Homogeneous transit timing analyses of 10 exoplanet systems

Creative Commons License

Basturk O., Esmer E. M., Yalçınkaya S., Torun L., Mancini L., Helweh F., ...Daha Fazla

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, cilt.512, sa.2, ss.2062-2081, 2022 (SCI-Expanded) identifier identifier identifier

  • Yayın Türü: Makale / Tam Makale
  • Cilt numarası: 512 Sayı: 2
  • Basım Tarihi: 2022
  • Doi Numarası: 10.1093/mnras/stac592
  • Dergi Adı: MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
  • Derginin Tarandığı İndeksler: Science Citation Index Expanded (SCI-EXPANDED), Scopus, Academic Search Premier, Aerospace Database, Applied Science & Technology Source, Communication Abstracts, INSPEC, Metadex, zbMATH, DIALNET, Civil Engineering Abstracts
  • Sayfa Sayıları: ss.2062-2081
  • Anahtar Kelimeler: methods: observational, techniques: photometric, planetary systems, stars: individual: HAT-P-23, WASP-37, WASP-69, WASP-74, HAT-P-56, WASP-2, WASP-14, HAT-P-32, WASP-103, HAT-P-37, OPTICAL-TRANSMISSION SPECTRUM, HIGH-PRECISION PHOTOMETRY, HOT JUPITERS, PHYSICAL-PROPERTIES, ECLIPSE PHOTOMETRY, PLANETARY SYSTEM, STARS, RADIUS, I., HAT-P-32AB
  • Atatürk Üniversitesi Adresli: Evet

Özet

We study the transit timings of 10 exoplanets in order to investigate potential transit timing variations in them. We model their available ground-based light curves, some presented here and others taken from the literature, and homogeneously measure the mid-transit times. We statistically compare our results with published values and find that the measurement errors agree. However, in terms of recovering the possible frequencies, homogeneous sets can be found to be more useful, of which no statistically relevant example has been found for the planets in our study. We corrected the ephemeris information of all 10 planets we studied and provide these most precise light elements as references for future transit observations with space-borne and ground-based instruments. We found no evidence for secular or periodic changes in the orbital periods of the planets in our sample, including the ultra-short period WASP-103 b, whose orbit is expected to decay on an observable time-scale. Therefore, we derive the lower limits for the reduced tidal quality factors (Q(*)') for the host stars based on best-fitting quadratic functions to their timing data. We also present a global model of all available data for WASP-74 b, which has a Gaia parallax-based distance value similar to 25 per cent larger than the published value.