Enrichments in Volatiles in Jupiter: A New Interpretation of the Galileo Measurements

By D. Gautier, F. Hersant, O. Mousis, Jonathan I. Lunine. 2001

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In Astronomy and Astrophysics

Citations in the corpus

Updated Galileo probe mass spectrometer measurements of carbon, oxygen, nitrogen, and sulfur on Jupiter (2004, background): “Another suggestion is that Jupiter began its formation after the solar nebula had cooled down below 40 K at 5 AU (Gautier et al., 2001).”
A Two-dimensional Model for the Primordial Nebula Constrained by D/H Measurements in the Solar System: Implications for the Formation of Giant Planets (2001, background): “Estimating the resulting abundances in the gaseous envelope of Jupiter requires additional modeling, which will be the subject of a forthcoming paper (Gautier et al. 2001).”
Jupiter Formed with More Tar than Ice (2004, methodology): “Gautier et al. (2001) use an initial H2S/H2 ratio of 0.65 times solar within the feeding zone of Jupiter in order to match the observed H2S abundance on Jupiter.”
Synthetic Spectra and Colors of Young Giant Planet Atmospheres: Effects of Initial Conditions and Atmospheric Metallicity (2008, background): “These potentially include planetesimal bomardment and accumulation during formation (Owen et al. 1999; Gautier et al. 2001a,b; Guillot & Gladman 2000; Alibert et al. 2005b), erosion of the heavy element core (Stevenson 1985; Guillot et al. 2004), direct accretion of metal-rich disk gas (Guillot &…”
A new vision of giant planet interiors: Impact of double diffusive convection (2012, background): “…super adiabaticity, they should not strongly depend on our modeling of diffusive/convective trans- 7 Note that the abundances of heavy elements brought to Jupiter and Saturn, in particular water, could already be enriched compared with the solar value (Gautier et al. 2001) port, as mentioned above.”
Sulphur-bearing species in the coma of comet 67P/Churyumov–Gerasimenko (2016, background): “The scenario by Gautier et al. (2001) is an alternate hypothesis which relies on the trapping of volatiles containing the heavy elements in clathrate hydrates in the cooling feeding zone of Jupiter to explain their high abundance.”
EXOPLANET ALBEDO SPECTRA AND COLORS AS A FUNCTION OF PLANET PHASE, SEPARATION, AND METALLICITY (2010, background): “…how giant planets formed and the role of processes such as planetesimal bombardment and accumulation during formation (Owen et al. 1999; Gautier et al. 2001a,b; Guillot & Gladman 2000; Alibert et al. 2005), erosion of the heavy-element core (Stevenson 1985; Guillot et al. 2004), direct…”
Dust flow in gas disks in the presence of embedded planets (2006, background): “This process works against the usual enrichment scenarios for the giant planets (Gautier et al. 2001a,b; Owen et al. 1999).”
A FRAMEWORK FOR CHARACTERIZING THE ATMOSPHERES OF LOW-MASS LOW-DENSITY TRANSITING PLANETS (2013, background): “The exact composition of such planetesimals may depend strongly on the abundances of the planet-forming disk and the location of the planets within the disk (Owen et al. 1999; Gautier et al. 2001; Öberg et al. 2011; Madhusudhan et al. 2011).”
A DETECTION OF WATER IN THE TRANSMISSION SPECTRUM OF THE HOT JUPITER WASP-12b AND IMPLICATIONS FOR ITS ATMOSPHERIC COMPOSITION (2015, background): “…at the formation site, the relative accretion rates of gas and solids, and possible migration pathways (e.g. Atreya et al. 1999; Owen et al. 1999; Gautier et al. 2001; Atreya et al. 2003; Hersant et al. 2004; Lodders 2004; DodsonRobinson et al. 2009; Öberg et al. 2011; Madhusudhan et al.…”