Transit timing analysis in the HAT-P-32 system

Seelıger, M.; Dımıtrov, D.; Kjurkchıeva, D.; Mallonn, M.; Fernandez, M.; Kıtze, M.; Casanova, V.; Macıejewskı, G.; Ohlert, J.; Schmıdt, J.; Pannıcke, A.; Puchalskı, D.; Gogus, E.; Guver, Tolga; Bilir, Selçuk; Ak, Tansel; Hohle, M.; Schmıdt, T.; Errmann, R.; Jensen, E.; Cohen, D.; Marschall, L.; Saral, G.; Bernt, I.; Derman, E.; Galan, C.; Neuhaeuser, R.

doi:10.1093/mnras/stu567

Transit timing analysis in the HAT-P-32 system

Atıf İçin Kopyala

Seelıger M., Dımıtrov D., Kjurkchıeva D., Mallonn M., Fernandez M., Kıtze M., ...Daha Fazla

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, cilt.441, ss.304-315, 2014 (SCI-Expanded)

Yayın Türü: Makale / Tam Makale
Cilt numarası: 441
Basım Tarihi: 2014
Doi Numarası: 10.1093/mnras/stu567
Dergi Adı: MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Derginin Tarandığı İndeksler: Science Citation Index Expanded (SCI-EXPANDED), Scopus
Sayfa Sayıları: ss.304-315
Anahtar Kelimeler: planets and satellites: individual: HAT-P-32b, stars: individual: HAT-P-32, planetary systems, HOT JUPITER, LIGHT CURVES, PLANETS, CONSTRAINTS, PHOTOMETRY, JITTER, STARS, ORBIT, TIME, I.
İstanbul Üniversitesi Adresli: Evet

Özet

We present the results of 45 transit observations obtained for the transiting exoplanet HATP-32b. The transits have been observed using several telescopes mainly throughout the YETI (Young Exoplanet Transit Initiative) network. In 25 cases, complete transit light curves with a timing precision better than 1.4 min have been obtained. These light curves have been used to refine the system properties, namely inclination i, planet-to-star radius ratio R-p/R-s, and the ratio between the semimajor axis and the stellar radius a/R-s. First analyses by Hartman et al. suggests the existence of a second planet in the system, thus we tried to find an additional body using the transit timing variation (TTV) technique. Taking also the literature data points into account, we can explain all mid-transit times by refining the linear ephemeris by 21 ms. Thus, we can exclude TTV amplitudes of more than similar to 1.5min.