The abundances of constituents of Titan's atmosphere from the GCMS instrument on the Huygens probe

By H. Niemann, S. Atreya, S. Bauer, G. Carignan, J. Demick, R. Frost, D. Gautier, J. Haberman, D. Harpold, D. Hunten and 8 more. Nature, 2005

917 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/1982c5ce8edb1c5f61053c57c25d2cccf46e12e3

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. Jon Fortney
2. N. Madhusudhan
3. T. Robinson
4. J. Cui
5. J. Leconte
6. J. Kasting
7. Francois Forget
8. F. Selsis

Citations in the corpus

• Cryovolcanic features on Titan's surface as revealed by the Cassini Titan Radar Mapper (2007, methodology): “Indeed, evidence from the Huygens landing site for liquid methane and ethane just beneath the visible surface (Niemann et al., 2005) suggests that quenching of the outer boundary of the lava by liquid hydrocarbons might occur even in the absence of a large-scale body of liquid.”
• Analysis of Titan's neutral upper atmosphere from Cassini Ion Neutral Mass Spectrometer measurements in the Closed Source Neutral mode (2009, methodology): “The most recent determination of the carbon isotope ratio on Titan gives y(CH4) = n(CH4)/n(13CH4) = 82.3 ± 0.1, based on the Huygens GCMS measurements made between 6 and 18 km (Niemann et al., 2005).”
• Titan's middle-atmospheric temperatures and dynamics observed by the Cassini Composite Infrared Spectrometer (2008, background): “A stratospheric CH4 mole fraction of 0.0141 is assumed ( Niemann et al., 2005 ), along with a[ CH 3D]/[CH4] ratio of 6.1 × 10−4.”
• Modeling climate diversity, tidal dynamics and the fate of volatiles on TRAPPIST-1 planets (2017, background): “Titan (0.012 S ⊕, 0.4 R⊕) has a 1.5 bars thick N2-dominated atmosphere, with as much as 5 % of methane near the surface (Niemann et al. 2005).”
• Observing the Atmospheres of Known Temperate Earth-sized Planets with JWST (2017, background): “Instead, we choose three very different atmospheric compositions that are by definition possible outcomes of planet formation simply because they exist in our own solar system: those of Earth, Venus, and Titan.”
• Analysis of Cassini/CIRS limb spectra of Titan acquired during the nominal mission I. Hydrocarbons, nitriles and CO2 vertical mixing ratio profiles (2010, background): “As this molecule is supposed to be chemically stable in the stratosphere, which would imply a less steep vertical mixing ratio profile, Vinatier et al. (2007a) have proposed that a sink, not included in the photochemical models, exists in the stratosphere.”
• The composition of Titan's stratosphere from Cassini/CIRS mid-infrared spectra (2007, methodology): “The opposite effect is found when we use the 1.41% CH4 abundance (inferred from Huygens GCMS measurements by Niemann et al., 2005 ) and its associated profiles, instead of 1.6%.”
• Oxygen compounds in Titan's stratosphere as observed by Cassini CIRS (2007, background): “Methane is expected to be uniformly mixed in the stratosphere and Huygens results show that this is indeed the case (Niemann et al., 2005).”