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Interior of Titan

Stevenson, David J. (1992) Interior of Titan. In: Symposium on Titan. ESA Special Publications. No.338. European Space Agency , Paris, France, pp. 29-33. ISBN 9789290921943. https://resolver.caltech.edu/CaltechAUTHORS:20130726-073136695

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Abstract

There is very little direct information on Titan's interior and even the precisely known mean density allows large uncertainties in volatile content (defined as all components more volatile than H_2O). Volatile-poor models, in which Titan is like Ganymede or Callisto with a thin (observed) volatile veneer, are discussed and discarded. Volatile-rich models are described in which the present Titan consists of a methane clathrate shell overlying a deep water-ammonia ocean and solid ammonia hydrate. The central core of rock (radius ≈ 1900 km) comprises about one half the total mass. The surficial hydrocarbon "ocean" is stored in an "aquifer" (subsurface caverns and pore space) thereby reconciling previous arguments for an ocean with radar and tidal constraints.


Item Type:Book Section
ORCID:
AuthorORCID
Stevenson, David J.0000-0001-9432-7159
Additional Information:© 1992 European Space Agency. This work has been supported by NASA Geology and Geophysics grant NAGW-185. Contribution No. 5109 of the Division of Geological and Planetary Sciences, California Institute of Technology.
Funders:
Funding AgencyGrant Number
NASANAGW-185
Subject Keywords:interior, ocean, evolution, clathrate, ammonia
Other Numbering System:
Other Numbering System NameOther Numbering System ID
Caltech Division of Geological and Planetary Sciences5109
Series Name:ESA Special Publications
Issue or Number:338
Record Number:CaltechAUTHORS:20130726-073136695
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20130726-073136695
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:39602
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:29 Jul 2013 22:10
Last Modified:03 Oct 2019 05:08

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