Origin of a Partially Differentiated Titan

Astronomy and Astrophysics – Astronomy

Scientific paper

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Scientific paper

Accretional temperature profiles for Titan are used to determine the conditions needed to avoid global melting as a function of the timing, duration, and nebular conditions of its formation. Titan can accrete undifferentiated in a gas-starved disk (Canup & Ward 2002, 2006, 2009) even with modest quantities of ammonia mixed in with its ices (Barr et al., 2010). The timetable required for formation of an undifferentiated Callisto (Barr & Canup 2008) is consistent with limited melting in Titan during formation.
Simulations of impact-induced core formation (Barr & Canup 2010) are used to show that Titan can remain in a partially differentiated state after an outer solar system late heavy bombardment (LHB), capable of melting its outer layers, permitting some of its rock to consolidate into a core. Thus, we describe a scenario for the formation and early evolution of Titan consistent with its relatively high moment of inertia (Iess et al., 2010). We will also discuss implications of the post-LHB heterogeneous density structure within Titan for interpretation of the moment of inertia coefficient.

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