<i>KEPLER</i>ECLIPSING BINARY STARS. II. 2165 ECLIPSING BINARIES IN THE SECOND DATA RELEASE

Slawson, Robert W.; Prša, Andrej; Welsh, William F.; Orosz, Jerome A.; Rucker, Michael; Batalha, Natalie M.; Doyle, Laurance R.; Engle, Scott G.; Conroy, Kyle E.; Coughlin, Jared; Gregg, Trevor A.; Fetherolf, Tara; Short, Donald R.; Windmiller, Gur; Fabrycky, Daniel C.; Howell, Steve B.; Jenkins, Jon M.; Uddin, Kamal; Mullally, Fergal; Seader, Shawn; Thompson, Susan E.; Sanderfer, Dwight T.; Borucki, W. J.; Koch, David

doi:10.1088/0004-6256/142/5/160

Cited by 403 publications

(253 citation statements)

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“…As part of this exoplanet reconnaissance, 2165 eclipsing binaries are being observed of which 1322 are detached or semi-detached systems 13 We investigate these two subclasses of eclipsing binaries because the eclipse timing technique outlined in Supplementary Section 8 does not work well if the first and fourth contact points (start of ingress and end of egress) are not well defined. We also chose to omit systems with P < 0.9 days, as these in general also suffer from eclipse timing measurement difficulties owing to out-of-eclipse variations due to tidal distortions and reflection effects.…”

Section: The Search For Transiting Circumbinary Planet Candidatesmentioning

confidence: 99%

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Transiting circumbinary planets Kepler-34 b and Kepler-35 b

Welsh

Orosz

Carter

et al. 2012

Nature

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The new planets were identified using 671 days of data from the NASA Kepler spacecraft 10 . As part of its mission 11 to detect Earth-like planets via the transit method, Kepler is monitoring over 2,000 eclipsing binary stars 12,13 . From these we selected a sample of 750 systems with orbital periods ranging from 0.9 to 276 days, and for which eclipses of both stars occur. For each system, we measured the eclipse times and searched for departures from strict periodicity, as would be produced by gravitational perturbations from a third body.All 750 systems were searched by eye for planetary transits, with particular attention to an 18% subset that exhibited significant differences between the periods derived from the deeper primary eclipses, and those from the shallower secondary eclipses (for details see the Supplementary Information, SI). This led to the discovery of Kepler-34 and Kepler-35, and a candidate system KOI-2939. KOI-2939 (Kepler Input Catalog 14 number 05473556) exhibited a single transit at BJD 2,454,996.995 ± 0.010 of duration 2.5 hours and depth 0.18%. The transit duration constrains the size and velocity of the third body and is consistent with a Jovian planet transiting the secondary star, but we cannot verify its planetary nature. We defer discussion for a future investigation.The stars of Kepler-34 have an orbital period of 28 days, with a period difference between primary and secondary eclipses of 4.91 ± 0.59 s. Three transits were detected (Fig 1), with the first and second being transits of the primary star, while the third is of the secondary star. Notably the transit durations are all different, ruling out the most common type of "false positive," a background eclipsing binary. Circumbinary transits naturally vary in duration as a consequence of the changing velocity of the stars. The Kepler photometry were supplemented by spectroscopic observations of the radial-velocity variations of both stars (Fig. 1f), in order to determine the orbital scale and sizes of all three bodies. The photometric and spectroscopic data were fit with a model 9,15 that accounts for the three-body gravitational dynamics and the loss of light due to eclipses and transits (see SI). The model fit confirms that the transiting body is a planet with 22% the mass of Jupiter (69 Earth masses) and 76% the radius of Jupiter (8.6 Earth radii). The primary and secondary stars are similar to the Sun. With the spectra we also measured the effective temperature and abundance of heavy elements (metallicity) of both stars. The observed stellar parameters match the Yonsei-Yale theoretical models of stellar evolution 16 for an age of 5-6 Gyr. The parameters and uncertainties are given in Table 1, with details in the SI.The stars of Kepler-35 have an orbital period of 21 days, with a period difference between primary and secondary eclipses of 1.89 ± 0.48 s. Four transits were detected (Fig. 2 b,c,d,e). The first, second, and fourth events are transits of the primary star, and the weaker third event is a transit of the secondary st...

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Section: The Search For Transiting Circumbinary Planet Candidatesmentioning

confidence: 99%

“…As part of its mission 11 to detect Earth-like planets via the transit method, Kepler is monitoring over 2,000 eclipsing binary stars 12,13 . From these we selected a sample of 750 systems with orbital periods ranging from 0.9 to 276 days, and for which eclipses of both stars occur.…”

mentioning

confidence: 99%

Transiting circumbinary planets Kepler-34 b and Kepler-35 b

Welsh

Orosz

Carter

et al. 2012

Nature

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416

323

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“…We do not know a priori which stars have such dilution. However, the effect on occurrence rates can be quantified via numerical simulation based on multiple star statistics from Kepler (84,85) and other (86) surveys.…”

Section: Requirements For Reliable Planet Occurrence Ratesmentioning

confidence: 99%

Exploring exoplanet populations with NASA’s Kepler Mission

Batalha

2014

Proc. Natl. Acad. Sci. U.S.A.

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The Kepler Mission is exploring the diversity of planets and planetary systems. Its legacy will be a catalog of discoveries sufficient for computing planet occurrence rates as a function of size, orbital period, star type, and insolation flux. The mission has made significant progress toward achieving that goal. Over 3,500 transiting exoplanets have been identified from the analysis of the first 3 y of data, 100 planets of which are in the habitable zone. The catalog has a high reliability rate (85-90% averaged over the period/radius plane), which is improving as follow-up observations continue. Dynamical (e.g., velocimetry and transit timing) and statistical methods have confirmed and characterized hundreds of planets over a large range of sizes and compositions for both single-and multiple-star systems. Population studies suggest that planets abound in our galaxy and that small planets are particularly frequent. Here, I report on the progress Kepler has made measuring the prevalence of exoplanets orbiting within one astronomical unit of their host stars in support of the National Aeronautics and Space Administration's long-term goal of finding habitable environments beyond the solar system. planet detection | transit photometry

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“…Although the transit light curve ( KIC3848972 as a false positive, which may consist of an evolved giant star that is redder and several magnitudes brighter than the eclipsing star. Slawson et al (2011) found an orbital period for this system that is twice as long. Moreover, we found a small difference between the odd and even transits in this system (0.000140) and a weak periodic background variability, which is very similar to an RS Canum Venaticorum-like distortion wave (see e.g.…”

Section: Exoplanet Candidate Kic3848972mentioning

confidence: 71%

Search for circum‐planetary material and orbital period variations of short‐period Kepler exoplanet candidates

et al. 2014

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A unique short-period (P = 0.65356(1) d) Mercury-size Kepler exoplanet candidate KIC012557548b has been discovered recently by Rappaport et al. (2012). This object is a transiting disintegrating exoplanet with a circum-planetary material-comet-like tail. Close-in exoplanets, like KIC012557548b, are subjected to the greatest planet-star interactions. This interaction may have various forms. In certain cases it may cause formation of the comet-like tail. Strong interaction with the host star, and/or presence of an additional planet may lead to variations in the orbital period of the planet. Our main aim is to search for comet-like tails similar to KIC012557548b and for long-term orbital period variations. We are curious about frequency of comet-like tail formation among short-period Kepler exoplanet candidates. We concentrate on a sample of 20 close-in candidates with a period similar to KIC012557548b from the Kepler mission. We first improved the preliminary orbital periods and obtained the transit light curves. Subsequently we searched for the signatures of a circum-planetary material in these light curves. For this purpose the final transit light curve of each planet was fitted with a theoretical light curve, and the residuals were examined for abnormalities. We then searched for possible long-term changes of the orbital periods using the method of phase dispersion minimization. In 8 cases out of 20 we found some interesting peculiarities, but none of the exoplanet candidates showed signs of a comet-like tail. It seems that the frequency of comet-like tail formation among short-period Kepler exoplanet candidates is very low. We searched for comet-like tails based on the period criterion. Based on our results we can conclude that the short-period criterion is not enough to cause comet-like tail formation. This result is in agreement with the theory of the thermal wind and planet evaporation (PerezBecker & Chiang 2013). We also found 3 cases of candidates which showed some changes of the orbital period. Based on our results we can see that orbital period changes are not caused by comet-like tail disintegration processes, but rather by possible massive outer companions.

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KEPLERECLIPSING BINARY STARS. II. 2165 ECLIPSING BINARIES IN THE SECOND DATA RELEASE

Cited by 403 publications

References 22 publications

Transiting circumbinary planets Kepler-34 b and Kepler-35 b

Transiting circumbinary planets Kepler-34 b and Kepler-35 b

Exploring exoplanet populations with NASA’s Kepler Mission

Search for circum‐planetary material and orbital period variations of short‐period Kepler exoplanet candidates

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