Interaction of a Giant Planet in an Inclined Orbit With a Circumstellar Disk

Marzari, F.; Nelson, Andrew F.

doi:10.1088/0004-637x/705/2/1575

Cited by 54 publications

(63 citation statements)

References 35 publications

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“…Fabrycky & Tremaine 2007), whereas near-circular and near-aligned orbits may be expected if they underwent planet-disc migration (e.g. Marzari & Nelson 2009). We placed an upper limit of e < 0.04 at 2 σ for WASP-105b, but the constraint is much weaker for WASP-107b (e < 0.4 at 2 σ) due to the lower mass of the planet and therefore the smaller amplitude of the stellar reflex motion.…”

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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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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“…This allows us to model more accurately close stellar flybys where the two disks closely interact. In addition, we can also explore the excitation of the planet inclination and its subsequent damping due to the interaction with the disk (Marzari & Nelson 2009;Bitsch & Kley 2011;Cresswell et al 2007). We concentrate in this paper on the effects of a single deep close stellar encounter on a planet still embedded in its birth disk.…”

Section: Introductionmentioning

confidence: 99%

Effects of stellar flybys on planetary systems: 3D modeling of the circumstellar disk’s damping effects

Picogna¹,

Marzari²

2014

A&A

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Context. Stellar flybys in star clusters are suspected of affecting the orbital architecture of planetary systems causing eccentricity excitation and orbital misalignment between the planet orbit and the equatorial plane of the star. Aims. We explore whether the impulsive changes in the orbital elements of planets, caused by a hyperbolic stellar flyby, can be fully damped by the circumstellar disk surrounding the star. The time required to disperse stellar clusters is comparable to the circumstellar disk's lifetime. Since we perform 3D simulations, we can also test the inclination, excitation, and damping. Methods. We have modeled in 3D with the SPH code VINE, a system made of a solar-type star surrounded by a low density disk with a giant planet embedded in it approached on a hyperbolic encounter trajectory by a second star of similar mass and with its own disk. Different inclinations between the disks, planet orbit, and star trajectory have been considered to explore various encounter geometries. We focus on an extreme configuration where a very deep stellar flyby perturbs a Jovian planet on an external orbit. This allows us to test in full the ability of the disk to erase the effects of the stellar encounter. Results. We find that the amount of mass lost by the disk during the stellar flyby is less than in 2D models where a single disk was considered. This is mostly related to the mass exchange between the two disks at the encounter. The damping in eccentricity is slightly faster than in 2D models and it occurs on timescales on the order of a few kyr. During the flyby both the disks are warped owing to the mutual interaction and to the stellar gravitational perturbations, but they quickly relax to a new orbital plane. The planet is quickly dragged back within the disk by the tidal interaction with the gas. The only trace of the flyby left in the planet system, after about 10 4 yr, is a small misalignment, lower than 9 • , between the star equatorial plane and the planet orbit. Conclusions. In a realistic model based on 3D simulations of star-planet-disk interactions, we find that stellar flybys cannot excite significant eccentricities and inclinations of planets in stellar clusters. The circumstellar disks hosting the planets damp on a short timescale all the step changes in the two orbital parameters produced during any stellar encounter. All records of past encounters are erased.

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“…Planets misaligned with the gaseous disk may both affect the disk through warping, and could be affected by it (Marzari & Nelson 2009). Small relative inclinations are likely to be damped through the planets interactions with the disk, re-aligning the planets (Cresswell et al 2007).…”

Section: First Generation Planets In Second Generation Disksmentioning

confidence: 99%

Planets in Evolved Binary Systems

Perets

2011

AIP Conference Proceedings

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Exoplanets are typically thought to form in protoplanetary disks left over from protostellar disk of their newly formed host star. However, additional planetary formation and evolution routes may exist in old evolved binary systems. Here we discuss the implications of binary stellar evolution on planetary systems in such environments. In these binary systems stellar evolution could lead to the formation of symbiotic stars, where mass is lost from one star and could be transferred to its binary companion, and may form an accretion disk around it. This raises the possibility that such a disk could provide the necessary environment for the formation of a new, second generation of planets in both circumstellar or circumbinary configurations. Pre-existing first generation planets surviving the post-MS evolution of such systems would be dynamically effected by the mass loss in the systems and may also interact with the newly formed disk. Such planets and/or planetesimals may also serve as seeds for the formation of the second generation planets, and/or interact with them, possibly forming atypical planetary systems. Second generation planetary systems should be typically found in white dwarf binary systems, and may show various observational signatures. Most notably, second generation planets could form in environment which are inaccessible, or less favorable, for first generation planets. The orbital phase space available for the second generation planets could be forbidden (in terms of the system stability) to first generation planets in the pre-evolved progenitor binaries. In addition planets could form in metal poor environments such as globular clusters and/or in double compact object binaries. Observations of exo-planets in such forbidden or unfavorable regions could possibly serve to uniquely identify their second generation character. Finally, we point out a few observed candidate second generation planetary systems, including Gl 86, HD 27442 and all of the currently observed circumbinary planet candidates. A second generation origin for these systems could naturally explain their unique configurations.

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Interaction of a Giant Planet in an Inclined Orbit With a Circumstellar Disk

Cited by 54 publications

References 35 publications

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 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

Effects of stellar flybys on planetary systems: 3D modeling of the circumstellar disk’s damping effects

Planets in Evolved Binary Systems

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