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

By M. Fulchignoni, F. Ferri, F. Angrilli, A. Ball, A. Bar-Nun, M. Barucci, C. Bettanini, G. Bianchini, William J. Borucki, G. Colombatti and 33 more. Nature, 2005

672 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Molecular Biology

View Paper: https://www.semanticscholar.org/paper/ab0e4c32bfe6708c2b17bb5a52d0f2ae71487d37

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Citations in the corpus

• Titan's methane cycle (2006, methodology): “…the methane saturation curves for: (i) ‘‘central’’ value of the temperatures (T HASI) measured by the Huygens Atmospheric Structure Instrument (HASI, Fulchignoni et al., 2005); (ii) T HASI +11, where the temperatures are systematically increased by 11 everywhere; (iii) T HASI 11, where the…”
• Equilibrium chemistry down to 100 K (2017, background): “At this stage, the build-up of the dust/gas ratio to a value of about 0.004 is mostly completed and there are 11 elements which are strongly reduced by condensation (see lower 5 Titan’s atmosphere has little hydrogen, hence it consists mainly of N2 with just some CH4, whereas oxygen is absent due to”
• Cryovolcanism on Titan: New results from Cassini RADAR and VIMS (2013, background): “…temperature of Titan’s surface is well known from Cassini’s Composite Spectrometer (CIRS) observations [Jennings et al., 2009; Cottini et al., 2012] and the Huygens probe landing site measurements [Fulchignoni et al., 2005]: it is ~93.7 K at the Equator and decreases toward the poles by ~2–3K.”