shock and magnetopause of the planet. While in the magnetosphere, field-aligned electron distributions provided unambiguous evidence of closed field lines to at least 200 RJ downstream from Jupiter. Simultaneously, highly charged (S3+, S4+, O3+, O2+, etc) ions were seen, suggesting that plasma outflow in the dusk magnetotail is dominated by magnetospheric rather than solar wind plasma. Evidence that Jovian plasmas are present to at least ~ 850RJ downstream will be presented and implications discussed on overall outflow of magnetospheric plasma.

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