Hot Jupiters with relatives: discovery of additional planets in orbit around WASP-41 and WASP-47

Neveu-VanMalle, M.; Queloz, D.; Anderson, D. R.; Brown, D. J. A.; Cameron, A. Collier; Delrez, Laetitia; Díaz, R. F.; Gillon, M.; Hellier, C.; Jehin, Emmanuël; Lister, Tim; Pepe, F.; Rojo, P.; Ségransan, D.; Triaud, A. H. M. J.; Turner, O. D.; Udry, S.

doi:10.1051/0004-6361/201526965

Cited by 69 publications

(69 citation statements)

References 44 publications

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“…Thanks to this detection, it was proposed as a target for the K2 mission. In the meantime, the radial-velocity monitoring of the system unveiled a second, long period gas giant (Neveu-VanMalle et al 2016). Becker et al (2015) analyzed the K2 data and announced the presence of two super-Earths, one inner to the hot Jupiter, and one between both gas giants.…”

Section: Formation Of Hot Jupitersmentioning

confidence: 99%

Warm Jupiters Are Less Lonely Than Hot Jupiters: Close Neighbors

Huang

Triaud

2016

ApJ

206

214

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Exploiting the Kepler transit data, we uncover a dramatic distinction in the prevalence of sub-Jovian companions, between systems that contain hot Jupiters (periods inward of 10 days) and those that host warm Jupiters (periods between 10 and 200 days). Hot Jupiters, with the singular exception of WASP-47b, do not have any detectable inner or outer planetary companions (with periods inward of 50 days and sizes down to 2R Earth ). Restricting ourselves to inner companions, our limits reach down to 1R Earth . In stark contrast, half of the warm Jupiters are closely flanked by small companions. Statistically, the companion fractions for hot and warm Jupiters are mutually exclusive, particularly in regard to inner companions.The high companion fraction of warm Jupiters also yields clues to their formation. The warm Jupiters that have close-by siblings should have low orbital eccentricities and low mutual inclinations. The orbital configurations of these systems are reminiscent of those of the low-mass, close-in planetary systems abundantly discovered by the Kepler mission. This, and other arguments, lead us to propose that these warm Jupiters are formed in-situ. There are indications that there may be a second population of warm Jupiters with different characteristics. In this picture, WASP-47b could be regarded as the extending tail of the in-situ warm Jupiters into the hot Jupiter region, and does not represent the generic formation route for hot Jupiters. Subject headings:1. FOREWORDS The origin of hot Jupiters (HJs, period inward of ∼ 10 days) has remained an unsolved issue. Although multiple scenarios have been proposed (disk migration, planet scattering, secular migration, etc.), none seem capable of satisfying all observational constraints. The recent discovery of two low-mass planetary companions (Becker et al. 2015) close to the hot Jupiter WASP-47b (Hellier et al. 2012) further obfuscates the picture. Motivated by the large population of low mass, closely-packed planets at small distances away from their host stars (Mayor et al. 2011;Howard et al. 2012;Borucki et al. 2011;Lissauer et al. 2011), and by the realization that some of them could have accumulated enough mass to undergo run-away gas accretion (Lee et al. 2014), Boley et al. (2016);Batygin et al. (2015) argue that WASP-47b, and possibly all hot Jupiters, were formed in-situ, instead of somehow transported inward. Only a tiny fraction of super-Earths need follow this path to be able to match the occurrence rate of hot Jupiters.While this seems a reasonable proposal for WASP-47b, could it explain the majority of hot Jupiters? To answer this, we focus on the following issue: is WASP-47b a generic hot Jupiter in terms of co-habiting with other planets? Currently, this question is best addressed by exploiting the Kepler data to look for small transiting bodies in systems hosting (either confirmed or candidate) There is a second goal to our paper: understanding the warm Jupiters (WJs). By this term we refer specifically to those giant planets orb...

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Section: Formation Of Hot Jupitersmentioning

confidence: 99%

Warm Jupiters Are Less Lonely Than Hot Jupiters: Close Neighbors

Huang

Triaud

2016

ApJ

206

214

View full text Add to dashboard Cite

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“…Further, WASP-47 comprises a hot Jupiter, a nearby super-Earth, a nearby Neptune, and a more distant Jupiter. The inner three planets are known to transit and the orbit of the hot Jupiter is nearaligned (Hellier et al 2012;Sanchis-Ojeda et al 2015;Becker et al 2015;Neveu-VanMalle et al 2016). It seems likely that disc migration operated in both of these hot-Jupiter systems.…”

Section: The Migration Of Short Period Giant Planetsmentioning

confidence: 99%

The discoveries of WASP-91b, WASP-105b and WASP-107b: Two warm Jupiters and a planet in the transition region between ice giants and gas giants

Anderson

Cameron

Delrez

et al. 2017

A&A

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We report the discoveries of three transiting exoplanets. WASP-91b is a warm Jupiter (1.34 M Jup , 1.03 R Jup ) in a 2.8-day orbit around a metal-rich K3 star. WASP-105b is a warm Jupiter (1.8 M Jup , 0.96 R Jup ) in a 7.9-day orbit around a metal-rich K2 star. WASP-107b is a warm super-Neptune/sub-Saturn (0.12 M Jup , 0.94 R Jup ) in a 5.7-day orbit around a solar-metallicity K6 star. Considering that giant planets seem to be more common around stars of higher metallicity and stars of higher mass, it is notable that the hosts are all metalrich, late-type stars. With orbital separations that place both WASP-105b and WASP-107b in the weak-tide regime, measurements of the alignment between the planets' orbital axes and their stars' spin axes may help us to understand the inward migration of shortperiod, giant planets. The mass of WASP-107b (2.2 M Nep , 0.40 M Sat ) places it in the transition region between the ice giants and gas giants of the Solar System. Its radius of 0.94 R Jup suggests that it is a low-mass gas giant with a H/He-dominated composition. The planet thus sets a lower limit of 2.2 M Nep on the planetary mass above which large gaseous envelopes can be accreted and retained by proto-planets on their way to becoming gas giants. We may discover whether WASP-107b more closely resembles an ice giant or a gas giant by measuring its atmospheric metallicity via transmission spectroscopy, for which WASP-107b is a very good target.

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“…Because of this, Hα has been used by several authors (e.g. Pasquini & Pallavicini 1991;Montes et al 1995;Cincunegui et al 2007a,b;Robertson et al 2013Robertson et al , 2014Neveu-VanMalle et al 2016). The parameters used for our H α analysis can be found in Díaz et al (2016a).…”

Section: Activity Indicatorsmentioning

confidence: 99%

The SOPHIE search for northern extrasolar planets

Rey

Hébrard

Bouchy

et al. 2017

A&A

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We present new radial velocity measurements for three low-metallicity solar-like stars observed with the SOPHIE spectrograph and its predecessor ELODIE, both installed at the 193 cm telescope of the Haute-Provence Observatory, allowing the detection and characterization of three new giant extrasolar planets in intermediate periods of 1.7 to 3.7 years. All three stars, HD17674, HD42012 and HD29021 present single giant planetary companions with minimum masses between 0.9 and 2.5 M Jup . The range of periods and masses of these companions, along with the distance of their host stars, make them good targets to look for astrometric signals over the lifetime of the new astrometry satellite Gaia. We discuss the preliminary astrometric solutions obtained from the first Gaia data release.

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Hot Jupiters with relatives: discovery of additional planets in orbit around WASP-41 and WASP-47

Cited by 69 publications

References 44 publications

Warm Jupiters Are Less Lonely Than Hot Jupiters: Close Neighbors

Warm Jupiters Are Less Lonely Than Hot Jupiters: Close Neighbors

The discoveries of WASP-91b, WASP-105b and WASP-107b: Two warm Jupiters and a planet in the transition region between ice giants and gas giants

The SOPHIE search for northern extrasolar planets

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