Kepler-413B

A slightly misaligned, neptune-size transiting circumbinary planet

V. B. Kostov, P. R. McCullough, J. A. Carter, M. Deleuil, R. F. Díaz, D. C. Fabrycky, G. Hébrard, T. C. Hinse, T. Mazeh, J. A. Orosz, Zlatan Tsvetanov, W. F. Welsh

Research output: Contribution to journalArticle

83 Citations (Scopus)

Abstract

We report the discovery of a transiting, Rp = 4.347 ± 0.099R , circumbinary planet (CBP) orbiting the Kepler K+M eclipsing binary (EB) system KIC 12351927 (Kepler-413) every ∼66 days on an eccentric orbit with ap = 0.355 ± 0.002 AU, ep = 0.118 ± 0.002. The two stars, with MA = 0.820 ± 0.015 M, RA = 0.776 ± 0.009 R and MB = 0.542 ± 0.008 M, R B = 0.484 ± 0.024 R, respectively, revolve around each other every 10.11615 ± 0.00001 days on a nearly circular (e EB = 0.037 ± 0.002) orbit. The orbital plane of the EB is slightly inclined to the line of sight (i EB = 87.°33 ± 0.°06), while that of the planet is inclined by ∼2.°5 to the binary plane at the reference epoch. Orbital precession with a period of ∼11 yr causes the inclination of the latter to the sky plane to continuously change. As a result, the planet often fails to transit the primary star at inferior conjunction, causing stretches of hundreds of days with no transits (corresponding to multiple planetary orbital periods). We predict that the next transit will not occur until 2020. The orbital configuration of the system places the planet slightly closer to its host stars than the inner edge of the extended habitable zone. Additionally, the orbital configuration of the system is such that the CBP may experience Cassini State dynamics under the influence of the EB, in which the planet's obliquity precesses with a rate comparable to its orbital precession. Depending on the angular precession frequency of the CBP, it could potentially undergo obliquity fluctuations of dozens of degrees (and complex seasonal cycles) on precession timescales.

Original languageEnglish
Article number14
JournalAstrophysical Journal
Volume784
Issue number1
DOIs
Publication statusPublished - 20 Mar 2014
Externally publishedYes

Fingerprint

Neptune (planet)
Neptune
planets
planet
precession
orbitals
transit
obliquity
stars
eccentric orbits
conjunction
configurations
line of sight
inclination
sky
time measurement
timescale
orbits
cycles
causes

Keywords

  • binaries: eclipsing
  • planetary systems
  • stars: individual (KIC 12351927, Kepler-413)
  • techniques: photometric

ASJC Scopus subject areas

  • Nuclear and High Energy Physics
  • Space and Planetary Science
  • Astronomy and Astrophysics

Cite this

Kostov, V. B., McCullough, P. R., Carter, J. A., Deleuil, M., Díaz, R. F., Fabrycky, D. C., ... Welsh, W. F. (2014). Kepler-413B: A slightly misaligned, neptune-size transiting circumbinary planet. Astrophysical Journal, 784(1), [14]. https://doi.org/10.1088/0004-637X/784/1/14

Kepler-413B : A slightly misaligned, neptune-size transiting circumbinary planet. / Kostov, V. B.; McCullough, P. R.; Carter, J. A.; Deleuil, M.; Díaz, R. F.; Fabrycky, D. C.; Hébrard, G.; Hinse, T. C.; Mazeh, T.; Orosz, J. A.; Tsvetanov, Zlatan; Welsh, W. F.

In: Astrophysical Journal, Vol. 784, No. 1, 14, 20.03.2014.

Research output: Contribution to journalArticle

Kostov, VB, McCullough, PR, Carter, JA, Deleuil, M, Díaz, RF, Fabrycky, DC, Hébrard, G, Hinse, TC, Mazeh, T, Orosz, JA, Tsvetanov, Z & Welsh, WF 2014, 'Kepler-413B: A slightly misaligned, neptune-size transiting circumbinary planet', Astrophysical Journal, vol. 784, no. 1, 14. https://doi.org/10.1088/0004-637X/784/1/14
Kostov VB, McCullough PR, Carter JA, Deleuil M, Díaz RF, Fabrycky DC et al. Kepler-413B: A slightly misaligned, neptune-size transiting circumbinary planet. Astrophysical Journal. 2014 Mar 20;784(1). 14. https://doi.org/10.1088/0004-637X/784/1/14
Kostov, V. B. ; McCullough, P. R. ; Carter, J. A. ; Deleuil, M. ; Díaz, R. F. ; Fabrycky, D. C. ; Hébrard, G. ; Hinse, T. C. ; Mazeh, T. ; Orosz, J. A. ; Tsvetanov, Zlatan ; Welsh, W. F. / Kepler-413B : A slightly misaligned, neptune-size transiting circumbinary planet. In: Astrophysical Journal. 2014 ; Vol. 784, No. 1.
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