Is the orbit of the exoplanet WASP-43b really decaying? <i>TESS</i> and MuSCAT2 observations confirm no detection

Garai, Z.; Pribulla, T.; Parviainen, H.; Πάλλη, Ε.; Claret, A.; Szigeti, László; Béjar, V. J. S.; Casasayas-Barris, N.; Crouzet, Nicolas; Fukui, A.; Chen, G.; Kawauchi, Kiyoe; Klagyivik, P.; Kurita, S.; Kusakabe, Nobuhiko; Leon, Jerome P. de; Livingston, John H.; Luque, R.; Mori, M.; Murgas, F.; Narita, Norio; Nishiumi, Taku; Oshagh, M.; Szabó, Gy. M.; Tamura, Motohide; Terada, Yuka; Watanabe, Noriharu

doi:10.1093/mnras/stab2929

Cited by 14 publications

(14 citation statements)

References 48 publications

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“…Consequently, the linear trend was removed from each chunk of data (including the transit data). This detrending method can effectively remove the long-term variability (mainly variability of the host star due to spots and rotation) while it does not introduce any nonlinear trend to the data, see e.g., Garai et al (2021). Outliers were cleaned using a 3σ clipping, where σ is the standard deviation of the light curve.…”

Section: Search For Long-term Tdvs -Signs Of Orbital Precessionmentioning

confidence: 99%

“…Subsequently, the O-C data were fitted with a quadratic function within the OC-FIT package FitQuad. The free parameters of the quadratic model are the mid-transit time Tc, the orbital period P orb , and the quadratic coefficient Q, see Garai et al (2021) for more information about this parameter. The uncertainties in the fitted parameters of P orb , Tc, and Q were derived within the OCFIT packages FitLinear and FitQuad, applying the covariance matrix method.…”

Section: Search For Long-term Tdvs -Signs Of Orbital Precessionmentioning

confidence: 99%

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Rapidly rotating stars and their transiting planets: KELT-17b, KELT-19Ab, and KELT-21b in the CHEOPS and TESS era

Garai,

Pribulla,

Kovács

et al. 2022

Preprint

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Rapidly rotating early-type main-sequence stars with transiting planets are interesting in many aspects. Unfortunately, several astrophysical effects in such systems are not well understood yet. Therefore, we performed a photometric mini-survey of three rapidly rotating stars with transiting planets, namely KELT-17b, KELT-19Ab, and KELT-21b, using the Characterising Exoplanets Satellite (CHEOPS ), complemented with Transiting Exoplanet Survey Satellite (TESS ) data, and spectroscopic data. We aimed at investigating the spin-orbit misalignment and its photometrical signs, therefore the high-quality light curves of the selected objects were tested for transit asymmetry, transit duration variations, and orbital precession. In addition, we performed transit time variation analyses, obtained new stellar parameters, and refined the system parameters. For KELT-17b and KELT-19Ab we obtained significantly smaller planet radius as found before. The gravity-darkening effect is very small compared to the precision of CHEOPS data. We can report only on a tentative detection of the stellar inclination of KELT-21, which is about 60 deg. In we were able to exclude long-term transit duration variations causing orbital precession. The shorter transit duration of KELT-19Ab compared to the discovery paper is probably a consequence of a smaller planet radius. KELT-21b is promising from this viewpoint, but further precise observations are needed. We did not find any convincing evidence for additional objects in the systems.

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Section: Search For Long-term Tdvs -Signs Of Orbital Precessionmentioning

confidence: 99%

Section: Search For Long-term Tdvs -Signs Of Orbital Precessionmentioning

confidence: 99%

Rapidly rotating stars and their transiting planets: KELT-17b, KELT-19Ab, and KELT-21b in the CHEOPS and TESS era

Garai,

Pribulla,

Kovács

et al. 2022

Preprint

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“…The transit timings of WASP-32b are monitored and no significant TTV is found with the available data (Sun et al, 2015). WASP-43b is reported as a candidate showing period decay (Jiang et al, 2016) which arises wide attention and scientific discussions (Davoudi et al, 2021;Garai et al, 2021). WASP-4b presents a significant TTV and is furtherly explained by the Rømer effect (Bouma et al, 2019(Bouma et al, , 2020.…”

Section: Introductionmentioning

confidence: 98%

Detecting and Monitoring Tidal Dissipation of Hot Jupiters in the Era of SiTian

Yang,

Wang,

Wei

et al. 2022

Preprint

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Transit Timing Variation (TTV) of hot Jupiters provides direct observational evidence of planet tidal dissipation. Detecting tidal dissipation through TTV needs high precision transit timings and long timing baselines. In this work, we predict and discuss the potential scientific contribution of SiTian Survey in detecting and analyzing exoplanet TTV. We develop a tidal dissipation detection pipeline for SiTian Survey that aims at time-domain astronomy with 72 1-meter optical telescopes. The pipeline includes the modules of light curve deblending, transit timing obtaining, and TTV modeling. SiTian is capable to detect more than 25,000 exoplanets among which we expect ∼50 sources showing evidence of tidal dissipation. We present detection and analysis of tidal dissipating targets, based on simulated SiTian light curves of XO-3b and WASP-161b. The transit light curve modeling gives consistent results within 1σ to input values of simulated light curves. Also, the parameter uncertainties predicted by Monte-Carlo Markov Chain are consistent with the distribution obtained from simulating and modeling the light curve 1000 times. The timing precision of SiTian observations is ∼ 0.5 minutes with one transit visit. We show that differences between TTV origins, e.g., tidal dissipation, apsidal precession, multiple planets, would be significant, considering the timing precision and baseline. The detection rate of tidal dissipating hot Jupiters would answer a crucial question of whether the planet migrates at an early formation stage or random stages due to perturbations, e.g., planet scattering, secular interaction. SiTian identified targets would be constructive given that the sample would extend tenfold.

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“…WASP-43b is a very well-studied "hot Jupiter" exoplanet (e.g. Louden & Kreidberg 2018;Gandhi & Madhusudhan 2017;Komacek et al 2017;Keating & Cowan 2017;Gandhi & Jermyn 2020;Feng et al 2020;Lustig-Yaeger et al 2021;Garai et al 2021). It has a rich variety of available observational data, including an emission phase curve (Stevenson et al 2014(Stevenson et al , 2017 and a transmission spectrum that has been found to contain strong evidence of molecular signatures (e.g.…”

Section: Introductionmentioning

confidence: 99%

Exoplanet Atmosphere Retrievals in 3D Using Phase Curve Data with ARCiS: Application to WASP-43b

Chubb

Min

2022

A&A

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Aims. Our goal is to create a retrieval framework which encapsulates the three-dimensional (3D) nature of exoplanet atmospheres, and to apply it to observed emission phase curve and transmission spectra of the 'hot Jupiter' exoplanet WASP-43b. Methods. We present our 3D framework, which is freely available as a stand-alone module from GitHub. We use the atmospheric modelling and Bayesian retrieval package ARCiS (ARtful modelling Code for exoplanet Science) to perform a series of eight 3D retrievals on simultaneous transmission (HST/WFC3) and phase-dependent emission (HST/WFC3 and Spitzer/IRAC) observations of WASP-43b as a case study. Via these retrieval setups, we assess how input assumptions affect our retrieval outcomes. In particular we look at constraining equilibrium chemistry vs a free molecular retrieval, the case of no clouds vs parametrised clouds, and using Spitzer phase data that have been reduced from two different literature sources. For the free chemistry retrievals, we retrieve abundances of H 2 O, CH 4 , CO, CO 2 , AlO, and NH 3 as a function of phase, with many more species considered for the equilibrium chemistry retrievals.Results. We find consistent super-solar C/O (0.6 -0.9) and super-solar metallicities (1.7 -2.9 dex) for all retrieval setups that assume equilibrium chemistry. We find that atmospheric heat distribution, hotspot shift (≈15.6 • vs 4.5 • for the different Spitzer datasets), and temperature structure are very influenced by the choice of Spitzer emission phase data. We see some trends in molecular abundances as a function of phase, in particular for CH 4 and H 2 O. Comparisons are made with other studies of WASP-43b, including global climate model (GCM) simulations, available in the literature. Conclusions. The parametrised 3D setup we have developed provides a valuable tool to analyse extensive observational datasets such as spectroscopic phase curves. We conclude that further near-future observations with missions such as the James Webb Space Telescope (JWST) and Ariel will greatly improve our understanding of the atmospheres of exoplanets such as WASP-43b. This is particularly evident from the effect that the current phase-dependent Spitzer emission data has on retrieved atmospheres.

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Is the orbit of the exoplanet WASP-43b really decaying? TESS and MuSCAT2 observations confirm no detection

Cited by 14 publications

References 48 publications

Rapidly rotating stars and their transiting planets: KELT-17b, KELT-19Ab, and KELT-21b in the CHEOPS and TESS era

Rapidly rotating stars and their transiting planets: KELT-17b, KELT-19Ab, and KELT-21b in the CHEOPS and TESS era

Detecting and Monitoring Tidal Dissipation of Hot Jupiters in the Era of SiTian

Exoplanet Atmosphere Retrievals in 3D Using Phase Curve Data with ARCiS: Application to WASP-43b

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