On the Occurrence Rate of Hot Jupiters in Different Stellar Environments

Ji, Wang; Fischer, Debra A.; Horch, Elliott; Huang, Chelsea X.

doi:10.1088/0004-637x/799/2/229

Cited by 95 publications

(62 citation statements)

References 50 publications

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“…The fraction of single stars with hot Jupiters (P < 10 days) is 1.2% ± 0.38% from the Doppler sample of Wright et al (2012) and 0.6% ± 0.1% from the Kepler photometric sample (Wang et al 2015b). The difference is mainly due to different stellar types.…”

Section: Limits To the Occurence Rate Of Circumbinary Planetsmentioning

confidence: 96%

Limits to the presence of transiting circumbinary planets in CoRoT Data

Klagyivik

Deeg

Cabrera

et al. 2017

A&A

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Aims. The CoRoT mission during its flight-phase 2007-2012 delivered the light-curves for over 2000 eclipsing binaries. Data from the Kepler mission have proven the existence of several transiting circumbinary planets. Albeit light-curves from CoRoT have typically lower precision and shorter coverage, CoRoT's number of targets is similar to Kepler, and some of the known circumbinary planets could potentially be detected in CoRoT data as well. The aim of this work has been a revision of the entire CoRoT data-set for the presence of circumbinary planets, and the derivation of limits to the abundances of such planets. Methods. We developed a code which removes the light curve of the eclipsing binaries and searches for quasi-periodic transit-like features in a light curve after removal of binary eclipses and instrumental features. The code needs little information on the sample systems and can be used for other space missions as well, like Kepler, K2, TESS and PLATO. The code is broad in the requirements leading to detections, but was tuned to deliver an amount of detections that is manageable in a subsequent, mainly visual, revision about their nature. Results. In the CoRoT sample we identified three planet candidates whose transits would have arisen from a single pass across the central binary. No candidates remained however with transit events from multiple planetary orbits. We calculated the upper limits for the number of Jupiter, Saturn and Neptune sized planets in co-planar orbits for different orbital period ranges. We found that there are much less giant planets in short-periodic orbits around close binary systems than around single stars.

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Section: Limits To the Occurence Rate Of Circumbinary Planetsmentioning

confidence: 96%

Limits to the presence of transiting circumbinary planets in CoRoT Data

Klagyivik

Deeg

Cabrera

et al. 2017

A&A

View full text Add to dashboard Cite

show abstract

“…Such differences could be caused by the requirement for long-term dynamical stability, or differences in the planet formation process. When the search sample includes both singles and binaries, the detected planets are thereby drawn from different occurrence distributions (see Wang et al 2015a;Kraus et al 2016).…”

Section: Understanding the Errorsmentioning

confidence: 99%

Biases in Planet Occurrence Caused by Unresolved Binaries in Transit Surveys

Bouma

Masuda

Winn

2018

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Wide-field surveys for transiting planets, such as the NASA Kepler and TESS missions, are usually conducted without knowing which stars have binary companions. Unresolved and unrecognized binaries give rise to systematic errors in planet occurrence rates, including misclassified planets and mistakes in completeness corrections. The individual errors can have different signs, making it difficult to anticipate the net effect on inferred occurrence rates. Here we use simplified models of signal-to-noise limited transit surveys to try and clarify the situation. We derive a formula for the apparent occurrence rate density measured by an observer who falsely assumes all stars are single. The formula depends on the binary fraction; the mass function of the secondary stars; and the true occurrence of planets around primaries, secondaries, and single stars. It also takes into account the Malmquist bias by which binaries are over-represented in flux-limited samples. Application of the formula to an idealized Kepler-like survey shows that for planets larger than 2 R ⊕ , the net systematic error is of order 5%. In particular, unrecognized binaries are unlikely to be the reason for the apparent discrepancies between hot Jupiter occurrence rates measured in different surveys. For smaller planets the errors are potentially larger: the occurrence of Earth-sized planets could be overestimated by as much as 50%. We also show that whenever high-resolution imaging reveals a transit host star to be a binary, the planet is usually more likely to orbit the primary star than the secondary star.

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“…There is a geometric bias toward shorter orbital periods (e.g., the geometric probability of transit scales as a −1 ), transits can be missed due to the rotation of the Earth, three transits are often required to confirm a planet which biases against long-period planets (with respect to the observing baseline), and the stellar demographics may differ from those of RV surveys (Wang et al 2015, and Figure 2). …”

Section: Datamentioning

confidence: 99%

Evidence for Two Hot-Jupiter Formation Paths

Nelson¹,

Rasio²

2017

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Disk migration and high-eccentricity migration are two well-studied theories to explain the formation of hot Jupiters. The former predicts that these planets can migrate up until the planet-star Roche separation (a Roche ) and the latter predicts they will tidally circularize at a minimum distance of 2a Roche . Considering long-running radial velocity and transit surveys have identified a couple hundred hot Jupiters to date, we can revisit the classic question of hot Jupiter formation in a data-driven manner. We approach this problem using data from several exoplanet surveys (radial velocity, Kepler, HAT, and WASP) allowing for either a single population or a mixture of populations associated with these formation channels, and applying a hierarchical Bayesian mixture model of truncated power laws of the form x γ−1 to constrain the population-level parameters of interest (e.g., location of inner edges, γ, mixture fractions). Within the limitations of our chosen models, we find the current radial velocity and Kepler sample of hot Jupiters can be well explained with a single truncated power law distribution with a lower cutoff near 2a Roche , a result that still holds after a decade, and γ = −0.51± 0.19 0.20 . However, the HAT and WASP data show evidence for multiple populations (Bayes factor ≈ 10 21 ). We find that 15 ± 9 6 % reside in a component consistent with disk migration (γ = −0.04± 0.53 1.27 ) and 85 ± 6 9 % in one consistent with high-eccentricity migration (γ = −1.38± 0.32 0.47 ). We find no immediately strong connections with some observed host star properties and speculate on how future exoplanet surveys could improve upon hot Jupiter population inference.

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On the Occurrence Rate of Hot Jupiters in Different Stellar Environments

Cited by 95 publications

References 50 publications

Limits to the presence of transiting circumbinary planets in CoRoT Data

Limits to the presence of transiting circumbinary planets in CoRoT Data

Biases in Planet Occurrence Caused by Unresolved Binaries in Transit Surveys

Evidence for Two Hot-Jupiter Formation Paths

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