Discovery and characterization of the exoplanets WASP-148b and c

Hébrard, G.; Díaz, R. F.; Correia, A. C. M.; Cameron, A. Collier; Laskar, Jacques; Pollacco, D.; Almenara, J. M.; Anderson, D. R.; Barros, S. C. C.; Boisse, I.; Bonomo, A. S.; Bouchy, F.; Boué, G.; Boumis, P.; Brown, D. J. A.; Dalal, S.; Deleuil, M.; Doyle, A. P.; Haswell, C. A.; Hellier, C.; Osborn, H.; Kiefer, F.; Kolb, U.; Lam, K. W. F.; Étangs, A. Lecavelier des; Lopez, T.; Martin-Lagarde, Marine; Maxted, P. F. L.; McCormac, J.; Nielsen, L. D.; Πάλλη, Ε.; Queloz, D.; Santerne, A.; Smalley, B.; Turner, O. D.; Udry, S.; Vérilhac, D.; West, R. G.; Wheatley, P. J.; Wilson, Paul

doi:10.1051/0004-6361/202038296

Cited by 16 publications

(5 citation statements)

References 86 publications

(70 reference statements)

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“…A value of f opa = 10 −2 is not small enough, whereas f opa = 10 −3 results in approximately 6% of the equal-mass simulations forming a hot Jupiter, which is higher than the ∼ 1% rate obtained when using the Coleman & Nelson (2016a) gas accretion prescription. Due to the high efficiency of giant formation with f opa = 10 −3 , ∼ 3% of the runs formed systems with two giant planets, similar to the recently reported planetary system, WASP-148 (Hébrard et al 2020).…”

Section: Discussionsupporting

confidence: 78%

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In situ formation of hot Jupiters with companion super-Earths

Poon,

Nelson,

Coleman

2021

Preprint

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Observations have confirmed the existence of multiple-planet systems containing a hot Jupiter and smaller planetary companions. Examples include WASP-47, Kepler-730, and TOI-1130. We examine the plausibility of forming such systems in situ using N-body simulations that include a realistic treatment of collisions, an evolving protoplanetary disc and eccentricity/inclination damping of planetary embryos. Initial conditions are constructed using two different models for the core of the giant planet: a 'seed-model' and an 'equal-mass-model'. The former has a more massive protoplanet placed among multiple small embryos in a compact configuration. The latter consists only of equal-mass embryos. Simulations of the seed-model lead to the formation of systems containing a hot Jupiter and super-Earths. The evolution consistently follows four distinct phases: early giant impacts; runaway gas accretion onto the seed protoplanet; disc damping-dominated evolution of the embryos orbiting exterior to the giant; a late chaotic phase after dispersal of the gas disc. Approximately 1% of the equal-mass simulations form a giant and follow the same four-phase evolution. Synthetic transit observations of the equal-mass simulations provide an occurrence rate of 0.26% for systems containing a hot Jupiter and an inner super-Earth, similar to the 0.2% occurrence rate from actual transit surveys, but simulated hot Jupiters are rarely detected as single transiting planets, in disagreement with observations. A subset of our simulations form two close-in giants, similar to the WASP-148 system. The scenario explored here provides a viable pathway for forming systems with unusual architectures, but does not apply to the majority of hot Jupiters.

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Section: Discussionsupporting

confidence: 78%

“…Recent observations of the WASP-148 system show that it may have two close-in giants (both have mass ∼ 100 M ⊕ ) orbiting and transiting the same star (Hébrard et al 2020). The semimajor axes of the two giants, WASP-148 b and c, are at ∼ 0.08 and 0.21 au respectively.…”

Section: Simulation Outcomesmentioning

confidence: 99%

In situ formation of hot Jupiters with companion super-Earths

Poon,

Nelson,

Coleman

2021

Preprint

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“…Recently, however, a few nearby planetary companions to hot Jupiters have begun to emerge. These companions have become possible to detect through extreme-precision photometric observations from space-based observatories (e.g., WASP-47, Becker et al 2015;Kepler-730 (Zhu et al 2018), Cañas et al 2019;TOI-1130, Huang et al 2020WASP-132, Hord et al 2022;TOI-2000, Sha et al 2022, as well as dedicated radial velocity follow-up measurements of known transiting hot Jupiters (WASP-148, Hébrard et al 2020). These new discoveries provide strong evidence that at least some hot Jupiters have quiescent dynamical histories.…”

Section: Dynamical High-eccentricity Migration In Which Coldmentioning

confidence: 99%

Evidence for Hidden Nearby Companions to Hot Jupiters

Rice

Wang

2023

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The first discovered extrasolar worlds—giant, “hot Jupiter” planets on short-period orbits—came as a surprise to solar system–centric models of planet formation, prompting the development of new theories for planetary system evolution. The near absence of observed nearby planetary companions to hot Jupiters has been widely quoted as evidence in support of high-eccentricity tidal migration, a framework in which hot Jupiters form further out in their natal protoplanetary disks before being thrown inward with extremely high eccentricities, stripping systems of any close-in planetary companions. In this work, we present new results from a search for transit timing variations across the full 4 yr Kepler data set, demonstrating that at least 12% ± 6% of hot Jupiters have a nearby planetary companion. This subset of hot Jupiters is expected to have a quiescent dynamical history such that the systems could retain their nearby companions. We also demonstrate a ubiquity of nearby planetary companions to warm Jupiters (≥70% ± 16%), indicating that warm Jupiters typically form quiescently. We conclude by combining our results with existing observational constraints to propose an “eccentric migration” framework for the formation of short-period giant planets through postdisk dynamical sculpting in compact multiplanet systems. Our framework suggests that hot Jupiters constitute the natural end stage for giant planets spanning a wide range of eccentricities, with orbits that reach small enough periapses—either from their final orbital configurations in the disk phase or from eccentricity excitation in the postdisk phase—to trigger efficient tidal circularization.

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“…The other numbers refer to other works reporting additional measurements of λ or other system parameters. Note-All data were taken from TEPCat (Southworth 2011) or the following references: 1 (Hirano et al 2020a), 2 (Albrecht et al 2021), 3 (Martioli et al 2020), 4 (Palle et al 2020, 5 (Addison et al 2021), 6 (Christiansen et al 2017), 7 (Bourrier et al 2021, (Dalal et al 2019), 9 (Mann et al 2020), 10 (Dai et al 2020), 11 (Zhou et al 2018, 12 (Hjorth et al 2019a), 13 (Hjorth et al 2021, 14 (Wang et al 2018), 15 (Albrecht et al 2013), 16 (Campante et al 2016, 17 (Benomar et al 2014), 18 (Sanchis-Ojeda et al 2012, 19 , 20 (Huber et al 2013), 21 (Hirano et al 2012), 22 (Newton et al 2021, 23 (Zhou et al 2021), 24 (Wirth et al 2021), 25 (Hirano et al 2020b), 26 (David et al 2019b), 27 (Johnson et al 2021), 28 (Biddle et al 2014), 29 (Gaidos et al 2021), 30 (Feinstein et al 2021), 31 (Sanchis-Ojeda et al 2015, 32 (Wang et al 2021b), 33 (Hébrard et al 2020) 3.1.12. Interlude: Mutual orbital inclinations Most of the available RM data are for stars with closeorbiting giant planets.…”

Section: Obliquity and Eccentricitymentioning

confidence: 99%

Stellar obliquities in exoplanetary systems

Albrecht,

Dawson,

Winn

2022

Preprint

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The rotation of a star and the revolutions of its planets are not necessarily aligned. This article reviews the measurement techniques, key findings, and theoretical interpretations related to the obliquities (spin-orbit angles) of planet-hosting stars. The best measurements are for stars with short-period giant planets, which have been found on prograde, polar, and retrograde orbits. It seems likely that dynamical processes such as planet-planet scattering and secular perturbations are responsible for tilting the orbits of close-in giant planets, just as those processes are implicated in exciting orbital eccentricities. The observed dependence of the obliquity on orbital separation, planet mass, and stellar structure suggests that in some cases, tidal dissipation damps a star's obliquity within its main-sequence lifetime. The situation is not as clear for stars with smaller or wider-orbiting planets. Although the earliest measurements of such systems tended to find low obliquities, some glaring exceptions are now known in which the star's rotation is misaligned with respect to the coplanar orbits of multiple planets. In addition, statistical analyses based on projected rotation velocities and photometric variability have found a broad range of obliquities for F-type stars hosting compact multiple-planet systems. The results suggest it is unsafe to assume that stars and their protoplanetary disks are aligned. Primordial misalignments might be produced by neighboring stars or more complex events that occur during the epoch of planet formation.

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Discovery and characterization of the exoplanets WASP-148b and c

Cited by 16 publications

References 86 publications

In situ formation of hot Jupiters with companion super-Earths

In situ formation of hot Jupiters with companion super-Earths

Evidence for Hidden Nearby Companions to Hot Jupiters

Stellar obliquities in exoplanetary systems

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