Shraddha Biswas, D. Bisht, Ing-Guey Jiang, Devesh P. Sariya, Kaviya Parthasarathy
{"title":"Probing the Possible Causes of the Transit Timing Variation for TrES-2b in TESS Era","authors":"Shraddha Biswas, D. Bisht, Ing-Guey Jiang, Devesh P. Sariya, Kaviya Parthasarathy","doi":"arxiv-2409.12069","DOIUrl":null,"url":null,"abstract":"Nowadays, transit timing variations (TTVs) are proving to be a very valuable\ntool in exoplanetary science to detect exoplanets by observing variations in\ntransit times. To study the transit timing variation of the hot Jupiter,\nTrES-2b, we have combined 64 high-quality transit light curves from all seven\nsectors of NASA's Transiting Exoplanet Survey Satellite (TESS) along with 60\nbest-quality light curves from the ground-based facility Exoplanet Transit\nDatabase (ETD) and 106 mid-transit times from the previous works. From the\nprecise transit timing analysis, we have observed a significant improvement in\nthe orbital ephemerides, but we did not detect any short period TTVs that might\nresult from an additional body. The inability to detect short-term TTVs further\nmotivates us to investigate long-term TTVs, which might be caused by orbital\ndecay, apsidal precession, Applegate mechanism, and $R{\\phi}$mer effect and the\norbital decay appeared to be a better explanation for the observed TTV with\n$\\Delta BIC$ = 4.32. The orbital period of the hot Jupiter TrES-2b appears to\nbe shrinking at a rate of $-5.58 \\pm 1.81$ ms/yr. Assuming this decay is\nprimarily caused by tidal dissipation within the host star, we have\nsubsequently calculated the stellar tidal quality factor value to be 9900,\nwhich is 2 to 3 orders of magnitude smaller than the theoretically predicted\nvalues for other hot-Jupiter systems and its low value indicates more efficient\ntidal dissipation within the host star. Additional precise photometric and\nradial velocity observations are required to pinpoint the cause of the change\nin the orbital period.","PeriodicalId":501209,"journal":{"name":"arXiv - PHYS - Earth and Planetary Astrophysics","volume":"48 1","pages":""},"PeriodicalIF":0.0000,"publicationDate":"2024-09-18","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":"0","resultStr":null,"platform":"Semanticscholar","paperid":null,"PeriodicalName":"arXiv - PHYS - Earth and Planetary Astrophysics","FirstCategoryId":"1085","ListUrlMain":"https://doi.org/arxiv-2409.12069","RegionNum":0,"RegionCategory":null,"ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":null,"EPubDate":"","PubModel":"","JCR":"","JCRName":"","Score":null,"Total":0}
引用次数: 0
Abstract
Nowadays, transit timing variations (TTVs) are proving to be a very valuable
tool in exoplanetary science to detect exoplanets by observing variations in
transit times. To study the transit timing variation of the hot Jupiter,
TrES-2b, we have combined 64 high-quality transit light curves from all seven
sectors of NASA's Transiting Exoplanet Survey Satellite (TESS) along with 60
best-quality light curves from the ground-based facility Exoplanet Transit
Database (ETD) and 106 mid-transit times from the previous works. From the
precise transit timing analysis, we have observed a significant improvement in
the orbital ephemerides, but we did not detect any short period TTVs that might
result from an additional body. The inability to detect short-term TTVs further
motivates us to investigate long-term TTVs, which might be caused by orbital
decay, apsidal precession, Applegate mechanism, and $R{\phi}$mer effect and the
orbital decay appeared to be a better explanation for the observed TTV with
$\Delta BIC$ = 4.32. The orbital period of the hot Jupiter TrES-2b appears to
be shrinking at a rate of $-5.58 \pm 1.81$ ms/yr. Assuming this decay is
primarily caused by tidal dissipation within the host star, we have
subsequently calculated the stellar tidal quality factor value to be 9900,
which is 2 to 3 orders of magnitude smaller than the theoretically predicted
values for other hot-Jupiter systems and its low value indicates more efficient
tidal dissipation within the host star. Additional precise photometric and
radial velocity observations are required to pinpoint the cause of the change
in the orbital period.