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Research in Infrared Aurorae in the Solar System

Explore H3+ formation and destruction, while imaging Jupiter and Saturn in infrared light. Spectroscopy provides insights into atmospheric densities and composition. High-resolution observations uncover unique features.

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Research in Infrared Aurorae in the Solar System

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  1. ATMOSPHERIC PHYSICS LABORATORYDEPARTMENT OF PHYSICS AND ASTROMONY Infrared Aurorae in the Solar System Tom Stallard Steve Miller, Henrik Melin, Makenzie Lystrup and the Cassini community, especially: Emma Bunce, Chris Arridge, Nick Achilleos and Michele Dougherty

  2. Hydrocarbons Hydrocarbons H3+ formation H2 + hn= H2+ + e H2 + e*= H2+ + e + e H2+ + H2 =H3+ + H H3+ destruction H3+ + X = HX+ + H2 H3+ + e- = H + H2

  3. Imaging: Jupiter Ultraviolet (Clarke et al) Infrared (Connerney et al)

  4. Saturn

  5. Uranus

  6. Spectroscopy: Jupiter

  7. Multiple line spectroscopy provides: • emission intensities • temperature • composition • cooling rates • vertical thermal profile • atmospheric densities

  8. IR observations of Jupiter

  9. Temperature

  10. Cooling

  11. Ion Winds

  12. High resolution observations of Saturn

  13. Compared with the UV emission

  14. 1.3” smear

  15. Extended Flanks Infilled

  16. Saturn Jupiter

  17. Saturn Co-rotation breakdown Jupiter

  18. Saturn Co-rotation breakdown Outer effects Jupiter

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