Discovery of a Third Transiting Planet in the Kepler-47 Circumbinary System

Orosz, Jerome A.; Welsh, William F.; Haghighipour, Nader; Quarles, Billy; Short, Donald R.; Mills, Sean M.; Satyal, Suman; Torres, Guillermo; Agol, Eric; Fabrycky, Daniel C.; Jontof-Hutter, Daniel; Windmiller, Gur; Müller, Tobias W. A.; Hinse, T. C.; Cochran, William D.; Endl, Michael; Ford, Eric B.; Mazeh, T.; Lissauer, Jack J.

doi:10.3847/1538-3881/ab0ca0

Cited by 100 publications

(95 citation statements)

References 143 publications

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“…Most of them (at present 10) were discovered by Kepler with the transit method while the more massive ones (2.3M J < m < 10M J ) were found either by eclipsing binary timing [64] around evolved stars or direct imaging. The most interesting among transiting circumbinary planets is Kepler-47, the only multi-planet system that has 3 exoplanets with masses ranging from 2 to about 43 Earth masses moving in almost circular orbits, coplanar to the binary orbital plane, stable at least over 100 Myr and with the inner and less massive planet right next to the dynamical stability limit [65]. Almost all Kepler circumbinary planets found so far orbit their stars very close to the plane of the binary in a prograde direction.…”

Section: Planets In P-type Orbits: Circumbinary Planetsmentioning

confidence: 99%

Planets in Binaries: Formation and Dynamical Evolution

Marzari

Thébault

2019

Galaxies

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Binary systems are very common among field stars, yet the vast majority of known exoplanets have been detected around single stars. While this relatively small number of planets in binaries is probably partly due to strong observational biases, there is, however, statistical evidence that planets are indeed less frequent in binaries with separations smaller than 100 au, strongly suggesting that the presence of a close-in companion star has an adverse effect on planet formation. It is indeed possible for the gravitational pull of the second star to affect all the different stages of planet formation, from proto-planetary disk formation to dust accumulation into planetesimals, to the accretion of these planetesimals into large planetary embryos and, eventually, the final growth of these embryos into planets. For the crucial planetesimal-accretion phase, the complex coupling between dynamical perturbations from the binary and friction due to gas in the proto-planetary disk suggests that planetesimal accretion might be hampered due to increased, accretion-hostile impact velocities. Likewise, the interplay between the binary's secular perturbations and mean motion resonances lead to unstable regions, where not only planet formation is inhibited, but where a massive body would be ejected from the system on a hyperbolic orbit. The amplitude of these two main effects is different for S-and P-type planets, so that a comparison between the two populations might outline the influence of the companion star on the planet formation process. Unfortunately, at present the two populations (circumstellar or circumbinary) are not known equally well and different biases and uncertainties prevent a quantitative comparison. We also highlight the long-term dynamical evolution of both S and P-type systems and focus on how these different evolutions influence the final architecture of planetary systems in binaries.We will focus here on the main characteristics of planets in both S and P-type orbital configurations which significantly differ in terms of perturbations by the companion star. In the S-type configuration, where planets orbit one of the star of the system, the most critical regions for planet formation are the outer ones where the gravity of the second star may excite large eccentricities, potentially leading to instability via resonance superposition and, in case of orbital misalignment, may also be involved in fast Kozai cycles with large eccentricity/inclination variations. The inner regions of the circumstellar disk appears then most promising for a 'regular' core-accretion growth of planets and for subsequent stable orbital behavior. In the case of P-type configurations, where the planets orbit around both stars, perturbations are the strongest in the inner regions close to the central binary. In this configuration, instability is expected close to the center of the system, while planet formation should safely occur in the outer regions of the circumbinary disk. In this case, planet migration may play a major role in brin...

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Section: Planets In P-type Orbits: Circumbinary Planetsmentioning

confidence: 99%

Planets in Binaries: Formation and Dynamical Evolution

Marzari

Thébault

2019

Galaxies

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“…By now about a dozen planets orbiting around binary star systems have been detected by the Kepler space mission. All of these are single-planet systems, except Kepler-47 whose third planet was recently detected (Orosz et al 2019), demonstrating that circumbinary systems can host multiple planets. This raises the question about their formation, evolution and stability.…”

Section: Introductionmentioning

confidence: 98%

1:1 orbital resonance of circumbinary planets

Penzlin

Ataiee

Kley

2019

A&A

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The recent detection of the third planet in Kepler-47 has shown that binary stars can host several planets in circumbinary orbits. To understand the evolution of such systems we have performed two-dimensional hydrodynamic simulations of the circumbinary disc with two embedded planets for several Kepler systems. In two cases, Kepler-47 and -413, the planets are captured in a 1:1 mean-motion resonance at the planet parking position near the inner edge of the disc. The orbits are fully aligned, have mean eccentricities of about 0.25 to 0.30, and the planets are entangled in a horseshoe type of motion. Subsequent n-body simulations without the disc show that the configurations are stable. Our results point to the existence of a new class of stable resonant orbits around binary stars. It remains to be seen if such orbits exist in reality.

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“…With their extremely low densities, the Kepler 51 planets join the ranks of a rare class of exoplanets known as superpuffs (Lee & Chiang 2016). Super-puffs, including Kepler 47c (Orosz et al 2019), Kepler 79d (Jontof-Hutter et al 2014), and Kepler 87c (Ofir et al 2014), are cooler and less massive than the inflated low-density hot-Jupiters. The thermal evolution models of Rogers et al (2011), Lopez et al (2012), and Batygin & Stevenson (2013) can reproduce such low-density exoplanets with large mass fractions of hydrogen and helium, but the process of forming low-mass, H/He-rich planets continues to present an interesting challenge.…”

Section: Introductionmentioning

confidence: 99%

The Featureless Transmission Spectra of Two Super-puff Planets

Libby-Roberts

Berta-Thompson

Désert

et al. 2020

Self Cite

102

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The Kepler mission revealed a class of planets known as "super-puffs," with masses only a few times larger than Earth's but radii larger than Neptune, giving them very low mean densities. All three of the known planets orbiting the young solar-type star Kepler 51 are super-puffs. The Kepler 51 system thereby provides an opportunity for a comparative study of the structures and atmospheres of this mysterious class of planets, which may provide clues about their formation and evolution. We observed two transits each of Kepler 51b and 51d with the Wide Field Camera 3 (WFC3) on the Hubble Space Telescope. Combining new WFC3 transit times with re-analyzed Kepler data and updated stellar parameters, we confirmed that all three planets have densities lower than 0.1 g/cm 3 . We measured the WFC3 transmission spectra to be featureless between 1.15 and 1.63 µm, ruling out any variations greater than 0.6 scale heights (assuming a H/He dominated atmosphere), thus showing no significant water absorption features. We interpreted the flat spectra as the result of a high-altitude aerosol layer (pressure <3 mbar) on each planet. Adding this new result to the collection of flat spectra that have been observed for other sub-Neptune planets, we find support for one of the two hypotheses introduced by Crossfield & Kreidberg (2017), that planets with cooler equilibrium temperatures have more high-altitude aerosols. We strongly disfavor their other hypothesis that the H/He mass fraction drives the appearance of large amplitude transmission features.

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Discovery of a Third Transiting Planet in the Kepler-47 Circumbinary System

Cited by 100 publications

References 143 publications

Planets in Binaries: Formation and Dynamical Evolution

Planets in Binaries: Formation and Dynamical Evolution

1:1 orbital resonance of circumbinary planets

The Featureless Transmission Spectra of Two Super-puff Planets

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