HR: 08:45h
AN: P21D-04    [Abstracts]
TI: Endogenic Origin of Titan's N2
AU: * Matson, D J
EM: Dennis.l.Matson@jpl.nasa.gov
AF: Jet Propulsion Laboratory/CalTech, 4800 Oak Grove Drive, Pasadena, CA 91109, United States
AU: Atreya, S J
EM: atreya@umich.edu
AF: Jet Propulsion Laboratory/CalTech, 4800 Oak Grove Drive, Pasadena, CA 91109, United States
AU: Atreya, S J
EM: atreya@umich.edu
AF: Planetary Science Lab, University of Michigan, 2455 Hayward Street, Ann Arbor, MI 48109, United States
AU: Castillo-Rogez, J J
EM: Julie.C.Castillo@jpl.nasa.gov
AF: Jet Propulsion Laboratory/CalTech, 4800 Oak Grove Drive, Pasadena, CA 91109, United States
AU: Johnson, T
EM: Torrence.v.johnson@jpl.nasa.gov
AF: Jet Propulsion Laboratory/CalTech, 4800 Oak Grove Drive, Pasadena, CA 91109, United States
AU: Adams, E
EM: eya@umich.edu
AF: Planetary Science Lab, University of Michigan, 2455 Hayward Street, Ann Arbor, MI 48109, United States
AU: Lunine, J
EM: jlunine@lpl.arizona.edu
AF: Jet Propulsion Laboratory/CalTech, 4800 Oak Grove Drive, Pasadena, CA 91109, United States
AU: Lunine, J
EM: jlunine@lpl.arizona.edu
AF: Lunar Planetary Lab, University of Arizona, 1629 E University Blvd, Tucson, AZ 85721, United States
AU: Lunine, J
EM: jlunine@lpl.arizona.edu
AF: INAF-IFSI, Via del Fosso del Cavaliere 100, Rome, 00133, Italy
AB: The composition of Titan's atmosphere measured by the Huygens probe has been interpreted as indicating that nitrogen was not a primordial ingredient; the abundance of non-radiogenic argon being so small relative to molecular nitrogen that very little of the either could have accreted in Titan. If Titan formed 2.5 to 5.0 My after the calcium-aluminum inclusions (CAIs) were created (as suggested for Iapetus, Castillo-Rogez et al., Icarus 190, 179-202, 2007) then differentiation occurred early and a stable core formed. During differentiation, heat from short-lived radioisotope decay and gravitational energy enabled rapid serpentinization of most of the silicate phase . Water and chemical reactants were trapped by the hydrated silicate that accumulates into the core. After a few hundred My, temperatures become high enough for ammonia decomposition to take place, producing molecular nitrogen and hydrogen. This process can be further aided by the catalytic action of metal and clay minerals. Released molecular hydrogen can engage in reactions involving organic material, C, CO and CO2 to produce primarily methane (Atreya et al., Planet. Space Sci. 54, 1177-1187, 2006). Some of the molecular nitrogen is conjectured to have reached the surface but the details of the process are not known. A high-pressure ice layer is expected to have formed a barrier against the upward transfer of material from the core to the ocean. This barrier would have become more efficient with time as it was thickening, The increasing temperatures in the core eventually induce silicate dehydration. We believe that during this stage volatiles and organics could have been released from the core, and the associated burst of hot upwelling material could have destabilized the high- pressure layer. The presence in the atmosphere of 40Ar (as a result of 40K decay) indicates that gases from the core reach the surface. The isotopic fractionation of nitrogen (14N/15N) in the atmosphere as measured by Huygens indicates that the loss of nitrogen to space may be happening over a long time, although an early, massive escape is a definite possibility. Since it is difficult for Ar to escape from the atmosphere to space, the under-abundance of 40Ar in the atmosphere compared to the amount expected to have accreted suggests that gases are still present in the interior of Titan. Thus, current venting from the interior might include N2, CH4, in addition to Ar. The near-terrestrial 12C/13C vs. non-terrestrial 14N/15N suggests a different evolutionary history for methane than nitrogen on Titan, however, and is being investigated. In a companion paper (Atreya et al., 2007, Fall AGU Meeting) we discuss the formation of Titan's nitrogen atmosphere by the solar UV photolysis of ammonia. This work was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA.
DE: 5220 Hydrothermal systems and weathering on other planets
DE: 6005 Atmospheres (1060)
DE: 6024 Interiors (8147)
DE: 6281 Titan
SC: Planetary Sciences [P]
MN: 2007 Fall Meeting