Hot Jupiters: Origins, Structure, Atmospheres

Fortney, Jonathan J.; Dawson, Rebekah I.; Komacek, Thaddeus D.

doi:10.1029/2020je006629

Cited by 78 publications

(61 citation statements)

References 468 publications

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“…Particularly for the scenarios where TOI-1266c loses most of its hydrogen, nitrogen could oxidize into NO x compounds, analogous to NO x derived from persistent lightning storms (e.g., Ardaseva et al 2017). However, the temperature profiles used here all lie above the N 2 /NH 3 equalabundance pressure-temperature curve (e.g., Fortney et al 2021), suggesting that ammonia incorporated as ice may affect the total atmospheric pressure (as N 2 ) and act as a source of reducing power by equilibrating to form H 2 at depth without NH 3 necessarily becoming a major constituent in the atmosphere. Lastly, if TOI-1266c has a silicate core, then moderately volatile elements like Na and Cl could contribute to atmospheric composition either directly (that is, there may be a rock vapor atmosphere) or indirectly (e.g., through catalytic and secondary reactions with the major species).…”

Section: Chemical Considerationsmentioning

confidence: 86%

A Snowball in Hell: The Potential Steam Atmosphere of TOI-1266c

et al. 2022

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TOI-1266c is a recently discovered super-Venus in the radius valley orbiting an early M dwarf. However, its notional bulk density (∼2.2 g cm−3) is consistent with a large volatile fraction, suggesting that it might have volatile reservoirs that have survived billions of years at more than twice Earth’s insolation. On the other hand, the upper mass limit paints a picture of a cool super-Mercury dominated by >50% iron core (∼9.2 g cm−3) that has tiptoed up to the collisional stripping limit and into the radius gap. Here we examine several hypothetical states for TOI-1266c using a combination of new and updated open-source atmospheric escape, radiative−convective, and photochemical models. We find that water-rich atmospheres with trace amounts of H2 and CO2 are potentially detectable (S/N > ∼ 5) in less than 20 hr of James Webb Space Telescope (JWST) observing time. We also find that water vapor spectral features are not substantially impacted by the presence of high-altitude water or ice clouds owing to the presence of a significant amount of water above the cloud deck, although further work with self-consistent cloud models is needed. Regardless of its mass, however, TOI-1266c represents a unique proving ground for several hypotheses related to the evolution of sub-Neptunes and Venus-like worlds, particularly those near the radius valley.

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Section: Chemical Considerationsmentioning

confidence: 86%

A Snowball in Hell: The Potential Steam Atmosphere of TOI-1266c

et al. 2022

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“…Heat deposition and mass loss The planet could be efficiently heated at depth, either driven by Ohmic dissipation, tidal heating, or stellar flux deposition at high pressures. Ohmic dissipation seems to be the most promising mechanism 42 . This is because the atmosphere of WASP-193 b is hot enough (with T eq of 1275 K) that trace elements in the H-He gas can be partially ionized and allow for atmospheric currents to penetrate deep into the interior.…”

Section: Planet Interiormentioning

confidence: 99%

WASP-193b: An extremely low-density super-Neptune

Barkaoui

Pozuelos

Hellier

et al. 2022

Preprint

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Gas giants transiting bright nearby stars are key objects for our understanding of planetary system formation and evolution mechanisms. This paper presents a new transiting exoplanet discovered by the WASP-South transit survey, WASP-193b. WASP-193b orbits its Vmag = 12.0 F9 main-sequence host star every 6.25d. Our analyses found that WASP-193b has a mass of Mp = 0.146 ± 0.033 M_Jup, a radius of R_p = 1.58 ± 0.14R_Jup, translating into an extremely low density of rho_p = 0.049 ± 0.015g/cm3. The planet was confirmed photometrically by the 0.6-m TRAPPIST-South and 1.0-m SPECULOOS-South telescopes and spectroscopically by the ESO-3.6-m/HARPS and Euler-1.2-m/CORALIE spectrographs. The combination of its large transit depth (dF≈1.4%), its super-low density, its high-equilibrium temperature (T_eq = 1275 ± 40K), and the infrared brightness of its host star (magnitude Kmag=10.7) makes WASP-193b an exquisite target for a detailed atmospheric characterization by transmission spectroscopy.

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“…Such drastic day-night temperature contrasts in these strongly irradiated atmospheres drive a wealth of atmospheric waves, jets, and turbulence that affects the atmospheric composition and structure (e.g., Showman & Guillot 2002). The exciting observations of strongly irradiated atmospheres motivate a series of theoretical studies to understand the relevant physical and chemical atmospheric processes, including the radiative cooling and advection (e.g., Showman & Guillot 2002), ohmic dissipation (e.g., Perna et al 2010), non-equilibrium chemistry (e.g., Agúndez et al 2014b), non-homogeneous cloud formation and distribution (e.g., Parmentier et al 2016;Powell et al 2018), and hydrogen dissociation and recombination effects (Bell & Cowan 2018;Komacek & Tan 2018;Tan & Showman 2019) (see Heng & Showman 2015;Parmentier & Crossfield 2018;Showman et al 2020;Fortney et al 2021 for reviews). Despite the significant progress made on both the observational and modeling fronts on understanding the strongly irradiated atmospheres, many fundamental questions remained unanswered: What are the dominating physical mechanisms in redistributing irradiation energy at different rotation rates, temperatures, and altitudes?…”

Section: Introductionmentioning

confidence: 99%

Mapping the pressure-dependent day-night temperature contrast of a strongly irradiated atmosphere with HST spectroscopic phase curve

Lew,

Apai,

Zhou

et al. 2021

Preprint

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Many brown dwarfs are on ultra-short period and tidally-locked orbits around white dwarf hosts. Because of these small orbital separations, the brown dwarfs are irradiated at levels similar to hot Jupiters. Yet, they are easier to observe than hot Jupiters because white dwarfs are fainter than main-sequence stars at near-infrared wavelengths. Irradiated brown dwarfs are, therefore, ideal hot Jupiter analogs for studying the atmospheric response under strong irradiation and fast rotation. We present the 1.1-1.67 µm spectroscopic phase curve of the irradiated brown dwarf (SDSS1411-B) in the SDSS J141126.20+200911.1 brown-dwarf white-dwarf binary with the near-infrared G141 grism of Hubble Space Telescope Wide Field Camera 3. SDSS1411-B is a 50M Jup brown dwarf with an irradiation temperature of 1300K and has an orbital period of 2.02864 hours. Our best-fit model suggests a phase-curve amplitude of 1.4% and places an upper limit of 11 degrees for the phase offset from the secondary eclipse. After fitting the white-dwarf spectrum, we extract the phase-resolved brown-dwarf emission spectra. We report a highly wavelength-dependent day-night spectral variation, with the water-band flux variation of about 360 ± 70% and a comparatively small J-band flux variation of 37 ± 2%. By combining the atmospheric modeling results and the day-night brightness-temperature variations, we derive a pressure-dependent temperature contrast. We discuss the difference in the spectral features of SDSS1411-B and hot Jupiter WASP-43b, and the lower-than-predicted day-night temperature contrast of J4111-BD. Our study provides the high-precision observational constraints on the atmospheric structures of an irradiated brown dwarf at different orbital phases.

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Hot Jupiters: Origins, Structure, Atmospheres

Cited by 78 publications

References 468 publications

A Snowball in Hell: The Potential Steam Atmosphere of TOI-1266c

A Snowball in Hell: The Potential Steam Atmosphere of TOI-1266c

WASP-193b: An extremely low-density super-Neptune

Mapping the pressure-dependent day-night temperature contrast of a strongly irradiated atmosphere with HST spectroscopic phase curve

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