Inflating Hot Jupiters With Ohmic Dissipation

Batygin, Konstantin; Stevenson, D. J.

doi:10.1088/2041-8205/714/2/l238

Cited by 276 publications

(384 citation statements)

References 30 publications

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“…A detection of potassium in XO-2b helps support this overall picture. Potassium and sodium could also play important roles in inflating hot Jupiters through ohmic dissipation mechanisms (Batygin & Stevenson 2010). Notably, there is also no particular evidence for K I photoionization, which could have been evident by depletion at high altitudes.…”

Section: Discussionmentioning

confidence: 99%

Gran Telescopio Canarias OSIRIS transiting exoplanet atmospheric survey: detection of potassium in XO-2b from narrowband spectrophotometry

Sing

Désert

Fortney

et al. 2011

A&A

131

138

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We present Gran Telescopio Canarias (GTC) optical transit narrowband photometry of the hot-Jupiter exoplanet XO-2b using the OSIRIS instrument. This unique instrument has the capabilities to deliver high-cadence narrowband photometric lightcurves, allowing us to probe the atmospheric composition of hot Jupiters from the ground. The observations were taken during three transit events that cover four wavelengths at spectral resolutions near 500, necessary for observing atmospheric features, and have near-photon limited sub-mmag precisions. Precision narrowband photometry on a large aperture telescope allows for atmospheric transmission spectral features to be observed for exoplanets around much fainter stars than those of the well studied targets HD 209458b and HD 189733b, providing access to the majority of known transiting planets. For XO-2b, we measure planet-to-star radius contrasts of R pl /R = 0.10508 ± 0.00052 at 6792 Å, 0.10640 ± 0.00058 at 7582 Å, and 0.10686 ± 0.00060 at 7664.9 Å, and 0.10362 ± 0.00051 at 8839 Å. These measurements reveal significant spectral features at two wavelengths, with an absorption level of 0.067 ± 0.016% at 7664.9 Å caused by atmospheric potassium in the line core (a 4.1-σ significance level), and an absorption level of 0.058 ± 0.016% at 7582 Å, (a 3.6-σ significance level). When comparing our measurements to hot-Jupiter atmospheric models, we find good agreement with models that are dominated in the optical by alkali metals. This is the first evidence for potassium in an extrasolar planet, an element that has along with sodium long been supposed to be a dominant source of opacity at optical wavelengths for hot Jupiters.

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Section: Discussionmentioning

confidence: 99%

Gran Telescopio Canarias OSIRIS transiting exoplanet atmospheric survey: detection of potassium in XO-2b from narrowband spectrophotometry

Sing

Désert

Fortney

et al. 2011

A&A

131

138

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“…Moreover, the unusually large radius (compared to its sub-Saturn mass) cannot be explained by the standard coreless model (e.g., Fortney et al 2007), and places it in the short-period Neptune desert, a region between Jovian and super-Earth planets with a lack of detected planets (Howard et al 2012;Mazeh et al 2016). Several inflation mechanisms have been proposed to explain this inflation, including tidal heating, enhanced atmospheric opacity, Ohmic heating, and/or reinflation by the host star when moving toward the red giant branch phase (Leconte et al 2010;Batygin & Stevenson 2010;Batygin et al 2011;Lammer et al 2013;Rauscher & Menou 2013;Spiegel & Burrows 2013;Wu & Lithwick 2013;Lopez & Fortney 2016), although no concluding observations have been established yet to favor one or the other. The formation and evolution mechanisms of WASP-127b are therfore very intriguing, given its transition size between these two classes of planets.…”

Section: Introductionmentioning

confidence: 99%

Feature-rich transmission spectrum for WASP-127b

Πάλλη

Chen

Nowak

et al. 2017

A&A

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Context. WASP-127b is a planet with one of the lowest densities discovered to date. With a sub-Saturn mass (M p = 0.18 ± 0.02 M J ) and super-Jupiter radius (R p = 1.37 ± 0.04 R J ), it orbits a bright G5 star that is about to leave the main-sequence. Aims. We aim to explore the atmosphere of WASP-127b in order to retrieve its main atmospheric components, and to find hints for its intriguing inflation and evolutionary history. Methods. We used the ALFOSC spectrograph at the NOT telescope to observe a low-resolution (R ∼ 330, seeing limited) long-slit spectroscopic time series during a planetary transit, and present here the first transmission spectrum for WASP-127b. Results. We find a strong Rayleigh slope at blue wavelengths and a hint of Na absorption, although the quality of the data does not allow us to claim a detection. At redder wavelengths the absorption features of TiO and VO are the best explanation to fit the data. Conclusions. Although observations with a higher signal-to-noise ratio are needed to conclusively confirm the absorption features, WASP-127b seems to posses a cloud-free atmosphere and is one of the best targets on which to perform further characterization studies in the near future.

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“…Several have markedly low densities, with WASP-17b (Anderson et al 2010(Anderson et al , 2011, Kepler-12b (Fortney et al 2011) and Kepler-7b (Latham et al 2010) having a density less than 1/10 that of Jupiter. The mechanisms for producing such bloated planets are at present unclear (Fortney & Nettelmann 2010), but several have been proposed, including Ohmic heating in the planetary atmosphere (Batygin & Stevenson 2010;Perna et al 2010) and thermal tidal effects (Arras & Socrates 2010).…”

Section: Introductionmentioning

confidence: 99%

WASP-78b and WASP-79b: two highly-bloated hot Jupiter-mass exoplanets orbiting F-type stars in Eridanus

Smalley

Anderson

Cameron

et al. 2012

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We report the discovery of WASP-78b and WASP-79b, two highly-bloated Jupiter-mass exoplanets orbiting F-type host stars. WASP-78b orbits its V = 12.0 host star (TYC 5889-271-1) every 2.175 days and WASP-79b orbits its V = 10.1 host star (CD-30 1812) every 3.662 days. Planetary parameters have been determined using a simultaneous fit to WASP and TRAPPIST transit photometry and CORALIE radial-velocity measurements. For WASP-78b a planetary mass of 0.89 ± 0.08 M Jup and a radius of 1.70 ± 0.11 R Jup is found. The planetary equilibrium temperature of T P = 2350 ± 80 K for WASP-78b makes it one of the hottest of the currently known exoplanets. WASP-79b its found to have a planetary mass of 0.90 ± 0.08 M Jup , but with a somewhat uncertain radius due to lack of sufficient TRAPPIST photometry. The planetary radius is at least 1.70 ± 0.11 R Jup , but could be as large as 2.09 ± 0.14 R Jup , which would make WASP-79b the largest known exoplanet.

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Inflating Hot Jupiters With Ohmic Dissipation

Cited by 276 publications

References 30 publications

Gran Telescopio Canarias OSIRIS transiting exoplanet atmospheric survey: detection of potassium in XO-2b from narrowband spectrophotometry

Gran Telescopio Canarias OSIRIS transiting exoplanet atmospheric survey: detection of potassium in XO-2b from narrowband spectrophotometry

Feature-rich transmission spectrum for WASP-127b

WASP-78b and WASP-79b: two highly-bloated hot Jupiter-mass exoplanets orbiting F-type stars in Eridanus

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