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Cited by 249Stellar, planetary, and galactic studiesAstronomy and Astrophysical ResearchHistory and Developments in Astronomy

A STUDY OF THE SHORTEST-PERIOD PLANETS FOUND WITH KEPLER

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Sanchis-Ojeda, Roberto, Rappaport, Saul, Winn, Joshua N., Kotson, Michael C., Levine, Alan, Mellah, Ileyk El·2014·The Astrophysical Journal
DOI 10.1088/0004-637x/787/1/47
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Abstract

We present the results of a survey aimed at discovering and studying transiting planets with orbital periods shorter than one day (ultra-short-period, or USP, planets), using data from the Kepler spacecraft. We computed Fourier transforms of the photometric time series for all 200,000 target stars, and detected transit signals based on the presence of regularly spaced sharp peaks in the Fourier spectrum. We present a list of 106 USP candidates, of which 18 have not previously been described in the literature. This list of candidates increases the number of planet candidates with orbital periods shorter than about six hours from two to seven. In addition, among the objects we studied, there are 26 USP candidates that had been previously reported in the literature which do not pass our various tests. All 106 of our candidates have passed several standard tests to rule out false positives due to eclipsing stellar systems. A low false positive rate is also implied by the relatively high fraction of candidates for which more than one transiting planet signal was detected. By assuming these multi-transit candidates represent coplanar multi-planet systems, we are able to infer that the USP planets are typically accompanied by other planets with periods in the range 1–50 days, in contrast with hot Jupiters which very rarely have companions in that same period range. Another clear pattern is that almost all USP planets are smaller than 2 R ⊕ , possibly because gas giants in very tight orbits would lose their atmospheres by photoevaporation when subject to extremely strong stellar irradiation. Based on our survey statistics, USP planets exist around approximately (0.51 ± 0.07)% of G-dwarf stars, and (0.83 ± 0.18)% of K-dwarf stars.

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Crossref · 10.1088/0004-637x/787/1/47

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  • The majority of USPs greater than 0.84 R⊕ are Earths (0.84-1.25 R⊕), rather than super-Earths.

    “the majority of these USPs are Earths (0.84-1.25 R ⊕ ), rather than super-Earths.”

    From Origins of Hot Jupiters (2018) · cites this paper as Sanchis-Ojeda et al. 2014

    Section 6.2 (page unavailable) reports that Earth-size USPs are more common than larger planet types and describes a modest excess over super-Earths. It does not establish that Earths make up a majority of all USPs above 0.84 R⊕ or specify the claimed 0.84–1.25 R⊕ range. (LLM, conf=0.84)

    Experimental — accuracy not yet measured

  • The overall occurrence rate of USPs is 0.5% for USPs greater than 0.84 R⊕.

    “The overall occurrence rate of USPs is 0.5% for USPs greater than 0.84 R ⊕ (Sanchis-Ojeda et al. 2014);”

    From Origins of Hot Jupiters (2018) · cites this paper as Sanchis-Ojeda et al. 2014

    Section 6.2 (page unavailable) reports 5.5 ± 0.5 USP planets per thousand stars—approximately 0.5%—for radii greater than 0.84 R⊕. But that estimate is specifically for G and K dwarfs, a population restriction the citing sentence omits. (LLM, conf=0.86)

    Experimental — accuracy not yet measured

  • Most USPs are likely not tidally stripped Jupiters because they reside in compact multi-planet systems and lack hot Jupiters' host star metallicity dependence.

    “However, most USPs are likely not tidally stripped Jupiters because, unlike most hot Jupiters, they reside in in compact multi-planet systems (Sanchis-Ojeda et al. 2014) and they lack hot Jupiters' host star metallicity dependence (Winn et al. 2017b).”

    From Origins of Hot Jupiters (2018) · cites this paper as Sanchis-Ojeda et al. 2014

  • USPs tend to reside in compact multi-planet systems.

    “USPS tend reside in compact multi-planet systems (SanchisOjeda et al. 2014).”

    From Origins of Hot Jupiters (2018) · cites this paper as Sanchis-Ojeda et al. 2014

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Cited by

Sorted by citations

Authors
Sanchis-Ojeda, R., Rappaport, S., Winn, J. N., Kotson, M. C., Levine, A., & Mellah, I. E.
Affiliations
  • Massachusetts Institute of Technology (US)
  • University of Hawaiʻi at Mānoa (US)
  • Laboratoire AstroParticule et Cosmologie (FR)
ORCID
Venue
The Astrophysical Journal
Publisher
American Astronomical Society
Published
2014-05-02
Volume
787
Issue
1
Pages
47
ISSN
  • 0004-637X (ISSN-L)
  • 1538-4357
DOI
10.1088/0004-637x/787/1/47
OpenAlex
W1602052939
Cited by
249
References
4
Citations by year
2026: 7 · 2025: 25 · 2024: 18 · 2023: 15 · 2022: 17 · 2021: 24 · 2020: 20 · 2019: 22 · 2018: 42 · 2017: 26 · 2016: 11 · 2015: 17 · 2014: 4
FWCI
10.42
Type
journal article
Language
en
Open access
Licence
Locations
  • The Astrophysical Journal (publishedVersion)
  • arXiv (Cornell University) (submittedVersion)
  • arXiv (Cornell University)
Funders
  • National Aeronautics and Space Administration (NNX09AF08G, NAS 526555)
  • California Institute of Technology
  • Space Telescope Science Institute (NAS5- 26555, 26555)
  • Science and Technology Facilities Council
Topics
  • Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Stellar, planetary, and galactic studies
  • Physical Sciences › Physics and Astronomy › Instrumentation › Astronomy and Astrophysical Research
  • Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › History and Developments in Astronomy
Keywords
ultra-short-period planets, transiting exoplanets, Kepler mission, false positive rejection, multi-planet systems, planet occurrence rate, G dwarfs, K dwarfs, photoevaporation, hot Jupiters

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