Jupiter Formed with More Tar than Ice

By K. Lodders. 2004

158 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/afa468519084fe3a3076b614442803056943e202

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In Astronomy and Astrophysics

Citations in the corpus

A PRECISE WATER ABUNDANCE MEASUREMENT FOR THE HOT JUPITER WASP-43b (2014, background): “…of a planet’s water content can therefore help constrain the disk chemistry, location, and surface density of solids where it formed (e.g. Lodders 2004; Mousis et al. 2009; Öberg et al. 2011; Madhusudhan et al. 2011; Mousis E-mail: laura.kreidberg@uchicago.edu 1 Department of Astronomy…”
Atmospheric Chemistry in Giant Planets, Brown Dwarfs, and Low-Mass Dwarf Stars. II. Sulfur and Phosphorus (2005, background): “However, condensation of FeS is preceded by Fe metal condensation and in the high-gravity environment of substellar objects, iron settles into a deep cloud layer at high temperatures (e.g. Prinn & Olaguer 1981; FL94; Lodders 1999a; LF02; Lodders & Fegley 2006).”
A DETECTION OF WATER IN THE TRANSMISSION SPECTRUM OF THE HOT JUPITER WASP-12b AND IMPLICATIONS FOR ITS ATMOSPHERIC COMPOSITION (2015, background): “…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. 2011a, 2014a).”
Synthetic Spectra and Colors of Young Giant Planet Atmospheres: Effects of Initial Conditions and Atmospheric Metallicity (2008, background): “…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 & Hueso 2006), and chemical fractionation within the planet (Stevenson & Salpeter 1977; Lodders 2004).”
A POSSIBLE CARBON-RICH INTERIOR IN SUPER-EARTH 55 Cancri e (2012, background): “However, several recent studies have suggested the possibility of carbon-rich extrasolar planets, both theoretically (Lodders 2004; Kuchner & Seager 2005; Bond et al. 2010; Madhusudhan et al. 2011b; Oberg et al. 2011; Mousis et al. 2012) and observationally (Madhusudhan et al. 2011; Madhusudhan…”
Chemical enrichment of giant planets and discs due to pebble drift (2017, background): “…two ways: 1) change the C/O ratio of the solids accreted, for example by accreting from an as of yet unknown family of organic rich planetesimals (Lodders 2004) or 2) change the abundance of the gas to make it more carbon rich, such as through photoevaporation (Guillot & Hueso 2006; Monga &…”
Detection of water absorption in the day side atmosphere of HD 189733 b using ground-based high-resolution spectroscopy at 3.2 μm (2013, background): “…to provide constraints on the relative abundances of these molecules in planetary atmospheres, and hence an estimate of the carbon-to-oxygen ratio (C/O), which is thought to have strong implications for the formation and migration history of the planets (see e.g. Lodders 2004; Öberg et al. 2011).”
THE IMPRINT OF EXOPLANET FORMATION HISTORY ON OBSERVABLE PRESENT-DAY SPECTRA OF HOT JUPITERS (2016, background): “Such a carbon rich region inside of the iceline, but outside of a “tar” line is reminiscent of the one proposed by Lodders (2004) to explain the high C/O ratio in Jupiter.”
The Effect of Jupiter's Formation on the Distribution of Refractory Elements and Inclusions in Meteorites (2017, background): “This temperature is below the “tar line” temperature of T = 350 K (Lodders 2004), consistent with accretion and retention of carbonaceous material, but is above the snow line temperature; we predict that the UPB would not accrete ice.”
A comparison of chemistry and dust cloud formation in ultracool dwarf model atmospheres (2008, methodology): “…elements.2 2.2.3.3 Condensate treatment: For the application to substellar atmospheres, the CONDOR code treats condensate formation by removing primary condensates (i.e. condensates that form from condensing gases) from the gas into cloud layers (Lodders 2004; Lodders & Fegley 2006; see Table 1).”
C/O RATIO AS A DIMENSION FOR CHARACTERIZING EXOPLANETARY ATMOSPHERES (2012, background): “…the protoplanetary conditions required to form CRPs, such as a naturally carbon-rich gas in the disk (Oberg et al. 2011), or a sink of oxygen in the disk (Madhusudhan et al. 2011b), or the predominance of planetesimals rich in carbonaceous material like tar, instead of water-ice (Lodders, 2004).”
NEAR-INFRARED SPECTROSCOPY OF THE EXTRASOLAR PLANET HR 8799 b (2010, background): “…from Hinz et al. (2010). metal-rich atmospheric compositions (metal abundances range from ∼2 to 4 times solar values for Jupiter, up to ∼10 times for Saturn, and even higher for some species in Uranus and Neptune; Atreya et al. 2003; Lodders 2004; Flasar et al. 2005; Fortney & Nettelmann 2009).”
EXOPLANET ALBEDO SPECTRA AND COLORS AS A FUNCTION OF PLANET PHASE, SEPARATION, AND METALLICITY (2010, background): “…Guillot et al. 2004), direct accretion of metal-rich disk gas (Guillot & Hueso 2006), or chemical fractionation within the planet (Stevenson & Salpeter 1977; Lodders 2004) in enriching gas giants in heavy elements is relevant both to understanding our own solar system as well as exoplanet systems.”