The Exploration of Titan and the Saturnian SystemA. Coustenis
LESIA, Observatoire de Paris-Meudon, 92195 Meudon, France,
athena.coustenis@ obspm.fr

The exploration of the outer solar system and in particular of the giant planetsand their environments is an on-going process with the Cassini spacecraft currently
around Saturn, the Juno mission to Jupiter preparing to depart and two large future
space missions planned to launch in the 2020-2025 time frame for the Jupiter system
and its satellites (Europa and Ganymede) on the one hand, and the Saturnian system
and Titan on the other hand [1,2]. Titan, Saturn’s largest satellite, is the only otherobject in our Solar system to possess an extensive nitrogen atmosphere, host to an
active organic chemistry, based on the interaction of N2 with methane (CH4).
Following the Voyager flyby in 1980, Titan has been intensely studied from theground-based large telescopes (such as the Keck or the VLT) and by artificial
satellites (such as the Infrared Space Observatory and the Hubble Space Telescope)for the past three decades. Prior to Cassini-Huygens, Titan’s atmosphericcomposition was thus known to us from the Voyager missions and also through theexplorations by the ISO. Our perception of Titan had thus greatly been enhanced
accordingly, but many questions remained as to the nature of the haze surrounding
the satellite and the composition of the surface. The recent revelations by theCassini-Huygens mission have managed to surprise us with many discoveries [3-8]and have yet to reveal more of the interesting aspects of the satellite.
The Cassini-Huygens mission to the Saturnian system has been an extraordinary
success for the planetary community since the Saturn-Orbit-Insertion (SOI) in July
2004 and again the very successful probe descent and landing of Huygens onJanuary 14, 2005. One of its main targets was Titan. Titan was revealed to be acomplex world more like the Earth than any other: it has a dense mostly nitrogen
atmosphere and active climate and meteorological cycles where the working fluid,
methane, behaves under Titan conditions the way that water does on Earth. Itsgeology, from lakes and seas to broad river valleys and mountains, while carved inice is, in its balance of processes, again most like Earth. Beneath this panoply of
Earth-like processes an ice crust floats atop what appears to be a liquid water ocean.
Titan is also rich in organic molecules—more so in its surface and atmosphere thananyplace in the solar system, including Earth [4]. These molecules were formed in
the atmosphere, deposited on the surface and, in coming into contact with liquidwater may undergo an aqueous chemistry that could replicate aspects of life’sorigins.

I will discuss our current understanding of Titan's complex environment in viewof recent exploration, in particular on the atmospheric structure (temperature andcomposition), and the surface nature. I will show how these and other elements cangive us clues as to the origin and evolution of the satellite, and how they connect tothe observations of the planet and the other satellites and rings.
Future space missions to Titan can help us understand the kronian and also ourSolar System as a whole. In particular, I will describe the future exploration of Titan
and the Saturnian System with TSSM, a mission studied jointly by ESA and NASAin 2008 [1] and prioritized second for a launch around 2023-2025. TSSM comprises
a Titan Orbiter provided by NASA that would carry two Titan in situ elements
provided by ESA: a montgolfière and a lake-landing lander. The mission would
arrive 9 years later for a 4-year duration in the Saturn system. Following delivery of
the ESA in situ elements to Titan, the Titan Orbiter would explore the Saturn system
via a 2-year tour that includes Enceladus and Titan flybys. The montgolfière would
last at least 6 months at Titan and the lake lander 8-10 hours. Following the Saturnsystem tour, the Titan Orbiter would culminate in a ~2-year orbit around Titan.
References[1] TSSM and EJSM NASA/ESA Joint Summary Report, 16 January 2009[2] Coustenis et al. (2008). TandEM: Titan and Enceladus mission. Experimental
Astronomy, 23, 893-946.
[3] Coustenis, A., Hirtzig, M., 2009. Cassini-Huygens results on Titan’s surface.
Research in Astronomy and Astrophysics 9, 249-268.
[4] Coustenis et al., 2010, Titan trace gaseous composition from CIRS at the endof the Cassini-Huygens prime mission Icarus, in press.
[5] Flasar, F. M., et al., 2005. Titan’s atmospheric temperatures, winds, andcomposition. Science, 308, 975-978.
[6] Fulchignoni, M., et al, 2005. In situ measurements of the physicalcharacteristics of Titan’s environment. Nature, 438, 785-791,
doi:10.1038/nature04126.
[7] Lebreton, J-P., Coustenis, A., et al., 2009. Results from the Huygens probe onTitan. Astron. & Astrophys. Rev. 17, 149-179.
[8] Tomasko, M. G., et al., 2005. Rain, winds and haze during the Huygens
probe’sdescent
toTitan’ssurface.
Nature,438,765-778,
doi:10.1038/nature04126.