Hostname: page-component-cd9895bd7-gvvz8 Total loading time: 0 Render date: 2024-12-24T17:02:32.514Z Has data issue: false hasContentIssue false
  • English
  • Français

Aspects on the Dynamics and Detection of Additional Circumbinary Extrasolar Planets

Published online by Cambridge University Press:  29 April 2014

Tobias C. Hinse ,
Nader Haghighipour  and
Krzysztof Goździewski
Tobias C. Hinse
Affiliation:
Korea Astronomy & Space Science Institute, 305-348 Daejeon, Republic of Korea Armagh Observatory, College Hill, BT61 9DG, Armagh, UK email: [email protected]
Nader Haghighipour
Affiliation:
Institute for Astronomy & NASA Astrobiology Institute, University of Hawaii, 96822 HI, USA
Krzysztof Goździewski
Affiliation:
Torun Center for Astronomy, Nicolai Copernicus University, Torun, Poland
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

The presence of additional bodies orbiting a binary star system can be detected by monitoring the binary's eclipse timing. These so-called circumbinary objects will reveal themselves by i) either introducing a reflex motion of the binary system about the total system's barycenter creating a geometric light-travel time effect (LITE), ii) by gravitational perturbations on the binary orbit, or iii) a combination of the two effects resulting in eclipse timing (ETV) and transit timing (TTV) variations. Motivated by the four recently detected circumbinary planets by the Kepler space telescope (Kepler-16b, Kepler-34b, Kepler-35b and Kepler-38b) we have begun to study their dynamics in the presence of an additional massive perturber. In particular we used Kepler-16b as a test bed case. We are aiming to study the detectability of non-transiting and inclined circumbinary planets using the ETV effect along with the fast indicator MEGNO to quantitatively map the chaotic/quasi-periodic regions of the orbital parameter-space and to determine where the orbit of a circumbinary planet will be stable. We have calculated the amplitudes of TTV and ETV signals for different values of the mass and orbital elements of the planet and binary.

Keywords

binaries: closeeclipsingsubdwarfs – methods: data analysisnumerical – planets and satellites: detectiondynamical evolution and stability
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S293: Formation, Detection, and Characterization of Extrasolar Habitable Planets , August 2012 , pp. 133 - 139
Copyright
Copyright © International Astronomical Union 2014 

References

Agol, E., Steffen, J., Sari, R., & Clarkson, W. 2005, MNRAS, 359, 567Google Scholar
Almeida, L. A., Jablonski, F., & Rodrigues, C. V. 2013, ApJ, 766, 11CrossRefGoogle Scholar
Beuermann, K.et al. 2010, A&A, 521, 60Google Scholar
Beuermann, K., Dreizler, S., Hessman, F. V., & Deller, J. 2012, A&A, 543, 138Google Scholar
Beuermann, K., Dreizler, S., & Hessman, F. V. 2013, A&A 555 id. A133Google Scholar
Cincotta, P. M. & Simó, C. 2000, A&AS, 147, 205Google Scholar
Cincotta, P. M., Giordano, C. M., & Simó, C. 2003, Physica D, 182, 151CrossRefGoogle Scholar
Doyle, L. R.et al. 2011, Science, 333, 1602CrossRefGoogle Scholar
Goździewski, K.et al. 2001, A&A 378, 569Google Scholar
Goździewski, K.et al. 2012, MNRAS, 425, 930CrossRefGoogle Scholar
Hinse, T. C., Lee, J. W., Goździewski, K., Haghighipour, N., Lee, C.-U., & Scullion, E. M. 2012, MNRAS, 420, 3609CrossRefGoogle Scholar
Horner, J., Marshall, J. P., Wittenmyer, R. A., & Tinney, C. G. 2011, MNRAS, 416, 11CrossRefGoogle Scholar
Horner, J., Wittenmyer, R. A., Hinse, T. C., & Tinney, C. G. 2012, MNRAS, 425, 749CrossRefGoogle Scholar
Horner, J., Hinse, T. C., Wittenmyer, R. A., Marshall, J. P., & Tinney, C. G. 2012, MNRAS, 427, 2812CrossRefGoogle Scholar
Irwin, J. B. 1952, ApJ, 116, 218Google Scholar
Kozai, Y. 1962, AJ 67, 591CrossRefGoogle Scholar
Lee, J. W.et al. 2009, AJ, 137, 3181CrossRefGoogle Scholar
Migaszewski, C., Goździewski, K., & Hinse, T. C. 2008, MNRAS, 395, 1204CrossRefGoogle Scholar
Murray, C. D. & Dermott, S. F. 2000, Solar System Dynamics, Cambridge University PressGoogle Scholar
Orosz, J. A.et al. 2012a, ApJ, 758, 87Google Scholar
Orosz, J. A.et al. 2012b, Science, 337, 1511CrossRefGoogle Scholar
Potter, S. B.et al. 2011, MNRAS, 416, 2202CrossRefGoogle Scholar
Qian, S.-B.et al. 2011, MNRAS, 414, 16CrossRefGoogle Scholar
Schwarz, R.et al. 2009, A&A, 496, 833Google Scholar
Slonina, M., Goździewski, K., & Migaszweski, C. 2012, in Arenou, F., Hestroffer, D., eds., Proc. Workshop “Orbital Couples: Pas de Deux in the Solar System and the Milky Way”. Observatoire de Paris, Paris, p. 125Google Scholar
Welsh, W.et al. 2012, Nature, 481, 475Google Scholar
Wittenmyer, R. A., Horner, J., Marshall, J. P., Butters, O. W., & Tinney, C. G. 2012 MNRAS, 419, 3258Google Scholar
Wittenmyer, R. A., Horner, J., & Marshall, J. P. 2013 MNRAS, 431, 2150CrossRefGoogle Scholar