Titanium and Vanadium Chemistry in Low-Mass Dwarf Stars

By K. Lodders. 2002

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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…”
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).”
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).”
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).”
The Influence of Atmospheric Dynamics on the Infrared Spectra and Light Curves of Hot Jupiters (2006, methodology): “When generating our model spectra, we use the elemental abundance data of Lodders (2003) and chemical equilibrium compositions computed with the CONDOR code, as described in Fegley & Lodders (1994), Lodders & Fegley (2002), and Lodders (2002).”
SpeX SPECTROSCOPY OF UNRESOLVED VERY LOW MASS BINARIES. I. IDENTIFICATION OF 17 CANDIDATE BINARIES STRADDLING THE L DWARF/T DWARF TRANSITION (2009, background): “2200 K (Golimowski et al. 2004), host a variety of mineral condensate species in their photospheres (Lodders 2002), as evident by their very red near-infrared colors, muted H2O absorption bands, weak TiO and VO bands (gaseous precursors to condensates) and presence of silicate grain features (e.g.,…”
From thermal dissociation to condensation in the atmospheres of ultra hot Jupiters: WASP-121b in context (2018, background): “1 and also Lodders (2002)) with decreasing pressure.”
A Unified Theory for the Atmospheres of the Hot and Very Hot Jupiters: Two Classes of Irradiated Atmospheres (2007, methodology): “We use the elemental abundance data of Lodders (2003) and chemical equilibrium compositions are computed with the CONDOR code, following Lodders & Fegley (2002, 2006), and Lodders (1999, 2002).”
The First Substellar Subdwarf? Discovery of a Metal-poor L Dwarf with Halo Kinematics (2003, background): “One possibility is that the mechanism of Ti depletion in these objects—incorporation into multiple-metal condensates of CaTiO3, Ca3Ti2O7, Ca4Ti3O10, and Ti2O3 (Lodders 2002)—may be inhibited in the low-metallicity atmosphere of 2MASS 0532+8246.”
A Spitzer Infrared Spectrograph Spectral Sequence of M, L, and T Dwarfs (2004, background): “In particular, titanium- and vanadium-bearing condensates form resulting in a loss of TiO and VO from the gas (Lodders 2002); the weakening and eventual loss of the TiO and VO bands mark the transition to the L spectral class (1400 .”
Atomic and Molecular Opacities for Brown Dwarf and Giant Planet Atmospheres (2006, background): “Both TiO and VO are influenced by the formation of condensates, which cause them to be very rapidly removed from the gas phase when the condensates form (Lodders 2002).”
An HST optical-to-near-IR transmission spectrum of the hot Jupiter WASP-19b: detection of atmospheric water and likely absence of TiO (2013, background): “Chemical mixing ratios and opacities assume solar metallicity and local chemical equilibrium accounting for condensation and thermal ionization but no photoionization (Lodders 1999, 2002, 2009; Lodders & Fegley 2002; Visscher, Lodders & Fegley 2006; Freedman, Marley & Lodders 2008).”
Discovery of a Very Young Field L Dwarf, 2MASS J01415823–4633574 (2005, background): “(See, for example, Table 2 and Figure 2 of Lodders (2002).)”
Line and Mean Opacities for Ultracool Dwarfs and Extrasolar Planets (2007, methodology): “Note that some frequently used compilations of thermodynamic properties and/or polynomial fits contain errors that also affect compounds important for brown dwarf chemistry (see Appendix 1 in Lodders 2002).”
CAN TiO EXPLAIN THERMAL INVERSIONS IN THE UPPER ATMOSPHERES OF IRRADIATED GIANT PLANETS? (2009, background): “In chemical equilibrium, at low temperatures or high pressures, Ti and V are found in a variety of condensates that form solid grains (Burrows & Sharp 1999; Lodders 2002; Sharp & Burrows 2007).”
Atmospheric Chemistry in Giant Planets, Brown Dwarfs, and Low-Mass Dwarf Stars. II. Sulfur and Phosphorus (2005, background): “These models have also been useful for explaining how the optical and infrared spectra of substellar objects are influenced by CNO (Lodders & Fegley 2002), alkali (Lodders 1999a), Ti and V (Lodders 2002), and condensation (e.g., Lodders & Fegley 2006) chemistry.”
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).”
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).”