A search for transit timing variations and orbital decay in WASP-46b

Petrucci, R.; Jofré, Edgardo; Ferrero, L. V.; Cúneo, V. A.; Saker, L.; Lovos, F. V.; Gómez, Maríana; Mauas, P. J. D.

doi:10.1093/mnras/stx2647

Cited by 36 publications

(9 citation statements)

References 54 publications

(105 reference statements)

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“…Nowadays, these planets are usually within the corotation radius of their billion year old stars but tidal dissipation of the dynamical tide is now extremely weak and does not lead to significant orbital decay. This is in agreement with the null detection of tidally driven orbital decay observed for the hot Jupiters WASP-43 b (Hoyer et al 2016b), OGLE-TR-113 b (Hoyer et al 2016a), and WASP-46 b (Petrucci et al 2018), which suggest Q 10 5 , and with the high tidal quality factors found in a recent census of the hot Jupiter population (Collier Cameron & Jardine 2018). Gener-ally speaking, we predict that the tidally driven orbital decay of hot Jupiters around Sun-like main-sequence stars cannot be observed in most cases due to the extremely ineffective tidal dissipation in the convective envelope, producing frequencyaveraged tidal dissipation factors of 10 8 Q 10 9 .…”

supporting

confidence: 88%

Formation of hot Jupiters through disk migration and evolving stellar tides

Heller

2019

A&A

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Since the discovery of Jupiter-sized planets in extremely close orbits around Sun-like stars, several mechanisms have been proposed to produce these "hot Jupiters". Here we address their pile-up at 0.05 AU observed in stellar radial velocity surveys, their longterm orbital stability in the presence of stellar tides, and their occurrence rate of 1.2 ±0.38 % in one framework. We calculate the combined torques on the planet from the stellar dynamical tide and from the protoplanetary disk in the type II migration regime. The disk is modelled as a 2D non-isothermal viscous disk parameterized to reproduce the minimum-mass solar nebula. We simulate an inner disk cavity at various radial positions near the star and simulate stellar rotation periods according to observations of young star clusters. The planet is on a circular orbit in the disk midplane and in the star's equatorial plane. We show that the two torques can add up to zero beyond the corotation radius around young, solar-type stars and stop inward migration. Monte Carlo simulations with plausible variations of our nominal parameterization of the star-disk-planet model predict hot Jupiter survival rates between about 3 % (for an α disk viscosity of 10 −1 ) and 15 % (for α = 10 −3 ) against consumption by the star. Once the protoplanetary disk has been fully accreted, the surviving hot Jupiters are pushed outward from their tidal migration barrier and pile up at about 0.05 AU, as we demonstrate using a numerical implementation of a stellar dynamical tide model coupled with stellar evolution tracks. Orbital decay is negligible on a billion year time scale due to the contraction of the highly dissipative convective envelopes in young Sun-like stars. We find that the higher pile-up efficiency around metal-rich stars can at least partly explain the observed positive correlation between stellar metallicity and hot Jupiter occurrence rate. Combined with the observed hot Jupiter occurrence rate, our results for the survival rate imply that 8 % (α = 10 −3 ) to 43 % (α = 10 −1 ) of sun-like stars initially encounter an inward migrating hot Jupiter. Our scenario reconciles models and observations of young spinning stars with the observed hot Jupiter pile up and hot Jupiter occurrence rates.

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supporting

confidence: 88%

Formation of hot Jupiters through disk migration and evolving stellar tides

Heller

2019

A&A

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“…For those light curves observed with no filter, we used the average of the values in the Johnson V and the Cousins R bands as in Nascimbeni et al (2013). Finally, the initial LD coefficients assumed for the observations in the J-, H-, and K-bands of GROND and those obtained by Bean et al (2013) in the same wavelength range, were those of Johnson J, H, and K. Here, it is important to notice that, as previously demonstrated in Petrucci et al (2018), the initial values adopted for the LD coefficients, even if they correspond to a filter with a different effective wavelength than that of the band used to perform the observations, cause a negligible effect on the measured mid-transit times with changes in the ephemeris within its 1σ error.…”

Section: Determination Of Photometric Parametersmentioning

confidence: 99%

“…Petrucci et al (2018): i) strongly correlated parameters if -1 ≤ r -0.8 or 0.8 r ≤ 1, ii) moderatly correlated parameters if -0.8 r -0.5 or 0.5 r 0.8, and weakly correlated parameters if -0.5 r ≤ 0 or 0 ≤ r 0.5.…”

mentioning

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

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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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“…We analyzed four highquality ETD light curves after epoch=1551, along with Tess light curves, and obtained the mid-transit times and the uncertainties. We have continued their method by choosing data points with uncertainties less than 1 min according to the result of Petrucci et al (2018). We plotted a new TTV diagram (Figure 9) using the ephemeris given by Petrucci et al (2018) (Equation 19) and realized that a decrease in the orbital period doesn't continue and TTV values become positive.…”

Section: Wasp-46bmentioning

confidence: 99%

Refined Ephemeris for Four Hot Jupiters using Ground-Based and TESS Observations

Davoudi¹,

MirshafieKhozani²,

Paki³

et al. 2021

Письма в Астрон. ж.

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Transit Timing Variation (TTV) is a powerful method to study the dynamics of multiple transiting planetary systems. We examined the TTV of four planetary systems: WASP-12b, WASP-33b, WASP-36b, and WASP-46b. The purpose of this work is to refine the reference ephemeris of these four systems and to draw inferences on any apparent variability of the transits' periodicity. We used the light curves of these systems from the Transiting light Exoplanet Survey Satellite (TESS) observations and some ground-based telescopes. We modeled these light curves to measure the transit times using Exofast. We plotted their TTV diagrams built from our obtained midtransit times and those available in the literature. Our MCMC analysis of these timings enabled us to refined the transit ephemeris of the four systems. We found an apparent variation of the orbital period, 𝑝̇= −24 ± 2 𝑚𝑠 𝑦𝑟 for WASP-12b and 𝑄 * = (2.16 ± 0.35) × 10 for the tidal quality parameter of its host star. We realized that the orbital period is increasing in the WASP-46b system, so its star magnetic activity is a stronger model than orbital decay for period variation of this system. We obtained ∆𝑃 = 7.37 ± 8.64 𝑚𝑠 during 10 years for WASP-36b; It indicates that orbital decay may be present in this system. But since there is no obvious quadratic trend in its TTV diagram, variations are likely due to wrong linear ephemeris that increased over 10 years.

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A search for transit timing variations and orbital decay in WASP-46b

Cited by 36 publications

References 54 publications

Formation of hot Jupiters through disk migration and evolving stellar tides

Formation of hot Jupiters through disk migration and evolving stellar tides

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

Refined Ephemeris for Four Hot Jupiters using Ground-Based and TESS Observations

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