On the volatile inventory of Titan from isotopic abundances in nitrogen and methane.
We analyze recently published nitrogen and hydrogen isotopic data to constrain the initial volatile abundances on Saturn's giant moon Titan. The nitrogen data are interpreted in terms of a model of non-thermal escape processes that lead to enhancement in the heavier isotope. We show that these data do not, in fact, strongly constrain the abundance of nitrogen present in Titan's early atmosphere, and that a wide range of initial atmospheric masses (all larger than the present value) can yield the measured enhancement. The enrichment in deuterated methane is now much better determined than it was when Pinto et al. (1986. Nature 319, 388-390) first proposed a photochemical mechanism to preferentially retain the deuterium. We develop a simple linear theory to provide a more reliable estimate of the relative dissociation rates of normal and deuterated methane. We utilize the improved data and models to compute initial methane reservoirs consistent with the observed enhancement. The result of this analysis agrees with an independent estimate for the initial methane abundance based solely on the present-day rate of photolysis and an assumption of steady state. This consistency in reservoir size is necessary but not sufficient to infer that methane photolysis has proceeded steadily over the age of the solar system to produce large quantities of less volatile organics. Our analysis indicates an epoch of early atmospheric escape of nitrogen, followed by a later addition of methane by outgassing from the interior. The results also suggest that Titan's volatile inventory came in part or largely from a circum-Saturnian disk of material more reducing than the surrounding solar nebula. Many of the ambiguities inherent in the present analysis can be resolved through Cassini-Huygens data and a program of laboratory studies on isotopic and molecular exchange processes. The value of, and interest in, the Cassini-Huygens data can be greatly enhanced if such a program were undertaken prior to the prime phase of the mission.
Lunine
J I
JI
Reparto di Planetologia, CNR-Istituto di Astrofisica Spaziale, Rome, Italy. jlunine@lpl.arizona.edu
Yung
Y L
YL
Lorenz
R D
RD
D001272:Atmosphere / Q000737:chemistry*; D002247:Carbon Isotopes; D003903:Deuterium; D019419:Evolution, Planetary; D005118:Extraterrestrial Environment; D006859:Hydrogen; D008697:Methane / Q000032:analysis* / Q000737:chemistry; D008956:Models, Chemical; D009584:Nitrogen / Q000032:analysis* / Q000737:chemistry; D009587:Nitrogen Isotopes; D010777:Photochemistry; D018539:Saturn
D002247:Carbon Isotopes; D009587:Nitrogen Isotopes; D006859:Hydrogen; D003903:Deuterium; D009584:Nitrogen; D008697:Methane