MASSES, RADII, AND ORBITS OF SMALL KEPLER PLANETS: THE TRANSITION FROM GASEOUS TO ROCKY PLANETS
Name
Marcy-2014-MASSES, RADII, AND O.pdf
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10.79 MB
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Checksum (MD5)
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Author(s)
Seager, Sara
Winn, Joshua Nathan
Sanchis Ojeda, Roberto
Carter, Joshua Adam
Date Issued
January 2014
Journal
The Astrophysical Journal. Supplement Series
Publisher
IOP Publishing
Citation
Marcy, Geoffrey W., Howard Isaacson, Andrew W. Howard, Jason F. Rowe, Jon M. Jenkins, Stephen T. Bryson, David W. Latham, et al. “MASSES, RADII, AND ORBITS OF SMALL KEPLER PLANETS: THE TRANSITION FROM GASEOUS TO ROCKY PLANETS.” The Astrophysical Journal Supplement Series 210, no. 2 (January 13, 2014): 20. © 2014 The American Astronomical Society
Version
Final published version
Abstract
We report on the masses, sizes, and orbits of the planets orbiting 22 Kepler stars. There are 49 planet candidates around these stars, including 42 detected through transits and 7 revealed by precise Doppler measurements of the host stars. Based on an analysis of the Kepler brightness measurements, along with high-resolution imaging and spectroscopy, Doppler spectroscopy, and (for 11 stars) asteroseismology, we establish low false-positive probabilities (FPPs) for all of the transiting planets (41 of 42 have an FPP under 1%), and we constrain their sizes and masses. Most of the transiting planets are smaller than three times the size of Earth. For 16 planets, the Doppler signal was securely detected, providing a direct measurement of the planet's mass. For the other 26 planets we provide either marginal mass measurements or upper limits to their masses and densities; in many cases we can rule out a rocky composition. We identify six planets with densities above 5 g cm[superscript –3], suggesting a mostly rocky interior for them. Indeed, the only planets that are compatible with a purely rocky composition are smaller than ~2 R [subscript ⊕]. Larger planets evidently contain a larger fraction of low-density material (H, He, and H[subscript 2]O).
MIT Department
Massachusetts Institute of Technology. Department of Earth, Atmospheric, and Planetary Sciences
Massachusetts Institute of Technology. Department of Physics
MIT Kavli Institute for Astrophysics and Space Research
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DOI of Published Version
https://doi.org/10.1088/0067-0049/210/2/20
