In situ measurements of the physical characteristics of Titan's environment

M. Fulchignoni, F. Ferri (), F. Angrilli, A. J. Ball, A. Bar-Nun, M. A. Barucci, C. Bettanini, G. Bianchini, W. Borucki, G. Colombatti, M. Coradini, A. Coustenis, S. Debei, P. Falkner, G. Fanti, E. Flamini, V. Gaborit, R. Grard, M. Hamelin, A. M. Harri, B. Hathi, I. Jernej, M. R. Leese, A. Lehto, P. F. Lion Stoppato, J. J. López-Moreno, T. Mäkinen, J. A. M. McDonnell, C. P. McKay, G. Molina-Cuberos, F. M. Neubauer, V. Pirronello, R. Rodrigo, B. Saggin, K. Schwingenschuh, A. Seiff, F. Simões, H. Svedhem, T. Tokano, M. C. Towner, R. Trautner, P. Withers and J. C. Zarnecki
Additional contact information
M. Fulchignoni: LESIA, Observatoire de Paris
F. Ferri: Università di Padova
F. Angrilli: Università di Padova
A. J. Ball: The Open University
A. Bar-Nun: University of Tel Aviv
M. A. Barucci: LESIA, Observatoire de Paris
C. Bettanini: Università di Padova
G. Bianchini: Università di Padova
W. Borucki: MS 244-30, Moffett Field
G. Colombatti: Università di Padova
M. Coradini: Science Directorate
A. Coustenis: LESIA, Observatoire de Paris
S. Debei: Università di Padova
P. Falkner: European Space Agency
G. Fanti: Università di Padova
E. Flamini: Agenzia Spaziale Italiana
V. Gaborit: LESIA, Observatoire de Paris
R. Grard: European Space Agency
M. Hamelin: CETP-IPSL
A. M. Harri: Finnish Meteorological Institute (FMI)
B. Hathi: The Open University
I. Jernej: Austrian Academy of Sciences (IWF)
M. R. Leese: The Open University
A. Lehto: Finnish Meteorological Institute (FMI)
P. F. Lion Stoppato: Università di Padova
J. J. López-Moreno: Instituto de Astrofisica de Andalucia (IAA-CSIC)
T. Mäkinen: Finnish Meteorological Institute (FMI)
J. A. M. McDonnell: The Open University
C. P. McKay: MS 244-30, Moffett Field
G. Molina-Cuberos: University of Murcia
F. M. Neubauer: Universität zu Köln, Albertus-Magnus-Platz
V. Pirronello: Università di Catania
R. Rodrigo: Instituto de Astrofisica de Andalucia (IAA-CSIC)
B. Saggin: Piazza Leonardo da Vinci 32
K. Schwingenschuh: Austrian Academy of Sciences (IWF)
F. Simões: CETP-IPSL
H. Svedhem: European Space Agency
T. Tokano: Universität zu Köln, Albertus-Magnus-Platz
M. C. Towner: The Open University
R. Trautner: European Space Agency
P. Withers: The Open University
J. C. Zarnecki: The Open University

Nature, 2005, vol. 438, issue 7069, 785-791

Abstract: Abstract On the basis of previous ground-based and fly-by information, we knew that Titan's atmosphere was mainly nitrogen, with some methane, but its temperature and pressure profiles were poorly constrained because of uncertainties in the detailed composition. The extent of atmospheric electricity (‘lightning’) was also hitherto unknown. Here we report the temperature and density profiles, as determined by the Huygens Atmospheric Structure Instrument (HASI), from an altitude of 1,400 km down to the surface. In the upper part of the atmosphere, the temperature and density were both higher than expected. There is a lower ionospheric layer between 140 km and 40 km, with electrical conductivity peaking near 60 km. We may also have seen the signature of lightning. At the surface, the temperature was 93.65 ± 0.25 K, and the pressure was 1,467 ± 1 hPa.

Date: 2005
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DOI: 10.1038/nature04314

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