Kepler-16: A Transiting Circumbinary Planet

Doyle, Laurance R.; Carter, Joshua A.; Fabrycky, Daniel C.; Slawson, Robert W.; Howell, Steve B.; Winn, Joshua N.; Orosz, Jerome A.; Prˇsa, Andrej; Welsh, William F.; Quinn, Samuel N.; Latham, David W.; Torres, Guillermo; Buchhave, Lars A.; Marcy, Geoffrey W.; Fortney, Jonathan J.; Shporer, Avi; Ford, Eric B.; Lissauer, Jack J.; Ragozzine, Darin; Rucker, Michael; Batalha, Natalie M.; Jenkins, Jon M.; Borucki, W. J.; Koch, David; Middour, Christopher K.; Hall, Jennifer R.; McCauliff, Sean; Fanelli, M. N.; Quintana, Elisa V.; Holman, Matthew J.; Caldwell, Douglas A.; Still, M.; Stefanik, R. P.; Brown, Warren R.; Esquerdo, Gilbert A.; Tang, Sumin; Fürész, Gábor; Geary, John C.; Berlind, P.; Calkins, M.; Short, Donald R.; Steffen, Jason H.; Sasselov, Dimitar; Dunham, E. W.; Cochran, William D.; Boss, Alan P.; Haas, Michael R.; Buzasi, Derek L.; Fischer, Debra A.

doi:10.1126/science.1210923

Cited by 675 publications

(561 citation statements)

References 33 publications

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“…For instance, the unevolved dG/dM binary Kepler 47 harbors two planets orbiting the system with semi-major axes of less than 1 AU . The binary star system Kepler 16 hosts the Saturn-sized planet Kepler 16b with a semi-major axis of 3.9 AU (Doyle et al 2011), and Kepler 34/35 hosts a planet with one fifth of Jupiter's mass at a semi-major axis of 1 AU on a somewhat eccentric orbit . For the PCEB system NN Ser, Beuermann et al (2010Beuermann et al ( , 2013 employed the light-travel time (LLT) effect to detect two planets with masses of 7.0 M J and 1.7 M J with a semi-major axis of 5.4 AU and 3.47 AU, respectively.…”

Section: Introductionmentioning

confidence: 99%

Planet formation from the ejecta of common envelopes

Schleicher

Dreizler

2014

A&A

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Context. The close binary system NN Serpentis must have gone through a common envelope phase before the formation of its white dwarf. During this phase, a substantial amount of mass was lost from the envelope. The recently detected orbits of circumbinary planets are probably inconsistent with planet formation before the mass loss. Aims. We explore whether new planets may have formed from the ejecta of the common envelope and derive the expected planetary mass as a function of radius. Methods. We employed the Kashi & Soker model to estimate the amount of mass that is retained during the ejection event and inferred the properties of the resulting disk from the conservation of mass and angular momentum. The resulting planetary masses were estimated from models with and without radiative feedback. Results. We show that the observed planetary masses can be reproduced for appropriate model parameters. Photoheating can stabilize the disks in the interior, potentially explaining the observed planetary orbits on scales of a few AU. We compare the expected mass scale of planets for 11 additional systems with observational results and find hints of two populations, one consistent with planet formation from the ejecta of common envelopes and the other a separate population that may have formed earlier.Conclusions. The formation of the observed planets from the ejecta of common envelopes seems feasible. The model proposed here can be tested through refined observations of additional post-common envelope systems. While it appears observationally challenging to distinguish between the accretion on pre-existing planets and their growth from new fragments, it may be possible to further constrain the properties of the protoplanetary disk through additional observations of current planetary candidates and post-common envelope binary systems.

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Section: Introductionmentioning

confidence: 99%

Planet formation from the ejecta of common envelopes

Schleicher

Dreizler

2014

A&A

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“…Given the context of a mission designed to measure the number of habitable planets in the galaxy and the alien nature of many of the systems that Kepler has found (e.g., circumbinary planets (Doyle et al 2011;Welsh et al 2012), planetary systems orbiting each component of a binary pair, such as Kepler-132 (Lissauer et al 2014), systems with planets near chains of MMRs such as Kepler-80 (Xie 2013) and Kepler-223 (Lissauer et al 2011), and systems with pairs of planets in strongly interacting orbits (and for the case of Kepler-36, manifestly chaotic orbits; Deck et al 2012), it is not much of a stretch to consider systems with multiple planets that orbit in the habitable zone of their host stars, including pairs in or near MMR.…”

Section: Introductionmentioning

confidence: 99%

Dynamical Considerations for Life in Multi-Habitable Planetary Systems

Steffen

2016

ApJ

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Inspired by the close-proximity pair of planets in the Kepler-36 system, we consider two effects that may have important ramifications for the development of life in similar systems where a pair of planets may reside entirely in the habitable zone of the hosting star. Specifically, we run numerical simulations to determine whether strong, resonant (or non-resonant) planet-planet interactions can cause large variations in planet obliquity-thereby inducing large variations in climate. We also determine whether or not resonant interactions affect the rate of lithopanspermia between the planet pair-which could facilitate the growth and maintenance of life on both planets. We find that first-order resonances do not cause larger obliquity variations when compared with nonresonant cases. We also find that these resonant interactions are not a primary consideration in lithopanspermia. Lithopanspermia is enhanced significantly as the planet orbits come closer together-reaching nearly the same rate as ejected material falling back to the surface of the originating planet (assuming that the ejected material makes it out to the location of our initial conditions). Thus, in both cases our results indicate that close-proximity planet pairs in multi-habitable systems are conducive to life in the system.

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“…To showcase the principles of circumbinary planet detection with astrometry, we discuss the Kepler-16 system (Doyle et al 2011). It consists of a 41.1-day binary with component masses of M1 = 0.6897 M and M2 = 0.2026 M , orbited by a planet with mass Mp = 0.333 MJ in a 228.8-day orbit.…”

Section: Example 1: Kepler-16mentioning

confidence: 99%

“…Beuermann et al 2010;Marsh et al 2013), like Kepler-16 detected from transits by the Kepler spacecraft (e.g. Doyle et al 2011), like Ross 458, a planetary-mass object directly imaged around an M-dwarf binary (Burgasser et al 2010), and like PSR B1620−26, a pulsar+white-dwarf binary that hosts a Jupiter-mass planet (Thorsett et al 1999;Sigurdsson et al 2008).…”

Section: Introductionmentioning

confidence: 99%

Gaia's potential for the discovery of circumbinary planets

Sahlmann

Triaud

Martin

2014

Monthly Notices of the Royal Astronomical Society

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The abundance and properties of planets orbiting binary stars -circumbinary planets -are largely unknown because they are difficult to detect with currently available techniques. Results from the Kepler satellite and other studies indicate a minimum occurrence rate of circumbinary giant planets of ∼10 %, yet only a handful are presently known. Here, we study the potential of ESA's Gaia mission to discover and characterise extrasolar planets orbiting nearby binary stars by detecting the binary's periodic astrometric motion caused by the orbiting planet. We expect that Gaia will discover hundreds of giant planets around binaries with FGK dwarf primaries within 200 pc of the Sun, if we assume that the giant planet mass distribution and abundance are similar around binaries and single stars. If on the other hand all circumbinary gas giants have masses lower than two Jupiter masses, we expect only four detections. Gaia is critically sensitive to the properties of giant circumbinary planets and will therefore make the detailed study of their population possible. Gaia's precision is such that the distribution in mutual inclination between the binary and planetary orbital planes will be obtained. It also possesses the capacity to establish the frequency of planets across the H-R diagram, both as a function of mass and of stellar evolutionary state from pre-main sequence to stellar remnants. Gaia's discoveries can reveal whether a second epoch of planetary formation occurs after the red-giant phase.

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Kepler-16: A Transiting Circumbinary Planet

Cited by 675 publications

References 33 publications

Planet formation from the ejecta of common envelopes

Planet formation from the ejecta of common envelopes

Dynamical Considerations for Life in Multi-Habitable Planetary Systems

Gaia's potential for the discovery of circumbinary planets

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