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Titan from Cassini-Huygens pp 393–453Cite as

Energy Deposition Processes in Titan's Upper Atmosphere and Its Induced Magnetosphere

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Abstract

Most of Titan's atmospheric organic and nitrogen chemistry, aerosol formation, and atmospheric loss are driven from external energy sources such as Solar UV, Saturn's magnetosphere, solar wind and galactic cosmic rays. The Solar UV tends to dominate the energy input at lower altitudes~1,200 km but which can extend down to ~400 km, while the plasma interaction from Saturn's magnetosphere, Saturn's magnetosheath or solar wind are more important at higher altitudes ~1,400 km, but the heavy ion plasma (O+) ~5 keV and energetic ions (H+) ~ 30 keV or higher from Saturn's magnetosphere can penetrate below 950 km. Cosmic rays with energies >1 GeV can penetrate much deeper into Titan's atmosphere with most of its energy deposited ~70 km altitude. Haze layers are observed in scattered solar photons starting at 510 km, but aerosols are broadly distributed and measured in extinction from 1,000 km downward, diffusively separated to 400 km. The induced magnetic field from Titan's interaction with the external plasma can be very complex and will tend to channel the flow of energy into Titan's upper atmosphere. Cassini observations combined with advanced hybrid simulations of the plasma interaction with Titan's upper atmosphere show significant changes in the character of the interaction with Saturn local time at Titan's orbit where the magnetosphere displays large and systematic changes with local time. The external solar wind can also drive sub-storms within the magnetosphere which can then modify the magnetospheric interaction with Titan. Another important parameter is solar zenith angle (SZA) with respect to the co-rotation direction of the magnetospheric flow which is referred to as the solar incidence-ram angle. Titan's interaction can contribute to atmospheric loss via pickup ion loss, scavenging of Titan's ionospheric plasma, loss of ionospheric plasma down its induced magnetotail via an ionospheric wind, and non-thermal loss of the atmosphere via heating and sputtering induced by the bombardment of magnetospheric keV ions and electrons. This energy input evidently drives the large positive and negative ions observed below ~1,100 km altitude with ion masses exceeding 10,000 Da. We refer to these ions as seed particles for the aerosols observed below 1,000 km altitude. These seed particles can be formed, for example, from the polymerization of acetylene (C2H2) and benzene (C6H6) molecules in Titan's upper atmosphere to form polycyclic aromatic hydrocarbons (PAH) and/or fullerenes (C60). In the case of fullerenes, which are hollow spherical carbon shells, magnetospheric keV O+ ions can become trapped inside the fullerenes and eventually find themselves inside the aerosols as free oxygen. The aerosols are then expected to fall to Titan's surface as polymerized hydrocarbons with trapped free oxygen where unknown surface chemistry can take place.

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Acknowledgments

We acknowledge assistance by Joseph Ajello with regard to the section on UVIS observations at Titan. Robert Kilgore from TRAX International Corporation at Goddard Space Flight Center performed all the graphic arts suppert for the chapter's figures. Work at GSFC is supported by the Cassini Program under JPL Contract 1243218 with SwRI. Additional support at GSFC is provided by NASA's Cassini Data Analysis Program (CDAP).

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Authors and Affiliations

  1. NASA/Goddard Space Flight Center, Greenbelt, MD, USA

    Edward C. Sittler & R. E. Hartle

  2. Institute for Astronomy and Space Physics — IAFE Ciudad Universitaria Buenos Aires, Argentina

    Cesar Bertucci

  3. Mullard Space Science Laboratory, University College London, UK

    Andrew Coates

  4. University of Kansas, Kansas, USA

    Thomas Cravens

  5. Centre National de la Recherche Scientifique (CNRS) at the Centre d'Etude Spatiale des Rayonnements (CESR) Laboratory, Toulouse, France

    Iannis Dandouras

  6. University of Southern California, Department of Aerospace and Mechanical Engineering, Los Angeles, California, USA

    Don Shemansky

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  1. University of Arizona, 1629 E. University Blvd., Tucson, AZ, 85721, USA

    Robert H. Brown

  2. ESA Space Science, Astrophysics Division, ESTEC, Noordwijk, AG, 2200, Netherlands

    Jean-Pierre Lebreton

  3. Space Research Division, Southwest Research Institute (SWRI), 6220 Clebra Road, 28510, San Antonio, TX, 78228, USA

    J. Hunter Waite

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Sittler, E.C. et al. (2009). Energy Deposition Processes in Titan's Upper Atmosphere and Its Induced Magnetosphere. In: Brown, R.H., Lebreton, JP., Waite, J.H. (eds) Titan from Cassini-Huygens. Springer, Dordrecht. https://doi.org/10.1007/978-1-4020-9215-2_16

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