Atmospheric Chemistry in Giant Planets, Brown Dwarfs, and Low-Mass Dwarf Stars. II. Sulfur and Phosphorus

By C. Visscher, K. Lodders, B. Fegley, Jr.. 2005

243 citations recorded by the source corpus.

Thermochemical equilibrium and kinetic calculations are used to model sulfur and phosphorus chemistry in giant planets, brown dwarfs, and extrasolar giant planets (EGPs). The chemical behavior of individual S- and P-bearing gases and condensates is determined as a function of pressure, temperature, and metallicity. The results are independent of particular model atmospheres, and in principle, the equilibrium composition along the pressure-temperature profile of any object can be determined. Hydrogen sulfide (H2S) is the dominant S-bearing gas throughout substellar atmospheres and approximately represents the atmospheric sulfur inventory. Silicon sulfide (SiS) is a potential tracer of weather in substellar atmospheres. Disequilibrium abundances of phosphine (PH3) approximately representative of the total atmospheric phosphorus inventory are expected to be mixed upward into the observable atmospheres of giant planets and T dwarfs. In hotter objects, several P-bearing gases (e.g., P2, PH3, PH 2, PH, and HCP) become increasingly important at high temperatures.

Subfields: Astronomy and Astrophysics, Atmospheric Science

View Paper: https://www.semanticscholar.org/paper/b9dcb767a69f3878cf2dfa9e0bd0e3bcac2480a4

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In Astronomy and Astrophysics

1. Jon Fortney
2. N. Madhusudhan
3. M. Marley
4. A. Showman
5. D. Sing
6. V. Parmentier
7. M. Line
8. D. Deming

In Atmospheric Science

1. M. Marley
2. Jon Fortney
3. R. Freedman
4. A. Showman
5. K. Lodders
6. D. Saumon
7. Adam Burrows
8. V. Parmentier

Citations in the corpus

• A chemical model for the atmosphere of hot Jupiters (2012, background): “Deviations from the thermodynamic equilibrium have been discussed with timescale arguments (e.g. Lodders & Fegley 2002; Fortney et al. 2006, 2008b; Visscher et al. 2006, 2010; Madhusudhan & Seager 2010) or modeled with a few reactions describing the CO-CH4 conversion coupled with the dynamics…”
• Line and Mean Opacities for Ultracool Dwarfs and Extrasolar Planets (2007, unknown): “…detection of H2S at about 3 times the solar S/H2 ratio in Jupiter’s atmosphere below the NH4SH cloud level (Niemann et al. 1998) shows that the cloud layer condensation approach works well in giant planet atmospheres such as in Jupiter (see also Lodders & Fegley 2002; Visscher et al. 2006).”
• QUANTITATIVELY ASSESSING THE ROLE OF CLOUDS IN THE TRANSMISSION SPECTRUM OF GJ 1214b (2013, methodology): “…silicate and iron clouds condense in L dwarfs (e.g. Tsuji et al. 1996; Allard et al. 2001; Marley et al. 2002; Burrows et al. 2006; Cushing et al. 2008; Visscher et al. 2010) and sulfide and chloride clouds condense in T dwarfs (Lodders & Fegley 2006; Visscher et al. 2006; Morley et al. 2012).”
• ATMOSPHERIC CHEMISTRY IN GIANT PLANETS, BROWN DWARFS, AND LOW-MASS DWARF STARS. III. IRON, MAGNESIUM, AND SILICON (2010, methodology): “Below the Fe cloud deck, the FeS abundance is ∼ 10 ppb and decreases at higher temperatures and lower pressures as H2S is replaced by SH and S (Visscher et al. 2006).”
• TRANSMISSION SPECTRA OF THREE-DIMENSIONAL HOT JUPITER MODEL ATMOSPHERES (2009, background): “…are calculated assuming local chemical equilibrium as a function of local temperature and pressure, accounting properly for depletion of gas-phase species via condensation, follow K. Lodders and collaborators (Lodders 1999; Lodders & Fegley 2002; Lodders 2002; Visscher et al. 2006; Lodders 2009).”
• ATMOSPHERIC SULFUR PHOTOCHEMISTRY ON HOT JUPITERS (2009, methodology): “Visscher et al (2006) predicted that HS would be very abundant in equilibrium at hot Jupiter conditions.”
• From thermal dissociation to condensation in the atmospheres of ultra hot Jupiters: WASP-121b in context (2018, methodology): “As in previous thermochemical grid models (see Lodders & Fegley 2002; Visscher et al. 2006, 2010), molecular species thermally dissociate at high temperatures and low pressures via net thermochemical reactions such as H2 2H H2O 2H+O TiO Ti+O VO V+O, 1 We define the azimuth as the projected angle…”
• Global Climate and Atmospheric Composition of the Ultra-hot Jupiter WASP-103b from HST and Spitzer Phase Curve Observations (2018, methodology): “Our fiducial model assumes a solar composition with elemental abundances of Lodders & Fegley (2002) and the chemical equilibrium gas phase composition from Visscher et al. (2006).”
• 3D mixing in hot Jupiters atmospheres. I. Application to the day/night cold trap in HD 209458b (2013, methodology): “We use the opacities developed by Freedman et al. (2008), including more recent updates, and the molecular abundances described by Lodders & Fegley (2002) and Visscher et al. (2006).”
• DISEQUILIBRIUM CARBON, OXYGEN, AND NITROGEN CHEMISTRY IN THE ATMOSPHERES OF HD 189733b AND HD 209458b (2011, background): “…from equilibrium are sometimes explored through evaluations of simple time-scale arguments (e.g., Lodders & Fegley 2002; Fortney et al. 2006a, 2008b; Visscher et al. 2006, 2010a; Madhusudhan & Seager 2011) or through more complex models with parameterized chemical kinetics (Cooper & Showman 2006).”
• Hubble Space Telescope hot Jupiter transmission spectral survey: a detection of Na and strong optical absorption in HAT-P-1b (2013, background): “Chemical mixing ratios and opacities assume solar metallicity and local chemical equilibrium, accounting for condensation and thermal ionisation though no photochemistry (Lodders 1999, 2002; Lodders & Fegley 2002, 2006; Visscher et al. 2006; Freedman et al. 2008; Lodders 2009).”
• NEGLECTED CLOUDS IN T AND Y DWARF ATMOSPHERES (2012, methodology): “Our modeling of sulfide condensation chemistry follows that of Visscher et al. (2006), and the condensation reactions and temperature-dependent expressions presented here are taken from that study.”