The ‘‘Detectability Window’’ Method to Take into Account Observational Selection in the Statistics of Exoplanets Discovered through Radial Velocity Measurements

Ivanova, A. E.; Yakovlev, O. Ya.; Ananyeva, V. I.; Shashkova, I. A.; Tavrov, A. V.; Bertaux, Jean-Loup

doi:10.1134/s1063773721010059

Cited by 4 publications

(2 citation statements)

References 7 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…In recent time substantial efforts have been dedicated to characterise a bunch of planetary parameters of hot Jupiter through different observational methods (6,7) . Current exoplanet discovery trend is piling up hot Jupiter numbers to make them suitable for applying statistical techniques to other planetary parameters.…”

Section: Introductionmentioning

confidence: 99%

Observational Evidence of Bimodal Distribution in Hot Jupiter Population

Mondal

2023

IJST

View full text Add to dashboard Cite

Objectives: Hot Jupiters, a special class of exoplanets always draw attention due to their intriguing characteristics. Here we wish to establish the differentiation of two planetary mass groups having orbital eccentricity discrimination. Methods: A comprehensive statistical approach has been carried out to understand the distribution of hot Jupiter population and the architecture of those planetary. 312 hot Jupiters have been filtered out from 4285 different scientifically recognized exoplanet databases and such a huge hot Jupiter sample size has not been used to find out any intrinsic correlation before. Different techniques to discover hot Jupiters have been studied here to segregate them. Relation between orbital eccentricity and other planetary parameters like mass, orbital periods have been investigated further to find any intrinsic characteristics. Findings: We established that transit method has better chances to discover light and short period candidates. Their orbital eccentricity has been studied w.r.t. their calculated planetary mass and orbital period. We have found eccentricity excitation and tidal circularisation due to low orbital period keeps hot Jupiters at close proximity to their parent stars. Effectively smaller average eccentricity of 0.05 0.5 0 ± 0.008 for intermediate and large hot Jupiters indicates lack of influence of tidal interaction on larger masses. Probability distribution of eccentricity supports the existence of a discontinuity in planetary mass distribution at ~4M J . Low p value (~0.037) in KS test indicates the existence of bimodal distribution of hot Jupiter populations having possibly different channel of formation. Novelty: Application of statistics on hot Jupiters is rare due to their infrequent detection. Already reported planetary parametric features of exoplanets are checked for trueness and new parameters have been studied. Here we also discussed theoretical and empirical implications of these statistical results for dynamical evolution. It opens up a new dimension to scientific realm.

show abstract

Section: Introductionmentioning

confidence: 99%

Observational Evidence of Bimodal Distribution in Hot Jupiter Population

Mondal

2023

IJST

View full text Add to dashboard Cite

show abstract

“…Earlier, we obtained two independent mass distributions for exoplanets discovered by the Kepler Space Telescope by the transit method (Ananyeva et al 2020) (A20 hereafter) and those discovered by the RV method (Ivanova et al 2021) (I20 hereafter). Several important observational selection factors were taken into account in both cases.…”

Section: Introductionmentioning

confidence: 99%

Comparison of the mass distributions of short-period exoplanets detected by transit and RV methods

Yakovlev

Ananyeva

Ivanova

et al. 2021

Monthly Notices of the Royal Astronomical Society: Letters

View full text Add to dashboard Cite

We analyse the causes of a discrepancy between the earlier obtained samples of the mass distributions of exoplanets detected by the transit method and the radial velocity (RV) one and corrected for some observational selection effects. It is found that this discrepancy can be removed by introducing the following restrictions into the procedures forming the samples: (i) to consider, among transit exoplanets, only those which masses were determined by the RV method (i.e. excluding the TTV method); (ii) to take into account exoplanets with orbital periods P ∈ [1, 100] days and masses M ∈ [0.02, 13]MJ (Jupiter masses). In addition, we compare here the distributions by projective masses (which is Msin i, where i is the orbital inclination of an exoplanet). For this, the mass distribution of transit exoplanets is transformed into the projective mass distribution. Due to these three changes in the procedure, the obtained RV and transit distributions exhibit a similar behaviour in an interval of M ∈ [0.02, Mmid]MJ and coincide at M ∈ [Mmid, 13]MJ, where Mmid ≈ 0.17MJ.

show abstract