Atmospheric Chemistry in Giant Planets, Brown Dwarfs, and Low-Mass Dwarf Stars: I. Carbon, Nitrogen, and Oxygen

By K. Lodders, B. Fegley. 2002

367 citations recorded by the source corpus.

Subfields: Atmospheric Science, Atomic and Molecular Physics, and Optics, Organic Chemistry

View Paper: https://www.semanticscholar.org/paper/aa72e65c6066a8dfd3dd16af49f6bad9cc2f5fc4

How researchers see this paper

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

In Atmospheric Science

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

In Atomic and Molecular Physics, and Optics

1. M. Marley
2. J. D. Kirkpatrick
3. Jon Fortney
4. A. Burgasser
5. K. Lodders
6. R. Freedman
7. D. Saumon
8. A. Showman

In Organic Chemistry

1. M. Marley
2. Jon Fortney
3. R. Freedman
4. D. Saumon
5. A. Showman
6. K. Lodders
7. J. D. Kirkpatrick
8. T. Tsuji

Citations in the corpus

• Temperature–pressure profile of the hot Jupiter HD 189733b from HST sodium observations: detection of upper atmospheric heating (2012, neutral): “The solar abundance ratio of sodium to water is ξNa/ξH2O[solar] = 6.63−9.95×10−3 or ln(ξNa/ξH2O[solar]) = −5.0 to −4.6 (Lodders 2003; Lodders & Fegley 2002; Sharp & Burrows 2007).”
• On the Cool Side: Modeling the Atmospheres of Brown Dwarfs and Giant Planets (2014, methodology): “Examples of equilibrium gas abundances, or ratios of gas abundances, for several key species of interest (from the rainout models of Lodders & Fegley 2002; Visscher et al. 2006) are shown in Figure 3, along with model temperature profiles for a few representative objects.”
• Comparative Planetary Atmospheres: Models of TrES-1 and HD 209458b (2005, methodology): “We use the elemental abundance data of Lodders (2003) and compute chemical equilibrium compositions following Fegley & Lodders (1994) and Lodders & Fegley (2002).”
• Titanium and Vanadium Chemistry in Low-Mass Dwarf Stars (2002, methodology): “Chemical equilibrium computations were done using the CONDOR code, which is described in detail elsewhere (e.g., Fegley & Lodders 1994; Lodders & Fegley 2002).”
• On the Luminosity of Young Jupiters (2006, methodology): “We use the elemental abundance data of Lodders (2003) and compute chemical equilibrium compositions following Fegley & Lodders (1994), Lodders & Fegley (2002), and Lodders (2002).”
• HST PanCET Program: A Cloudy Atmosphere for the Promising JWST Target WASP-101b (2017, background): “These models account for condensation and thermal ionization, though do not include photochemistry (Lodders 1999; Lodders & Fegley 2002; Lodders 2002; Visscher A Cloudy Atmosphere for WASP-101b 5 WASP-101b WASP-31b WASP-17b WASP-101b WASP-31b WASP-17b WASP-101b WASP-31b WASP-17b Al2O3 Fe MgSiO3 Cr…”
• The Evolution of L and T Dwarfs in Color-Magnitude Diagrams (2008, methodology): “Our chemical equilibrium grid of molecular, atomic, and ionic abundances as a function of temperature, pressure, and metallicity is based on the work of Fegley & Lodders (1994,1996), Lodders (1999, 2002), and Lodders & Fegley (2002, 2006).”
• A Spitzer Infrared Spectrograph Spectral Sequence of M, L, and T Dwarfs (2004, background): “The changes in the spectral morphology across the MLT sequence illustrate all of the major chemical transitions expected to occur in the atmospheres of ultracool dwarfs (Fegley & Lodders 1996; Lodders 1999; Burrows & Sharp 1999; Lodders & Fegley 2002).”
• Spitzer IRAC Photometry of M, L, and T Dwarfs (2006, positive): “More recently, the models have begun to take into account nonequilibrium chemistry (e.g., Noll et al. 1997; Saumon et al. 2000, 2003, 2006; Burrows et al. 2000; Ackerman & Marley 2001; Allard et al. 2001; Lodders & Fegley 2002; Marley et al. 2002; Tsuji 2002).”
• NEGLECTED CLOUDS IN T AND Y DWARF ATMOSPHERES (2012, methodology): “The abundances of molecular, atomic, and ionic species are calculated using thermochemical equilibrium following the models of Fegley & Lodders (1994, 1996); Lodders (1999); Lodders & Fegley (2002); Lodders (2002, 2003); Lodders & Fegley (2006); Lodders (2009).”
• New spectral types L and T (2005, methodology): “For more information on this topic, the reader is referred to the detailed papers by Lodders (2002) and Lodders & Fegley (2002) and the review by Burrows et al. (2001).”
• TRANSITIONS IN THE CLOUD COMPOSITION OF HOT JUPITERS (2016, methodology): “We use the opacities described in Freedman et al. (2008), including more recent updates (Freedman et al. 2014), and the molecular abundances described by Lodders & Fegley (2002) and Visscher et al. (2006).”
• Atmosphere, Interior, and Evolution of the Metal-rich Transiting Planet HD 149026b (2005, methodology): “The specifics of CO and CH4 abundances are discussed in detail in Lodders & Fegley (2002).”
• Atomic and Molecular Opacities for Brown Dwarf and Giant Planet Atmospheres (2006, background): “Extensive updates to these thermodynamic databases have been made by Lodders & Fegley (2002).”
• TRANSMISSION SPECTRA OF THREE-DIMENSIONAL HOT JUPITER MODEL ATMOSPHERES (2009, methodology): “The equilibrium chemistry mixing ratios (Lodders & Fegley 2002, 2006; Lodders 2009) are paired with the opacity database (Freedman et al. 2008) to generate pressure-, temperature-, and wavelength-dependent absorption cross-sections that are used for that particular column.”
• CLOUDS AND CHEMISTRY IN THE ATMOSPHERE OF EXTRASOLAR PLANET HR8799b (2011, background): “The reaction time scales (in seconds) for N2 → NH3 and CO → CH4 are from Lodders & Fegley (2002) and Yung et al. (1988), respectively: τN2 = 1 κN2N(H2) (1) κN2 = 8.45× 10 −8exp ( −81515 T ) (2) τCO = N(CO) κ7N(H)N(H2CO) (3) where T is the gas temperature in Kelvin, κ are the rate coefficients in…”
• VULCAN: An Open-source, Validated Chemical Kinetics Python Code for Exoplanetary Atmospheres (2016, background): “…of work on the atmospheric chemistry of exoplanets, and the published models fall into two basic groups: chemical equilibrium (Burrows & Sharp 1999; Lodders & Fegley 2002; Madhusudhan 2012; Blecic et al. 2016) and photochemical kinetics (Kopparapu, Kasting & Zahnle 2012; Line et al. 2011; Visscher…”
• THE DEUTERIUM-BURNING MASS LIMIT FOR BROWN DWARFS AND GIANT PLANETS (2010, background): “…al. 2001, 2003; Baraffe et al. 2002, 2003; Allard et al. 2003; Chabrier et al. 2000b,a; Chabrier & Baraffe 2000; Sharp & Burrows 2007; Barman 2008) and sophisticated chemical models (Fegley & Lodders 1994; Lodders & Fegley 2002; Burrows & Sharp 1999; Sharp & Burrows 2007; Allard & Hauschildt 1995).”
• A Possible Bifurcation in Atmospheres of Strongly Irradiated Stars and Planets (2003, background): “However, thermochemical equilibrium calculations with rainout (Burrows & Sharp 1999; Lodders & Fegley 2002) suggest that TiO and VO would exist at such high-T/low-P points.”