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Transit timing variations in WASP-10b induced by stellar activity
Barros, S. C. C.; Boué, G.; Gibson, N. P.; Pollacco, D. L.; Santerne, A.; Keenan, F. P.; Skillen, I.; Street, R. A.
AA(Aix Marseille Université, CNRS, LAM (Laboratoire d'Astrophysique de Marseille), UMR 7326, 13388 Marseille, France; ), AB(Centro de Astrofísica, Universidade do Porto, Rua das Estrelas, 4150-762 Porto, Portugal; Astronomie et Systèmes Dynamiques, IMCCE-CNRS UMR8028, Observatoire de Paris, UPMC, 77 Avenue Denfert-Rochereau, 75014 Paris, France; Department of Astronomy and Astrophysics, University of Chicago, 5640 South Ellis Avenue, Chicago, IL 60637, USA), AC(European Southern Observatory, Karl-Schwarzschild-Str. 2, D-85748 Garching bei München, Germany), AD(Department of Physics, University of Warwick, Coventry CV4 7AL, UK), AE(Aix Marseille Université, CNRS, LAM (Laboratoire d'Astrophysique de Marseille), UMR 7326, 13388 Marseille, France), AF(Astrophysics Research Centre, School of Mathematics and Physics, Queen's University Belfast, University Road, Belfast BT7 1NN, UK), AG(Isaac Newton Group of Telescopes, Apartado de Correos 321, E-38700 Santa Cruz de la Palma, Tenerife, Spain), AH(Las Cumbres Observatory, 6740 Cortona Drive Suite 102, Goleta, CA 93117, USA)
Monthly Notices of the Royal Astronomical Society, Volume 430, Issue 4, p.3032-3047 (MNRAS Homepage)
Publication Date:
Astronomy Keywords:
techniques: photometric, time, stars: activity, stars: individual: WASP-10, planetary systems, starspots
Abstract Copyright:
2013 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society
Bibliographic Code:


The hot-Jupiter WASP-10b was reported by Maciejewski et al. to show transit timing variations (TTVs) with an amplitude of ˜3.5 min. These authors proposed that the observed TTVs were caused by a 0.1MJup perturbing companion with an orbital period of ˜5.23 d, and hence, close to the outer 5:3 mean-motion resonance with WASP-10b. To test this scenario, we present eight new transit light curves of WASP-10b obtained with the Faulkes Telescope North and the Liverpool Telescope. The new light curves, together with 22 previously published ones, were modelled with a Markov Chain Monte Carlo transit fitting code. Transit depth differences reported for WASP-10b are thought to be due to starspot-induced brightness modulation of the host star. Assuming the star is brighter at the activity minimum, we favour a small planetary radius. We find R_p =1.039^{+0.043}_{-0.049} {R_Jup} in agreement with Johnson et al. and Maciejewski et al. Recent studies find no evidence for a significant eccentricity in this system. We present consistent system parameters for a circular orbit and refine the orbital ephemeris of WASP-10b. Our homogeneously derived transit times do not support the previous claimed TTV signal, which was strongly dependent on two previously published transits that have been incorrectly normalized. Nevertheless, a linear ephemeris is not a statistically good fit to the transit times of WASP-10b. We show that the observed transit time variations are due to spot occultation features or systematics. We discuss and exemplify the effects of occultation spot features in the measured transit times and show that despite spot occultation during egress and ingress being difficult to distinguish in the transit light curves, they have a significant effect in the measured transit times. We conclude that if we account for spot features, the transit times of WASP-10b are consistent with a linear ephemeris with the exception of one transit (epoch 143) which is a partial transit. Therefore, there is currently no evidence for the existence of a companion to WASP-10b. Our results support the lack of TTVs of hot-Jupiters reported for the Kepler sample.
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