THE NEPTUNE-SIZED CIRCUMBINARY PLANET KEPLER-38b

Orosz, Jerome A.; Welsh, William F.; Carter, Joshua A.; Brugamyer, Erik; Buchhave, Lars A.; Cochran, William D.; Endl, Michael; Ford, Eric B.; MacQueen, Phillip J.; Short, Donald R.; Torres, Guillermo; Windmiller, Gur; Agol, Eric; Barclay, Thomas; Caldwell, Douglas A.; Clarke, Bruce; Doyle, Laurance R.; Fabrycky, Daniel C.; Geary, John C.; Haghighipour, Nader; Holman, Matthew J.; Ibrahim, Khadeejah A.; Jenkins, Jon M.; Kinemuchi, Karen; Li, Jie; Lissauer, Jack J.; Prša, Andrej; Ragozzine, Darin; Shporer, Avi; Still, M.; Wade, Richard A.

doi:10.1088/0004-637x/758/2/87

Cited by 228 publications

(103 citation statements)

References 50 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The first was Kepler 16b (Doyle et al 2011). Following this were the discoveries of Kepler 34b and 35b (Welsh et al 2012), Kepler 47b and 47c (Orosz et al 2012a), Kepler 38b (Orosz et al 2012b), Kepler 64b (Schwamb et al 2013;Kostov et al 2013), Kepler 413b (Kostov et al 2014), Kepler 453b , and KOI 2939b (Kostov et al 2015). With the exception of the most recent planet, which is Jupiter-sized, all are between approximately 0.75 -2.25 R N .…”

Section: Introductionmentioning

confidence: 99%

Examining Tatooine: Atmospheric Models of Neptune-Like Circumbinary Planets

May

Rauscher

2016

ApJ

View full text Add to dashboard Cite

Circumbinary planets experience a time varying irradiation pattern as they orbit their two host stars. In this work, we present the first detailed study of the atmospheric effects of this irradiation pattern on known and hypothetical gaseous circumbinary planets. Using both a one-dimensional Energy Balance Model and a three-dimensional General Circulation Model, we look at the temperature differences between circumbinary planets and their equivalent single-star cases in order to determine the nature of the atmospheres of these planets. We find that for circumbinary planets on stable orbits around their host stars, temperature differences are on average no more than 1.0% in the most extreme cases. Based on detailed modeling with the General Circulation Model, we find that these temperature differences are not large enough to excite circulation differences between the two cases. We conclude that gaseous circumbinary planets can be treated as their equivalent single-star case in future atmospheric modeling efforts.

show abstract

Section: Introductionmentioning

confidence: 99%

Examining Tatooine: Atmospheric Models of Neptune-Like Circumbinary Planets

May

Rauscher

2016

ApJ

View full text Add to dashboard Cite

show abstract

“…The binary and planet parameters for these three systems are summarised in Table 1. More recent detections include the Neptune-sized circumbinary planet Kepler-38b (Orosz et al 2012a), a system of 2 planets around Kepler-47 (Orosz et al 2012b), and a transiting circumbinary planet around KIC 4862625 (Schwamb et al 2013).…”

Section: Introductionmentioning

confidence: 99%

Migration and gas accretion scenarios for the Kepler 16, 34, and 35 circumbinary planets

Pierens

Nelson

2013

A&A

119

View full text Add to dashboard Cite

Context. Several circumbinary planets have been detected by the Kepler mission. Recent work has emphasized the difficulty of forming these planets at their observed locations due to perturbations by the binary. It has been suggested that these planets formed further out in their discs in more quiescent environments and migrated in to locations where they are observed. Aims. We examine the orbital evolution of planets embedded in circumbinary disc models for the three systems . The aims are: to explore the plausibility of a formation scenario in which cores form at large distances from the binaries and undergo inward migration and gas accretion as the gas disc disperses; to determine which sets of disc parameters lead to planets whose final orbits provide reasonable fits to the observed systems. Methods. Using a grid-based hydrodynamics code we performed simulations of a close binary system interacting with circumbinary discs with differing aspect ratios, h, and viscous stress parameters α. Once the binary+disc system reaches quasi-equilibrium we embed a planet in the disc and examine its evolution under the action of binary and disc forces. We consider fully-formed planets with masses equal to those inferred from Kepler data, and low-mass cores that migrate and accrete gas while the gas disc is being dispersed. Results. A typical outcome for all systems is stalling of inward migration as the planet enters the tidally-truncated inner cavity formed by the binary system. The circumbinary disc becomes eccentric through interaction with the binary, and the disc eccentricity forces the planet into a non-circular orbit. For each of the Kepler-16b, Kepler-34b and Kepler-35b systems we obtain planets whose parameters agree reasonably well with the observational data, but none of our simulations are able to produce highly accurate fits for all orbital parameters. Conclusions. The final orbital configuration of a circumbinary planet is determined by a delicate interplay between the detailed stucture of the circumbinary disc and the orbital parameters of the planet as it migrates into the inner disc cavity. Simplified simulations such as those presented here provide support for a formation scenario in which a core forms, migrates inward and accretes gas, but accurate fitting of the observed Kepler systems is likely to require disc models that are significantly more sophisticated in terms of their input physics.

show abstract

“…(A color version of this figure is available in the online journal.) Orosz et al (2012bOrosz et al ( , 2012a, Schwamb et al (2013), and Kostov et al (2014), respectively. b Q ttA and Q ttB is calculated via Equation (3), z = e P (t) sin ω P (t).…”

Section: The Seven Current Circumbinary Systemsmentioning

confidence: 99%

Transits of Planets With Small Intervals in Circumbinary Systems

Liu

Wang

Zhang

et al. 2014

ApJ

View full text Add to dashboard Cite

Transit times around single stars can be described well by a linear ephemeris. However, transit times in circumbinary systems are influenced both by the gravitational perturbations and the orbital phase variations of the central binary star. Adopting a coplanar analog of Kepler-16 as an example, we find that circumbinary planets can transit the same star more than once during a single planetary orbit, a phenomenon we call "tight transits." In certain geometric architecture, the projected orbital velocity of the planet and the secondary star can approach zero and change sign, resulting in very long transits and/or 2-3 transits during a single binary orbit. Whether tight transits are possible for a particular system depends primarily on the binary mass ratio and the orbital architecture of both the binary and the planet. We derive a time-dependent criterion to judge when tight transits are possible for any circumbinary system. These results are verified with full dynamical integrations that also reveal other tight transit characteristics, i.e., the transit durations and the intervals between tight transits. For the seven currently known circumbinary systems, we estimate these critical parameters both analytically and numerically. Due to the mutual inclination between the planet and the binary, tight transits can only occur across the less massive star B in . The long-term average frequency of tight transits (compared to typical transits) for are estimated to be several percent. Using full numerical integrations, the next tight transit for each system is predicted and the soonest example appears to be Kepler-47b and -47c, which are likely to have tight transits before 2025. These unique and valuable events often deserve special observational scrutiny.

show abstract

THE NEPTUNE-SIZED CIRCUMBINARY PLANET KEPLER-38b

Cited by 228 publications

References 50 publications

Examining Tatooine: Atmospheric Models of Neptune-Like Circumbinary Planets

Examining Tatooine: Atmospheric Models of Neptune-Like Circumbinary Planets

Migration and gas accretion scenarios for the Kepler 16, 34, and 35 circumbinary planets

Transits of Planets With Small Intervals in Circumbinary Systems

Contact Info

Product

Resources

About