Composition and origin of the atmosphere of Jupiter—an update, and implications for the extrasolar giant planets

By S. Atreya, P. Mahaffy, H. Niemann, M. Wong, T. Owen. 2003

163 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Ecology

View Paper: https://www.semanticscholar.org/paper/d3b343fcdffc320508d99988ce65dcf570d46c21

How researchers see this paper

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

In Astronomy and Astrophysics

1. Jon Fortney
2. N. Madhusudhan
3. M. Marley
4. A. Showman
5. Adam Burrows
6. M. Line
7. K. Lodders
8. Laura Kreidberg

In Ecology

1. Jon Fortney
2. K. Lodders
3. M. Marley
4. N. Madhusudhan
5. D. Saumon
6. A. Showman
7. N. Nettelmann
8. Kerri L. Cahoy

Citations in the corpus

• The effect of condensates on the characterization of transiting planet atmospheres with transmission spectroscopy (2005, background): “…were put forth in Charbonneau et al. (2002), including a global underabundance of sodium, ionization of sodium by stellar flux, sodium being tied up in condensates or molecules (see also Atreya et al. 2003), or high clouds obscuring the absorption of sodium (see also Seager & Sasselov 2000).”
• Possible Solutions to the Radius Anomalies of Transiting Giant Planets (2006, background): “In situ and remote-sensing measurements of the atmospheric compositions of the giant planets Jupiter and Saturn reveal that most of the dominant elements, such as carbon, nitrogen, and sulfur, exist there in supersolar abundances (Atreya et al. 2003).”
• 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).”
• JUpiter ICy moons Explorer (JUICE): An ESA mission to orbit Ganymede and to characterise the Jupiter system (2013, background): “Jupiter’s atmospheric composition is the product of a myriad of thermochemical and photochemical pathways (Atreya et al., 2003).”
• Jupiter Formed with More Tar than Ice (2004, methodology): “…Probe Mass Spectrometer measured the content of noble gases, hydrogen, carbon (as CH4), nitrogen (as NH3), oxygen (as H2O), sulfur (as H2S), and other minor constituents in Jupiter’s atmosphere down to a pressure of 20 bars (Niemann et al. 1998; Mahaffy et al. 2000; Atreya et al. 1999, 2003).”
• Sulphur-bearing species in the coma of comet 67P/Churyumov–Gerasimenko (2016, background): “For sulphur, this enhancement factor is up to 2.5 (Atreya et al. 2003).”
• Material Enhancement in Protoplanetary Nebulae by Particle Drift through Evaporation Fronts (2004, background): “Looking somewhat further beyond the boundaries of this paper, we suspect that evaporation fronts of low-temperature volatiles might also have important implications for their enhancement in the gaseous envelope of Jupiter, a problem highlighted by Owen et al. (1999) and Atreya et al. (2003).”
• EXOPLANET ALBEDO SPECTRA AND COLORS AS A FUNCTION OF PLANET PHASE, SEPARATION, AND METALLICITY (2010, background): “For example, Jupiter has ∼ 2× to 4× solar abundances of oxygen, carbon, nitrogen, sulfur, and various noble gases (Atreya et al. 2003).”
• Updated Galileo probe mass spectrometer measurements of carbon, oxygen, nitrogen, and sulfur on Jupiter (2004, result): “This estimate is consistent with previously stated GPMS deep H2S mixing ratios ( Atreya et al., 2003, 1999; Wong et al., 1999; Niemann et al., 1998), but has a larger uncertainty to reflect the more thorough error analysis in this work.”
• Synthetic Spectra and Colors of Young Giant Planet Atmospheres: Effects of Initial Conditions and Atmospheric Metallicity (2008, background): “Except for oxygen, an enhancement of∼2-4× solar for each element was found (Atreya et al. 2003), although the oxygen abundance determination may have been hindered by meteorological effects (Showman & Ingersoll 1998).”
• Ab Initio Equation of State Data for Hydrogen, Helium, and Water and the Internal Structure of Jupiter (2007, unknown): “Choosing threefold enrichment in heavy elements in accordance with measurements (Atreya et al. 2003; Mahaffy et al. 2000) for the molecular envelope, an enrichment of 7.5 times solar was required in the metallic envelope to match J2, in total 35 M .”
• JUPITER MODELS WITH IMPROVED AB INITIO HYDROGEN EQUATION OF STATE (H-REOS.2) (2011, background): “3) are taken to be representative for the convective region below the 1-bar level, the outer boundary of our models, as they are not subject to non-equilibrium chemistry, cloud formation, or other processes that could significantly affect their abundance at such low altitudes (Atreya et al. 2003).”
• 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).”