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We describe a scenario of Titan's formation matching the constraints imposedby its current atmospheric composition. Assuming that the abundances of allelements, including oxygen, are solar in the outer nebula, we show that the icyplanetesimals were agglomerated in the feeding zone of Saturn from a mixture ofclathrates with multiple guest species, so-called stochiometric hydrates suchas ammonia hydrate, and pure condensates. We also use a statisticalthermodynamic approach to constrain the composition of multiple guestclathrates formed in the solar nebula. We then infer that krypton and xenon,that are expected to condense in the 20-30 K temperature range in the solarnebula, are trapped in clathrates at higher temperatures than 50 K. Onceformed, these ices either were accreted by Saturn or remained embedded in itssurrounding subnebula until they found their way into the regular satellitesgrowing around Saturn. In order to explain the carbon monoxide and primordialargon deficiencies of Titan's atmosphere, we suggest that the satellite wasformed from icy planetesimals initially produced in the solar nebula and thatwere partially devolatilized at a temperature not exceeding 50 K during theirmigration within Saturn's subnebula. The observed deficiencies of Titan'satmosphere in krypton and xenon could result from other processes that may haveoccurred both prior or after the completion of Titan. Thus, krypton and xenonmay have been sequestrated in the form of XH3+ complexes in the solar nebulagas phase, causing the formation of noble gas-poor planetesimals ultimatelyaccreted by Titan. Alternatively, krypton and xenon may have also been trappedefficiently in clathrates located on the satellite's surface or in itsatmospheric haze.

Clathration of Volatiles in the Solar Nebula and Implications for the Origin of Titan's atmosphere