Transiting Exoplanet Monitoring Project (TEMP). IV. Refined System Parameters, Transit Timing Variations, and Orbital Stability of the Transiting Planetary System HAT-P-25

Wang, Xianyu; Wang, Songhu; Hinse, T. C.; Li, Kai; Wang, Yong-Hao; Laughlin, Gregory; Liu, Hui-Gen; Zhang, Hui; Wu, Zhaoyang; Zhou, Xu; Zhou, Ji-Lin; Hu, Shaoming; Wu, Dong-Hong; Peng, Xiyan; Chen, Yuanyuan

doi:10.1088/1538-3873/aab93e

Cited by 22 publications

(16 citation statements)

References 49 publications

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“…Here we apply the technique for TTV calculations as described in Wang et al (2017Wang et al ( , 2018a. The calculation of an upper mass-limit is performed numerically from directly integrating the orbits.…”

Section: Constraints On the Mass Of A Possible Perturbermentioning

confidence: 99%

“…This setting provides a most conservative estimate of the upper mass limit of a possible perturber (Bean 2009;Fukui et al 2011;Hoyer et al 2011Hoyer et al , 2012. We refer the interested reader to Wang et al (2018a) where the authors have studied the effect on upper mass limit for various initial orbital parameters. For example, while the initial eccentricity would change the overall system stability and introduce higher-order mean-motion resonances, the effect on upper mass limit due to different initial phase of the peturbing planet is subtle.…”

Section: Constraints On the Mass Of A Possible Perturbermentioning

confidence: 99%

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Discarding orbital decay in WASP-19b after one decade of transit observations★†

Petrucci

Jofré

Chew

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We present a empirical study of orbital decay for the exoplanet WASP-19b, based on mid-time measurements of 74 complete transits (12 newly obtained by our team and 62 from the literature), covering a 10-year baseline. A linear ephemeris best represents the mid-transit times as a function of epoch. Thus, we detect no evidence of the shortening of WASP-19b's orbital period and establish an upper limit of its steady changing rate,Ṗ = −2.294 ms yr −1 , and a lower limit for the modified tidal quality factor Q = (1.23 ± 0.231) × 10 6 . Both are in agreement with previous works. This is the first estimation of Q directly derived from the mid-times of WASP-19b obtained through homogeneously analyzed transit measurements. Additionally, we do not detect periodic variations in the transit timings within the measured uncertainties in the midtimes of transit. We are therefore able to discard the existence of planetary companions in the system down to a few M ⊕ in the first order mean-motion resonances 1:2 and 2:1 with WASP-19b, in the most conservative case of circular orbits. Finally, we measure the empirical Q values of 15 exoplanet host stars which suggest that stars with T eff 5600K dissipate tidal energy more efficiently than hotter stars. This tentative trend needs to be confirmed with a larger sample of empirically measured Q .

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Section: Constraints On the Mass Of A Possible Perturbermentioning

confidence: 99%

Section: Constraints On the Mass Of A Possible Perturbermentioning

confidence: 99%

Discarding orbital decay in WASP-19b after one decade of transit observations★†

Petrucci

Jofré

Chew

et al. 2019

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

show abstract

“…This setting provides the most conservative estimate of the upper mass limit of a possible perturber (Bean 2009;Fukui et al 2011;Hoyer et al 2011Hoyer et al , 2012. For the interested readers, we refer to Wang et al (2018d), which has studied the effects of TTVs on varying initial orbital parameters.…”

Section: Orbital Stability and Mass Limits Of Additional Perturbersmentioning

confidence: 99%

“…The assumption on the orbital shape of the perturber is somewhat arbitrary. We refer the reader to Wang et al (2018d) for an exploration of the effects of starting the perturbing planet on a higher eccentricity orbit.…”

Section: Orbital Stability and Mass Limits Of Additional Perturbersmentioning

confidence: 99%

Transiting Exoplanet Monitoring Project (TEMP). V. Transit Follow Up for HAT-P-9b, HAT-P-32b, and HAT-P-36b

Wang

Hinse

et al. 2019

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During the past five years, 6, 7, and 26 transit observations were carried out for the HAT-P-9b, HAT-P-32b, and HAT-P-36b systems, respectively, through the Transiting Exoplanet Monitoring Project network. Combined with the published photometric data and radial-velocity measurements, our new photometry allows us to revisit the system parameters and search for additional close-in planetary companions in these hot Jupiter systems. We measure an updated R P /R * = 0.1260 ± 0.0011 for HAT-P-36 system in the R band, which is 4.5σ larger than the published i-band radius ratio of 0.1186 ± 0.0012. We also perform a transit timing variation (TTV) analysis for each system. Because no significant TTVs were found, we place an upper mass limit on an additional planet for each system.

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“…The applied method follows the technique described in Wang et al (2018aWang et al ( , 2017bWang et al ( , 2018c. The calculation of an upper mass limit is performed numerically via direct orbit integrations.…”

Section: Upper Mass Limits Of a Hypothetical Perturbermentioning

confidence: 99%

TraMoS

Cortés-Zuleta

Rojo

Wang

et al. 2020

A&A

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We present 22 new transit observations of the exoplanets WASP-18Ab, WASP-19b, and WASP-77Ab, from the Transit Monitoring in the South project. We simultaneously model our newly collected transit light curves with archival photometry and radial velocity data to obtain refined physical and orbital parameters. We include TESS light curves of the three exoplanets to perform an extended analysis of the variations in their transit mid-time (TTV) and to refine their planetary orbital ephemeris. We did not find significant TTVRMS variations larger than 47, 65, and 86 s for WASP-18Ab, WASP-19b, and WASP-77Ab, respectively. Dynamical simulations were carried out to constrain the masses of a possible perturber. The observed mean square (RMS) could be produced by a perturber body with an upper limit mass of 9, 2.5, 11 and 4 M⊕ in 1:2, 1:3, 2:1, and 3:1 resonances in the WASP-18Ab system. In the case of WASP-19b, companions with masses up to 0.26, 0.65, 1, and 2.8 M⊕, in 1:2, 2:1, 3:1, and 5:3 resonances respectively, produce the RMS. For the WASP-77Ab system, this RMS could be produced by a planet with mass in the range of 1.5−9 M⊕ in 1:2, 1:3, 2:1, 2:3, 3:1, 3:5, or 5:3 resonances. Comparing our results with RV variations, we discard massive companions with 350 M⊕ in 17:5 resonance for WASP-18Ab, 95 M⊕ in 4:1 resonance for WASP-19b, and 105 M⊕ in 5:2 resonance for WASP-77Ab. Finally, using a Lomb-Scargle period search we find no evidence of a periodic trend on our TTV data for the three exoplanets.

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Transiting Exoplanet Monitoring Project (TEMP). IV. Refined System Parameters, Transit Timing Variations, and Orbital Stability of the Transiting Planetary System HAT-P-25

Cited by 22 publications

References 49 publications

Discarding orbital decay in WASP-19b after one decade of transit observations★†

Discarding orbital decay in WASP-19b after one decade of transit observations★†

Transiting Exoplanet Monitoring Project (TEMP). V. Transit Follow Up for HAT-P-9b, HAT-P-32b, and HAT-P-36b

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