Physics of Substellar Objects Interiors, Atmospheres, Evolution

Guillot, T.

doi:10.1007/978-3-540-31470-7_2

Cited by 2 publications

(1 citation statement)

References 144 publications

(248 reference statements)

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“…Based on observed gravitational moments and other basic parameters, (2000) found an absolute maximum proportion of gas (by mass) of about 30% for Uranus and Neptune, under the unrealistic assumption that the planets were composed entirely of rock and gas. Models constructed assuming a rocky core surrounded by a mantle composed of ice and gas, and constrained by available equation of state data, are reviewed by Hubbard et al (1995) and Guillot (2006). These models generally agree that the proportion of gas (by mass) in these planets is around 5-15%, so the O/H ratio in these planets should be very large.…”

Section: Volatile Enrichments In the Other Outer Planetsmentioning

confidence: 99%

Oxygen and Other Volatiles in the Giant Planets and their Satellites

Wong

Lunine

Atreya

et al. 2008

Reviews in Mineralogy and Geochemistry

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Giant planet atmospheric composition and satellite densities provide insights into protoplanetary disk conditions. Abundances of condensable species and noble gases in wellmixed atmospheres can distinguish among several giant planet formation scenarios, and satellite densities are fi rst order measurements of ice:rock ratios. Recent work on protosolar abundances, relying on three-dimensional spectroscopic modeling of the solar photosphere, provides the framework for the interpretation of measurements.Model densities of protoplanetary disk condensates are shown as a function of carbon partitioning between CO, CH 4 and organics. Comparison with observed satellite densities shows that Saturn's icy satellites are inconsistent with solar composition, and must either have formed in a water-rich environment or have suffered a complex collisional history. The larger satellites of the giant planets are consistent with solar composition, with densities that speak of variation in the partitioning of carbon. 68_Oxygen.indb 219 68_Oxygen.indb 219 1/9/2008 11:13:34 PM 1/9/2008 11:13:34 PM 220 Wong et al.Thermochemical equilibrium calculations predict water as the deepest tropospheric cloud on Jupiter, the planet with the best-constrained bulk water abundance. Yet cloud base pressure levels, remote spectroscopic water vapor measurements, and in situ mass-spectral measurements have all been unable to distinguish conclusively between subsolar and supersolar Jovian bulk water abundances, due to modeling assumptions and/or the spatially-variable water vapor distribution in Jupiter's troposphere. Modeling of images of lightning fl ashes is consistent with supersolar water abundances.Galileo probe measurements are consistent with an enrichment factor of 4±2 over the protosolar values for most volatiles other than water (C, N, S, and the noble gases Ar, Kr, and Xe). With that of oxygen unknown, Jupiter's enrichments of other volatiles could be explained in terms of enrichment by heretofore unidentifi ed solar composition icy planetesimals, by planetesimals containing volatiles trapped in water ice clathrates, or by enriched gas in the evolved disk. All models involving delivery of elements by planetesimals require planetesimal formation at temperatures below 40 K, to trap argon and molecular nitrogen. Although atmospheric C/H ratios have been measured for all four giant planets, a conclusive test of the competing formation scenarios cannot be made until O/H is measured on all four planets (extremely diffi cult on Uranus and Neptune), and abundances of the other volatiles and noble gases are measured for the outer three.

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Section: Volatile Enrichments In the Other Outer Planetsmentioning

confidence: 99%

Oxygen and Other Volatiles in the Giant Planets and their Satellites

Wong

Lunine

Atreya

et al. 2008

Reviews in Mineralogy and Geochemistry

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Radio Emission From Red-Giant Hot Jupiters

Fujii

Spiegel

Mroczkowski

et al. 2016

ApJ

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When planet-hosting stars evolve off the main sequence and go through the red-giant branch, the stars become orders of magnitudes more luminous and, at the same time, lose mass at much higher rates than their mainsequence counterparts. Accordingly, if planetary companions exist around these stars at orbital distances of a few au, they will be heated up to the level of canonical hot Jupiters and also be subjected to a dense stellar wind. Given that magnetized planets interacting with stellar winds emit radio waves, such "Red-Giant Hot Jupiters" (RGHJs) may also be candidate radio emitters. We estimate the spectral auroral radio intensity of RGHJs based on the empirical relation with the stellar wind as well as a proposed scaling for planetary magnetic fields. RGHJs might be intrinsically as bright as or brighter than canonical hot Jupiters and about 100 times brighter than equivalent objects around main-sequence stars. We examine the capabilities of low-frequency radio observatories to detect this emission and find that the signal from an RGHJ may be detectable at distances up to a few hundred parsecs with the Square Kilometer Array.

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Physics of Substellar Objects Interiors, Atmospheres, Evolution

Cited by 2 publications

References 144 publications

Oxygen and Other Volatiles in the Giant Planets and their Satellites

Oxygen and Other Volatiles in the Giant Planets and their Satellites

Radio Emission From Red-Giant Hot Jupiters

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