Hostname: page-component-cd9895bd7-dzt6s Total loading time: 0 Render date: 2024-12-27T05:01:43.064Z Has data issue: false hasContentIssue false
  • English
  • Français

Kepler-410Ab and Transit Timing Variations

Published online by Cambridge University Press:  29 August 2019

P. Gajdoš ,
Š. Parimucha  and
M. Fedurco
P. Gajdoš
Affiliation:
Institute of Physics, Faculty of Natural Sciences, Šafárik University, Košice, Slovakia email: [email protected]
Š. Parimucha
Affiliation:
Institute of Physics, Faculty of Natural Sciences, Šafárik University, Košice, Slovakia email: [email protected]
M. Fedurco
Affiliation:
Institute of Physics, Faculty of Natural Sciences, Šafárik University, Košice, Slovakia email: [email protected]
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.

Our poster presented a new analysis of the transit-time variations displayed by the extrasolar planet Kepler-410Ab. We assumed that the observed changes in the transit times are caused by the gravitational influence of another body in the system. To determine the mass of that perturbing body, we considered the light-time effect and an analytical approximation of the perturbation model. The solutions resulting from both methods gave comparable results, with an orbital period of 970 days and a slightly eccentric orbit for the third body. We proposed two possible models of a perturbing body orbiting a common barycentre with Kepler-410A: a single star with mass of at least 0.906 M⊙, or a binary star with a total component mass of at least 2.15 M⊙.

Keywords

Eclipsesplanets and satellites: individual (Kepler-410Ab)techniques: photometricstars: binaries: general
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 14 , Symposium S339: Southern Horizons in Time-Domain Astronomy , November 2017 , pp. 299 - 302
Copyright
© International Astronomical Union 2019 

References

Adams, E. R., et al. 2012, AJ, 144, 4210.1088/0004-6256/144/2/42CrossRefGoogle Scholar
Agol, E. et al. 2005, MNRAS, 359, 56710.1111/j.1365-2966.2005.08922.xCrossRefGoogle Scholar
Gajdoš, P., et al. 2017, MNRAS, 469, 290710.1093/mnras/stx963CrossRefGoogle Scholar
Gajdoš, P., Parimucha, Š. 2018, Astron. Comput., 2019ascl.soft01002GGoogle Scholar
Irwin, J. B. 1952, ApJ, 116, 21110.1086/145604CrossRefGoogle Scholar
Mandel, K., & Agol, E. 2002, ApJ, 580, L17110.1086/345520CrossRefGoogle Scholar
Mazeh, T., et al. 2013, ApJS, 208, 16CrossRefGoogle Scholar
Van Eylen, V., et al. 2014, ApJ, 782, 14CrossRefGoogle Scholar