We present four new light curves of the transiting exoplanets WASP-1b and HAT-P-20b, observed within the TASTE (The Asiago Search for Transit timing variations of Exoplanets) project. We re-analyzed light curves from the literature in a homogeneous way, calculating a refined ephemeris and orbital-physical parameters for both objects. WASP-1b does not show any significant Transit Timing Variation signal at the 120 s level. As for HAT-P-20b, we detected a deviation from our re-estimated linear ephemeris that could be ascribed to the presence of a perturber or, more probably, to a previously unnoticed high level of stellar activity. The rotational period of HAT-P-20 A that we obtained from archival data (P-rot similar or equal to 14.5 d), combined with its optical variability and strong emission of Ca ii H & K lines, is consistent with a young stellar age (<1 Gyr) and support the hypothesis that stellar activity may be responsible of the measured deviations of the transit times. ((c) 2014 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim)

TASTE IV: Refining ephemeris and orbital parameters for HAT-P-20b and WASP-1b

GRANATA, VALENTINA;NASCIMBENI, VALERIO;PIOTTO, GIAMPAOLO;BORSATO, LUCA;CUNIAL, ANDREA;DAMASSO, MARIO;MALAVOLTA, LUCA
2014

Abstract

We present four new light curves of the transiting exoplanets WASP-1b and HAT-P-20b, observed within the TASTE (The Asiago Search for Transit timing variations of Exoplanets) project. We re-analyzed light curves from the literature in a homogeneous way, calculating a refined ephemeris and orbital-physical parameters for both objects. WASP-1b does not show any significant Transit Timing Variation signal at the 120 s level. As for HAT-P-20b, we detected a deviation from our re-estimated linear ephemeris that could be ascribed to the presence of a perturber or, more probably, to a previously unnoticed high level of stellar activity. The rotational period of HAT-P-20 A that we obtained from archival data (P-rot similar or equal to 14.5 d), combined with its optical variability and strong emission of Ca ii H & K lines, is consistent with a young stellar age (<1 Gyr) and support the hypothesis that stellar activity may be responsible of the measured deviations of the transit times. ((c) 2014 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim)
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/11577/3037508
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