gchange  > 气候减缓与适应
DOI: 10.1002/2017JE005416
Scopus ID: 2-s2.0-85044855475
Title:
Electrical Properties of Tholins and Derived Constraints on the Huygens Landing Site Composition at the Surface of Titan
Author: Lethuillier A.; LeGall A.; Hamelin M.; Caujolle-Bert S.; Schreiber F.; Carrasco N.; Cernogora G.; Szopa C.; Brouet Y.; Simões F.; Correia J.J.; Ruffié G.
Source Publication: Journal of Geophysical Research: Planets
ISSN: 21699097
Indexed By: SCI ; SCI-E
Publishing Year: 2018
Volume: 123, Issue:4
pages begin: 807
pages end: 822
Language: 英语
Keyword: Cassini-Huygens ; permittivity ; tholins ; Titan
Scopus Keyword: aerosol ; electrical property ; permittivity ; Saturn ; Titan
English Abstract: In 2005, the complex permittivity of the surface of Saturn's moon Titan was measured by the PWA-MIP/HASI (Permittivity Wave Altimetry-Mutual Impedance Probe/Huygens Atmospheric Structure Instrument) experiment on board the Huygens probe. The analysis of these measurements was recently refined but could not be interpreted in terms of composition due to the lack of knowledge on the low-frequency/low-temperature electrical properties of Titan's organic material, a likely key ingredient of the surface composition. In order to fill that gap, we developed a dedicated measurement bench and investigated the complex permittivity of analogs of Titan's organic aerosols called “tholins.” These laboratory measurements, together with those performed in the microwave domain, are then used to derive constraints on the composition of Titan's first meter below the surface based on both the PWA-MIP/HASI and the Cassini Radar observations. Assuming a ternary mixture of water ice, tholin-like dust and pores (filled or not with liquid methane), we find that at least 10% of water ice and 15% of porosity are required to explain observations. On the other hand, there should be at most 50–60% of organic dust. PWA-MIP/HASI measurements also suggest the presence of a thin conductive superficial layer at the Huygens landing site. Using accurate numerical simulations, we put constraints on the electrical conductivity of this layer as a function of its thickness (e.g., in the range 7–40 nS/m for a 7-mm thick layer). Potential candidates for the composition of this layer are discussed. ©2018. American Geophysical Union. All Rights Reserved.
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Document Type: 期刊论文
Identifier: http://119.78.100.177/globalchange/handle/2HF3EXSE/114178
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Affiliation: LATMOS/IPSL, UVSQ Universités Paris-Saclay, Paris, France; LATMOS/IPSL, UPMC Université Paris 06 Sorbonne Universités, Paris, France; Physics Institute, University of Bern, Bern, Switzerland; Active Space Technologies, Parque Industrial de Taviero, Coimbra, Portugal; IPAG-CNRS, Université Grenoble Alpes, Grenoble, France; IMS Laboratory, Bordeaux University, Pessac, France

Recommended Citation:
Lethuillier A.,LeGall A.,Hamelin M.,et al. Electrical Properties of Tholins and Derived Constraints on the Huygens Landing Site Composition at the Surface of Titan[J]. Journal of Geophysical Research: Planets,2018-01-01,123(4)
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