globalchange  > 气候减缓与适应
DOI: 10.1002/2017JE005341
Scopus记录号: 2-s2.0-85041081136
论文题名:
Geophysical Investigations of Habitability in Ice-Covered Ocean Worlds
作者: Vance S.D.; Panning M.P.; Stähler S.; Cammarano F.; Bills B.G.; Tobie G.; Kamata S.; Kedar S.; Sotin C.; Pike W.T.; Lorenz R.; Huang H.-H.; Jackson J.M.; Banerdt B.
刊名: Journal of Geophysical Research: Planets
ISSN: 21699097
出版年: 2018
卷: 123, 期:1
起始页码: 180
结束页码: 205
语种: 英语
英文关键词: anelasticity ; electrical conductivity ; habitability ; icy ocean worlds ; interior structure ; seismology
Scopus关键词: electrical conductivity ; geophysical method ; ice cover ; seismology ; water-rock interaction
英文摘要: Geophysical measurements can reveal the structures and thermal states of icy ocean worlds. The interior density, temperature, sound speed, and electrical conductivity thus characterize their habitability. We explore the variability and correlation of these parameters using 1-D internal structure models. We invoke thermodynamic consistency using available thermodynamics of aqueous MgSO4, NaCl (as seawater), and NH3; pure water ice phases I, II, III, V, and VI; silicates; and any metallic core that may be present. Model results suggest, for Europa, that combinations of geophysical parameters might be used to distinguish an oxidized ocean dominated by MgSO4 from a more reduced ocean dominated by NaCl. In contrast with Jupiter's icy ocean moons, Titan and Enceladus have low-density rocky interiors, with minimal or no metallic core. The low-density rocky core of Enceladus may comprise hydrated minerals or anhydrous minerals with high porosity. Cassini gravity data for Titan indicate a high tidal potential Love number (k2>0.6), which requires a dense internal ocean (ρocean>1,200 kg m−3) and icy lithosphere thinner than 100 km. In that case, Titan may have little or no high-pressure ice, or a surprisingly deep water-rock interface more than 500 km below the surface, covered only by ice VI. Ganymede's water-rock interface is the deepest among known ocean worlds, at around 800 km. Its ocean may contain multiple phases of high-pressure ice, which will become buoyant if the ocean is sufficiently salty. Callisto's interior structure may be intermediate to those of Titan and Europa, with a water-rock interface 250 km below the surface covered by ice V but not ice VI. ©2017. American Geophysical Union. All Rights Reserved.
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资源类型: 期刊论文
标识符: http://119.78.100.158/handle/2HF3EXSE/114767
Appears in Collections:气候减缓与适应

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作者单位: Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, United States; Institute of Geophysics, ETH Zürich, Zürich, Switzerland; Leibniz-Institute for Baltic Sea Research (IOW), Rostock, Germany; Laboratoire de Planétologie et Géodynamique, Dipartimento di Scienze Geologiche, Universita Roma Tre, Rome, Italy; Université de Nantes, Nantes, France; CNRS, Nantes, France; Creative Research Institution, Hokkaido University, Sapporo, Japan; Department of Electrical and Electronic Engineering, Imperial College, London, United Kingdom; Johns Hopkins University Applied Physics Laboratory, Laurel, MD, United States; Seismological Laboratory, California Institute of Technology, Pasadena, CA, United States; Institute of Earth Sciences, Academia Sinica, Taipei, Taiwan

Recommended Citation:
Vance S.D.,Panning M.P.,Stähler S.,et al. Geophysical Investigations of Habitability in Ice-Covered Ocean Worlds[J]. Journal of Geophysical Research: Planets,2018-01-01,123(1)
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