Kepler-1647b: The Largest and Longest-Period Kepler Transiting Circumbinary Planet

Kostov, Veselin B.; Orosz, Jerome A.; Welsh, William F.; Doyle, Laurance R.; Fabrycky, Daniel C.; Haghighipour, Nader; Quarles, Billy; Short, Donald R.; Cochran, William D.; Endl, Michael; Ford, Eric B.; Gregorio, J.; Hinse, T. C.; Isaacson, Howard; Jenkins, Jon M.; Jensen, Eric L. N.; Kane, Stephen R.; Kull, Ilya; Latham, David W.; Lissauer, Jack J.; Marcy, Geoffrey W.; Mazeh, T.; Müller, Tobias W. A.; Pepper, Joshua; Quinn, Samuel N.; Ragozzine, Darin; Shporer, Avi; Steffen, Jason H.; Torres, Guillermo; Windmiller, Gur; Borucki, W. J.

doi:10.3847/0004-637x/827/1/86

Cited by 128 publications

(118 citation statements)

References 113 publications

Supporting

Mentioning

111

Contrasting

Order By: Relevance

“…These include planets orbiting a pulsar (Wolszczan & Frail 1992); hot Jupiters (Mayor & Queloz 1995); systems of short-period, low-density planets in tightly packed orbits (Lissauer 2011); and circumbinary planets (Doyle et al 2011) close to the stability limit. Circumbinary planets and planets in close binary systems are very difficult to detect with the radial velocity method, but Kepler has proved quite adept at finding such systems (Doyle et al 2011;Orosz et al 2012;Welsh et al 2012Welsh et al , 2015Kostov et al 2013Kostov et al , 2014Kostov et al , 2016. Gravitational microlensing (Bennett 2008;Gaudi 2012) has demonstrated the ability to detect such systems (Bennett et al 1999;Gould et al 2014;Poleski et al 2014;Udalski et al 2015) (either circumbinary planets or planets orbiting one member of a relatively close binary).…”

Section: Introductionmentioning

confidence: 99%

THE FIRST CIRCUMBINARY PLANET FOUND BY MICROLENSING: OGLE-2007-BLG-349L(AB)c

Bennett¹,

Rhie²,

Udalski³

et al. 2016

Self Cite

106

View full text Add to dashboard Cite

We present the analysis of the first circumbinary planet microlensing event, OGLE-2007-BLG-349. This event has a strong planetary signal that is best fit with a mass ratio of q≈3.4×10 −4 , but there is an additional signal due to an additional lens mass, either another planet or another star. We find acceptable light-curve fits with two classes of models: two-planet models (with a single host star) and circumbinary planet models. The light curve also reveals a significant microlensing parallax effect, which constrains the mass of the lens system to be M L ≈0.7  M . Hubble Space Telescope (HST) images resolve the lens and source stars from their neighbors and indicate excess flux due to the star(s) in the lens system. This is consistent with the predicted flux from the circumbinary models, where the lens mass is shared between two stars, but there is not enough flux to be consistent with the two-planet, one-star models. So, only the circumbinary models are consistent with the HST data. They indicate a planet of mass m c =80±13 Å M , orbiting a pair of M dwarfs with masses of M A =0.41±0.07 and M B =0.30±0.07, which makes this the lowest-mass circumbinary planet system known. The ratio of the separation between the planet and the center of mass to the separation of the two stars is ∼40, so unlike most of the circumbinary planets found by Kepler, the planet does not orbit near the stability limit.

show abstract

Section: Introductionmentioning

confidence: 99%

THE FIRST CIRCUMBINARY PLANET FOUND BY MICROLENSING: OGLE-2007-BLG-349L(AB)c

Bennett¹,

Rhie²,

Udalski³

et al. 2016

Self Cite

106

View full text Add to dashboard Cite

show abstract

“…Borucki & Summers (1984) noted that photometric searches around eclipsing binaries would have enhanced transit probabilities, which was later expanded upon by Schneider & Chevreton (1990) and Schneider (1994). After the unambiguous discovery of the first transiting circumbinary planet Kepler-16 (Doyle et al 2011) the field has flourished, leading to an additional ten transiting discoveries (the latest being Kepler-1647 by Kostov et al 2016) and a wealth of related studies.…”

Section: Introductionmentioning

confidence: 99%

“…Within this year, the original Kepler field is likely to receive roughly one or two months of time coverage. Refs: Doyle et al (2011);Welsh et al (2012Welsh et al ( , 2014; Orosz et al (2012a,b); Schwamb et al (2013); Kostov et al (2013Kostov et al ( , 2014Kostov et al ( , 2016. Note: Updated elements for Kepler-453 and -1647 provided by Veselin Kostov (priv.…”

Section: Predicted Future Transits and Observations With Tess Cheopsmentioning

confidence: 99%

Circumbinary planets – II. When transits come and go

Martin¹

2016

Mon. Not. R. Astron. Soc.

View full text Add to dashboard Cite

Circumbinary planets are generally more likely to transit than equivalent single-star planets, but practically the geometry and orbital dynamics of circumbinary planets make the chance of observing a transit inherently time-dependent. In this follow-up paper to Martin & Triaud (2015), the time-dependence is probed deeper by analytically calculating when and for how long the binary and planet orbits overlap, allowing for transits to occur. The derived equations are applied to the known transiting circumbinary planets found by Kepler to predict when future transits will occur, and whether they will be observable by upcoming space telescopes TESS, CHEOPS and PLATO. The majority of these planets spend less than 50% of their time in a transiting configuration, some less than 20%. From this it is calculated that the known Kepler eclipsing binaries likely host an additional ∼ 17 − 30 circumbinary planets that are similar to the ten published discoveries, and they will ultimately transit some day, potentially during the TESS and PLATO surveys.

show abstract

“…Orosz 2015; Borkovits et al 2015, and references therein), and have recently been used to study CBPs as well. In particular, the former effect has been measured for several of the Kepler CBP systems and used to constrain the respective planetary masses (Doyle et al 2011;Welsh et al 2012;Kostov et al 2016). The latter effect has been suggested as the cause for measured Fig.…”

Section: Discussionmentioning

confidence: 99%

“…Specifically, the CE phase can occur on timescales as short as one year (Paczynski 1976;Passy et al 2012), and during this year a binary can expel ∼ 2M worth of mass (Ricker & Taam 2008, 2012Iaconi et al 2016). Interestingly, such timescales are well within a single orbit of CBPs like Kepler-1647 with P CBP = 3 yrs (Kostov et al 2016). Such a dramatic restructuring will have a profound impact on the dynamics of the system -for example, a CBP can achieve very high eccentricity -and may even result in the ejection of the planet.…”

Section: Introductionmentioning

confidence: 99%

Tatooine’s Future: The Eccentric Response of Kepler’s Circumbinary Planets to Common-Envelope Evolution of Their Host Stars

Kostov

Moore

Tamayo

et al. 2016

ApJ

Self Cite

View full text Add to dashboard Cite

Inspired by the recent Kepler discoveries of circumbinary planets orbiting nine close binary stars, we explore the fate of the former as the latter evolve off the main sequence. We combine binary star evolution models with dynamical simulations to study the orbital evolution of these planets as their hosts undergo common-envelope stages, losing in the process a tremendous amount of mass on dynamical timescales. Five of the systems experience at least one Roche-lobe overflow and common-envelope stages (Kepler-1647 experiences three), and the binary stars either shrink to very short orbits or coalesce; two systems trigger a double-degenerate supernova explosion. Kepler's circumbinary planets predominantly remain gravitationally bound at the end of the common-envelope phase, migrate to larger orbits, and may gain significant eccentricity; their orbital expansion can be more than an order of magnitude and can occur over the course of a single planetary orbit. The orbits these planets can reach are qualitatively consistent with those of the currently known post-commonenvelope, eclipse-time variations circumbinary candidates. Our results also show that circumbinary planets can experience both modes of orbital expansion (adiabatic and -2 -non-adiabatic) if their host binaries undergo more than one common-envelope stage; multiplanet circumbinary systems like Kepler-47 can experience both modes during the same common-envelope stage. Additionally, unlike Mercury orbiting the Sun, a circumbinary planet with the same semi-major axis can survive the common envelope evolution of a close binary star with a total mass of 1 M .

show abstract

Kepler-1647b: The Largest and Longest-Period Kepler Transiting Circumbinary Planet

Cited by 128 publications

References 113 publications

THE FIRST CIRCUMBINARY PLANET FOUND BY MICROLENSING: OGLE-2007-BLG-349L(AB)c

THE FIRST CIRCUMBINARY PLANET FOUND BY MICROLENSING: OGLE-2007-BLG-349L(AB)c

Circumbinary planets – II. When transits come and go

Tatooine’s Future: The Eccentric Response of Kepler’s Circumbinary Planets to Common-Envelope Evolution of Their Host Stars

Contact Info

Product

Resources

About