Evolution of Ohmically Heated Hot Jupiters

Batygin, Konstantin; Stevenson, D. J.; Bodenheimer, Peter

doi:10.1088/0004-637x/738/1/1

Cited by 170 publications

(267 citation statements)

References 46 publications

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“…10) and hence requires an additional source of heat to explain its size, in line with what is inferred from a significant fraction of close-in transiting giant planets (e.g. Guillot et al 2006;Laughlin et al 2011;Batygin et al 2011 Fig. 8.…”

Section: Planetary System Evolution Modelssupporting

confidence: 61%

Transiting exoplanets from the CoRoT space mission

Almenara¹,

Bouchy²,

Gaulme³

et al. 2013

A&A

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We report the discovery of two transiting exoplanets, CoRoT-25b and CoRoT-26b, both of low density, one of which is in the Saturn mass-regime. For each star, ground-based complementary observations through optical photometry and radial velocity measurements secured the planetary nature of the transiting body and allowed us to fully characterize them. For CoRoT-25b we found a planetary mass of 0.27 ± 0.04 M Jup , a radius of 1.08 +0.3 −0.10 R Jup and hence a mean density of 0.15 +0.15 −0.06 g cm −3 . The planet orbits an F9 mainsequence star in a 4.86-day period, that has a V magnitude of 15.0, solar metallicity, and an age of 4.5 +1.8 −2.0 -Gyr. CoRoT-26b orbits a slightly evolved G5 star of 9.06 ± 1.5-Gyr age in a 4.20-day period that has solar metallicity and a V magnitude of 15.8. With a mass of 0.52± 0.05 M Jup , a radius of 1.26 +0.13 −0.07 R Jup , and a mean density of 0.28 +0.09 −0.07 g cm −3 , it belongs to the low-mass hot-Jupiter population. Planetary evolution models allowed us to estimate a core mass of a few tens of Earth mass for the two planets with heavy-element mass fractions of 0.52 +0.08 −0.15 and 0.26 +0.05 −0.08 , respectively, assuming that a small fraction of the incoming flux is dissipated at the center of the planet. In addition, these models indicate that CoRoT-26b is anomalously large compared with what standard models could account for, indicating that dissipation from stellar heating could cause this size. Key words. planetary systems -techniques: photometric -techniques: radial velocities -techniques: spectroscopicThe CoRoT space mission, launched on December 27th 2006, has been developed and is operated by CNES, with the contribution

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Section: Planetary System Evolution Modelssupporting

confidence: 61%

Transiting exoplanets from the CoRoT space mission

Almenara¹,

Bouchy²,

Gaulme³

et al. 2013

A&A

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“…However, we do not know precisely how much the planet could actually dissipate in its interior (e.g. Guillot & Showman 2002;Batygin et al 2011;Laughlin et al 2011): reducing by 2 (respectively 5 and 10) the amount of energy dissipated in the planet's interior, moves the 0 M ⊕ line from 1.444 to 1.391 R Jup (respectively 1.332 and 1.294, Fig. 8), which corresponds to a 3.7% reduction in radius (respectively 7.7% and 10%).…”

Section: Referencesmentioning

confidence: 99%

SOPHIE velocimetry ofKeplertransit candidates XI. Kepler-412 system: probing the properties of a new inflated hot Jupiter

Deleuil

Almenara

Santerne

et al. 2014

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Context. Hot Jupiters are still a fascinating exoplanet population that presents a diversity we are still far from understanding. Highprecision photometric observations combined with radial velocity measurements give us a unique opportunity to constrain their properties better, on both their internal structure and their atmospheric bulk properties. Aims. We initiated a follow-up program of Kepler-released planet candidates with the goal of confirming the planetary nature of a number of them through radial velocity measurements. For those that successfully passed the radial velocity screening, we furthermore performed a detailed exploration of their properties to characterize the systems. As a byproduct, these systematic observations allow us to consolidate the exoplanets' occurrence rate. Methods. We performed a complete analysis of the Kepler-412 system, listed as planet candidate KOI-202 in the Kepler catalog, by combining the Kepler observations from Q1 to Q15, to ground-based spectroscopic observations that allowed us to derive radial velocity measurements, together with the host-star parameters and properties. We also analyzed the light curve to derive the star's rotation period and the phase function of the planet, including the secondary eclipse. Results. We secured the planetary nature of Kepler-412b. We found the planet has a mass of 0.939 ± 0.085 M Jup and a radius of 1.325 ± 0.043 R Jup , which makes it a member of the bloated giant subgroup. It orbits its G3 V host star in 1.72 days. The system has an isochronal age of 5.1 Gyr, consistent with its moderate stellar activity as observed in the Kepler light curve and the rotation of the star of 17.2 ± 1.6 days. From the detected secondary we derived the day-side temperature as a function of the geometric albedo. We estimated that the geometrical albedo A g should be between 0.094 ± 0.015 and 0.013 +0.017 −0.013 and the brightness of the day side 2380 ± 40 K. The measured night-side flux corresponds to a night-side brightness temperature of 2154 ± 83 K, much greater than what is expected for a planet with homogeneous heat redistribution. From the comparison to star and planet evolution models, we found that dissipation should operate in the deep interior of the planet. This modeling also shows that despite its inflated radius, the planet presents a noticeable amount of heavy elements, which accounts for a mass fraction of 0.11 ± 0.04.

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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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Evolution of Ohmically Heated Hot Jupiters

Cited by 170 publications

References 46 publications

Transiting exoplanets from the CoRoT space mission

Transiting exoplanets from the CoRoT space mission

SOPHIE velocimetry ofKeplertransit candidates XI. Kepler-412 system: probing the properties of a new inflated hot Jupiter

Feature-rich transmission spectrum for WASP-127b

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