Planet Hunters: A Transiting Circumbinary Planet in a Quadruple Star System

Schwamb, Megan E.; Orosz, Jerome A.; Carter, Joshua A.; Welsh, William F.; Fischer, Debra A.; Torres, Guillermo; Howard, Andrew W.; Crepp, Justin R.; Keel, William C.; Lintott, Chris; Kaib, Nathan A.; Terrell, Dirk; Gagliano, R.; Jek, Kian J.; Parrish, Michael; Smith, Arfon M.; Lynn, Stuart; Simpson, Robert J.; Giguere, Matthew J.; Schawinski, Kevin

doi:10.1088/0004-637x/768/2/127

Cited by 241 publications

(196 citation statements)

References 75 publications

Supporting

Mentioning

189

Contrasting

Unclassified

Order By: Relevance

“…4 or 5 in a quantitative way. There are only two planets in this mass range observed so far, PH1-Kepler-64b (Schwamb et al 2013) and HAT-P-44c (Hartman et al 2014), that have a separation of more than 0.5 AU. The first one is a circumbinary planet in a four-star system, and we do not know the radius of the second planet.…”

Section: Discussionmentioning

confidence: 90%

Mass of WASP-33b

Lehmann

Guenther

Sebastian

et al. 2015

A&A

View full text Add to dashboard Cite

We analysed an extended time series of high-resolution spectra of the δ Sct star WASP-33 with the aim to determine the effect of its planet WASP-33b. We found ten frequencies in the measured radial velocities. Three of them we can attribute to previously observed photometric oscillations due to non-radial pulsations. One frequency exactly agrees with the orbital period of the planet. The semiamplitude of the corresponding variation is 304 ± 20 m s −1 . This finding allows us to give a new estimate of the mass of WASP-33b of 2.1 ± 0.2 Jupiter masses. Its mean density probably is at least 0.6 g cm −3 , a value that can be expected for a planet of its mass that orbits an A-type star in 1.22 d.

show abstract

Section: Discussionmentioning

confidence: 90%

Mass of WASP-33b

Lehmann

Guenther

Sebastian

et al. 2015

A&A

View full text Add to dashboard Cite

show abstract

“…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

“…References. Doyle et al (2011);Welsh et al (2012); Orosz et al (2012a,b); Schwamb et al (2013); Kostov et al (2014).…”

Section: Numerical Simulationsmentioning

confidence: 98%

Effects of X-ray and extreme UV radiation on circumbinary planets

Sanz-Forcada

Desidera

Micela

2014

A&A

View full text Add to dashboard Cite

Context. Several circumbinary planets have recently been discovered. The orbit of a planet around a binary stellar system poses several dynamic constraints. In addition to these constraints, the effects that radiation from the host stars may have on the planet atmospheres must be considered. We here evaluate these effects. Because of the configuration of a close binary system, these stars have a high rotation rate, even for old stars. The fast rotation of close, tidally locked binaries causes a permanent state of high stellar activity and copious XUV radiation. The accumulated effects are stronger than for normal exoplanets around single stars and cause a faster evaporation of their atmospheres. Aims. We evaluate the effects that stellar radiation has on the evaporation of exoplanets around binary systems and on the survival of these planets. Methods. We considered the X-ray and EUV spectral ranges (XUV, 1-912 Å) to account for the photons that are easily absorbed by a planet atmosphere that is mainly composed of hydrogen. A more complex atmospheric composition is expected to absorb this radiation more efficiently. We used direct X-ray observations to evaluate the energy in the X-rays range and coronal models to calculate the (nondetectable) EUV part of the spectrum. Results. We considered in this problem different configurations of stellar masses, and a resonance of 4:1 and 3:1. The simulations show that exoplanets orbiting close binary systems in a close orbit will suffer strong photoevaporation that may cause a total loss of atmosphere in a short time. We also applied our models to the best real example, Kepler-47 b, to estimate the current mass-loss rates in circumbinary planets and the accumulated effects over the time. Conclusions. A binary system of two solar-like stars will be highly efficient in evaporating the atmosphere of the planet (less than 6 Gyr in our case). These systems will be difficult to find, even if they are dynamically stable. Still, planets may orbit around binary systems of low mass stars for wider orbits. Currently known circumbinary planets are not substantially affected by thermal photoevaporation processes, unless Kepler-47 b has an inflated atmosphere. The distribution of the orbital periods of circumbinary planets is shifted to much longer periods than the average of Kepler planets, which supports a scenario of strong photoevaporation in close-in circumbinary planets.

show abstract

Planet Hunters: A Transiting Circumbinary Planet in a Quadruple Star System

Cited by 241 publications

References 75 publications

Mass of WASP-33b

Mass of WASP-33b

Circumbinary planets – II. When transits come and go

Effects of X-ray and extreme UV radiation on circumbinary planets

Contact Info

Product

Resources

About