Revisiting the Transit Timing Variation of Extra-solar Planets TrES-3b and Qatar-1b with TESS data
Creators
- 1. Department of Pure and Applied Physics, Guru Ghasidas Vishwavidyalaya (A Central University), Bilaspur (C.G.)-495009, India
- 2. Indian Institute of Astrophysics, Bangalore-560034, India
- 3. Department of Physics and Institute of Astronomy, National Tsing-Hua University, Hsinchu, Taiwan
- 4. Astrophysics Group, Keele University, Staffordshire ST5 5BG, UK
- 5. Max Planck Institute for Astronomy, Königstuh l17, D-69117 Heidelberg, Germany
- 6. Astronomical Institute, Slovak Academy of Sciences, SK-059 60 Tatranská Lomnica, Slovakia
- 7. Institute of Physics, Faculty of Science, Pavol Jozef 𝑆áfrik University, Košice, Slovakia
- 8. Institute of Computational and Modeling Science, National Tsing-Hua University, Hsinchu, Taiwan
Description
We have investigated the possibility of transit timing variation (TTV) and its plausible cause in the hot-Jupiter systems TrES-3 and Qatar-1. In this study, total160 transit light curves of TrES-3b and 197 transit light curves of Qatar-1b are considered. Using the mid-transit times determined from these light curves, we have improved the transit ephemeris for both these hot-Jupiters. Our timing analysis show the presence of TTVs in these planetary systems that are unlikely to be periodic. To explore the possibility of a long-term TTVs, the orbital decay model was fitted to transit timing data which reveals the period change of 2.71 ± 1.49 ms/yr and 12.39 ± 2.74 ms/yr for TrES-3b and Qatar-1b, respectively. It is worth to mention here that we have observed increasing period for both hot-Jupiters in contrast to the previous results available in literature. Because of the statistically less significant estimate of period change of TrES-3b, we prefer a linear ephemeris model over the decay model. However, the linear model does not appear to represent the transit data of Qatar-1b considered here as the observed change in period is highly significant. This change may not be attributed to orbital decay and there may be some other plausible reasons such as presence of a third body in wider orbit and the apsidal precession.
