Cited by 302Stellar, planetary, and galactic studiesAstro and Planetary ScienceHistory and Developments in Astronomy

THE MASS OF KOI-94d AND A RELATION FOR PLANET RADIUS, MASS, AND INCIDENT FLUX

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Weiss, Lauren M., Marcy, Geoffrey W., Rowe, Jason F., Howard, Andrew W., Isaacson, Howard, Fortney, Jonathan J., Miller, Neil, Demory, Brice-Olivier +10 more·2013·The Astrophysical Journal

Abstract

We measure the mass of a modestly irradiated giant planet, KOI-94d. We wish to determine whether this planet, which is in a 22 day orbit and receives 2700 times as much incident flux as Jupiter, is as dense as Jupiter or rarefied like inflated hot Jupiters. KOI-94 also hosts at least three smaller transiting planets, all of which were detected by the Kepler mission. With 26 radial velocities of KOI-94 from the W. M. Keck Observatory and a simultaneous fit to the Kepler light curve, we measure the mass of the giant planet and determine that it is not inflated. Support for the planetary interpretation of the other three candidates comes from gravitational interactions through transit timing variations, the statistical robustness of multi-planet systems against false positives, and several lines of evidence that no other star resides within the photometric aperture. We report the properties of KOI-94b ( M P = 10.5 ± 4.6 M ⊕ , R P = 1.71 ± 0.16 R ⊕ , P = 3.74 days), KOI-94c ( M P = M ⊕ , R P = 4.32 ± 0.41 R ⊕ , P = 10.4 days), KOI-94d ( M P = 106 ± 11 M ⊕ , R P = 11.27 ± 1.06 R ⊕ , P = 22.3 days), and KOI-94e ( M P = M ⊕ , R P = 6.56 ± 0.62 R ⊕ , P = 54.3 days). The radial velocity analyses of KOI-94b and KOI-94e offer marginal (>2σ) mass detections, whereas the observations of KOI-94c offer only an upper limit to its mass. Using the KOI-94 system and other planets with published values for both mass and radius (138 exoplanets total, including 35 with M P < 150 M ⊕ ), we establish two fundamental planes for exoplanets that relate their mass, incident flux, and radius from a few Earth masses up to 13 Jupiter masses: ( R P / R ⊕ ) = 1.78( M P / M ⊕ ) 0.53 ( F /erg s −1 cm −2 ) −0.03 for M P < 150 M ⊕ , and R P / R ⊕ = 2.45( M P / M ⊕ ) −0.039 ( F /erg s −1 cm −2 ) 0.094 for M P > 150 M ⊕ . These equations can be used to predict the radius or mass of a planet.

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  • Hot Jupiter radii are observed to be strongly correlated with stellar flux, supporting the interpretation that one or more stellar irradiation deposition mechanisms plays a role.

    “Hot Jupiter radii are observed to be strongly correlated with stellar flux (e.g., Weiss et al. 2013), supporting the interpretation that one or more stellar irradiation deposition mechanisms plays a role.”

    From Origins of Hot Jupiters (2018) · cites this paper as Weiss et al. 2013

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Authors
Weiss, L. M., Marcy, G. W., Rowe, J. F., Howard, A. W., Isaacson, H., Fortney, J. J., Miller, N., Demory, B.-O., Fischer, D. A., Adams, E. R., Dupree, A. K., Howell, S. B., Kolbl, R., Johnson, J. A., Horch, E. P., Everett, M. E., Fabrycky, D. C., & Seager, S.
Affiliations
  • University of California, Berkeley (US)
  • Ames Research Center (US)
  • University of Hawaiʻi at Mānoa (US)
  • University of California, Santa Cruz (US)
  • Massachusetts Institute of Technology (US)
  • Yale University (US)
  • Center for Astrophysics Harvard & Smithsonian (US)
  • California Institute of Technology (US)
  • Southern Connecticut State University (US)
  • University of Chicago (US)
Corresponding author
Weiss, Lauren M.
Venue
The Astrophysical Journal
Published
2013-04-09
Volume
768
Issue
1
Pages
14
ISSN
  • 0004-637X (ISSN-L)
  • 1538-4357
OpenAlex
W2107596287
Cited by
302
References
7
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FWCI
19.08
Type
journal article
Language
en
Open access
Locations
  • The Astrophysical Journal (publishedVersion)
  • arXiv (Cornell University) (submittedVersion)
  • CaltechAUTHORS (California Institute of Technology) (submittedVersion)
  • Bern Open Repository and Information System (University of Bern) (submittedVersion, other-oa)
  • DSpace@MIT (Massachusetts Institute of Technology) (submittedVersion, cc-by-nc-sa)
  • arXiv (Cornell University)
  • Open Access CRIS of the University of Bern
Funders
  • National Science Foundation (1106400)
  • California Institute of Technology
Topics
  • Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Stellar, planetary, and galactic studies
  • Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Astro and Planetary Science
  • Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › History and Developments in Astronomy
Keywords
exoplanet masses, planetary radius, incident flux, fundamental plane, hot Jupiters, radial velocity, transit timing variations, multi-planet systems, false positives, Kepler light curves, transiting exoplanets

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