The Period Distribution of Hot Jupiters Is Not Dependent on Host Star Metallicity

Yee, Samuel W.; Winn, Joshua N.

doi:10.3847/2041-8213/acd552

Cited by 4 publications

(1 citation statement)

References 47 publications

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“…A recent study on host star metallicity of HJs suggested population of HJs formed in a similar process to other gas giants, and may differ only in their migration histories (27) . When we have dug it further with a larger set of samples, no conclusive evidence has been inferred as already reported (28) . It motivated us to cultivate other planetary parameters viz.…”

Section: Formation and Migration Depending On Metallicitymentioning

confidence: 56%

Observational Evidence of Bimodal Distribution in Hot Jupiter Population

Mondal

2023

IJST

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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.

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Section: Formation and Migration Depending On Metallicitymentioning

confidence: 56%

Observational Evidence of Bimodal Distribution in Hot Jupiter Population

Mondal

2023

IJST

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Gas, not dust: Migration of TESS/Gaia hot Jupiters possibly halted by the magnetospheres of protoplanetary disks

Mendigutía,

Lillo-Box,

Vioque

et al. 2024

A&A

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The presence of short-period (< 10 days) planets around main sequence (MS) stars has been associated either with the dust-destruction region or with the magnetospheric gas-truncation radius in the protoplanetary disks that surround them during the pre-MS phase. However, previous analyses have only considered low-mass FGK stars, making it difficult to disentangle the two scenarios. This exploratory study is aimed at testing whether it is the inner dust or gas disk driving the location of short-period, giant planets. By combining TESS and Gaia DR3 data, we identified a sample of 47 intermediate-mass (1.5 -- 3 M$_ odot $) MS stars hosting confirmed and firm candidate hot Jupiters. We compared their orbits with the rough position of the inner dust and gas disks, which are well separated around their Herbig stars precursors. We also made a comparison with the orbits of confirmed hot Jupiters around a similarly extracted TESS/ Gaia sample of low-mass sources (0.5 -- 1.5 M$_ odot The orbits of hot Jupiters around intermediate-mass stars tend to be closer to the central sources than the inner dust disk, most generally consistent with the small magnetospheric truncation radii typical of Herbig stars (lesssim 5R$_*$). A similar study considering the low-mass stars alone has been less conclusive due to the similar spatial scales of their inner dust and gas disks (gtrsim 5R$_*$). However, considering the whole sample, we do not find the correlation between orbit sizes and stellar luminosities that is otherwise expected if the dust-destruction radius limits the hot Jupiters' orbits. On the contrary, the comparative analysis reveals that such orbits tend to be closer to the stellar surface for intermediate-mass stars than for low-mass stars, with both being mostly consistent with the rough sizes of the corresponding magnetospheres. Our results suggest that the inner gas (and not the dust) disk limits the innermost orbits of hot Jupiters around intermediate-mass stars. These findings also provide tentative support to previous works that have claimed this is indeed the case for low-mass sources. We propose that hot Jupiters could be explained via a combination of the core-accretion paradigm and migration up to the gas-truncation radius, which may be responsible for halting inward migration regardless of the stellar mass regime. Larger samples of intermediate-mass stars with hot Jupiters are necessary to confirm our hypothesis, which implies that massive Herbig stars without magnetospheres ($>$ 3-4 M$_ odot $) may be the most efficient in swallowing their newborn planets.

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Revisiting mass–radius relationships for exoplanet populations: a machine learning insight

Mousavi-Sadr,

Jassur,

Gozaliasl

2023

Monthly Notices of the Royal Astronomical Society

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The growing number of exoplanet discoveries and advances in machine learning techniques have opened new avenues for exploring and understanding the characteristics of worlds beyond our Solar system. In this study, we employ efficient machine learning approaches to analyse a data set comprising 762 confirmed exoplanets and eight Solar system planets, aiming to characterize their fundamental quantities. By applying different unsupervised clustering algorithms, we classify the data into two main classes: ‘small’ and ‘giant’ planets, with cut-off values at Rp = 8.13R⊕ and Mp = 52.48M⊕. This classification reveals an intriguing distinction: giant planets have lower densities, suggesting higher H–He mass fractions, while small planets are denser, composed mainly of heavier elements. We apply various regression models to uncover correlations between physical parameters and their predictive power for exoplanet radius. Our analysis highlights that planetary mass, orbital period, and stellar mass play crucial roles in predicting exoplanet radius. Among the models evaluated, the Support Vector Regression consistently outperforms others, demonstrating its promise for obtaining accurate planetary radius estimates. Furthermore, we derive parametric equations using the M5P and Markov Chain Monte Carlo methods. Notably, our study reveals a noteworthy result: small planets exhibit a positive linear mass–radius relation, aligning with previous findings. Conversely, for giant planets, we observe a strong correlation between planetary radius and the mass of their host stars, which might provide intriguing insights into the relationship between giant planet formation and stellar characteristics.

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The Period Distribution of Hot Jupiters Is Not Dependent on Host Star Metallicity

Cited by 4 publications

References 47 publications

Observational Evidence of Bimodal Distribution in Hot Jupiter Population

Observational Evidence of Bimodal Distribution in Hot Jupiter Population

Gas, not dust: Migration of TESS/Gaia hot Jupiters possibly halted by the magnetospheres of protoplanetary disks

Revisiting mass–radius relationships for exoplanet populations: a machine learning insight

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