Architecture of Kepler's Multi-transiting Systems. II. New Investigations with Twice as Many Candidates
- Creators
- Fabrycky, Daniel C.
- Lissauer, Jack J.
- Ragozzine, Darin
- Rowe, Jason F.
- Steffen, Jason H.
- Agol, Eric
- Barclay, Thomas
- Batalha, Natalie
- Borucki, William
- Ciardi, David R.
- Ford, Eric B.
- Gautier, Thomas N.
- Geary, John C.
- Holman, Matthew J.
- Jenkins, Jon M.
- Li, Jie
- Morehead, Robert C.
- Morris, Robert L.
- Shporer, Avi
- Smith, Jeffrey C.
- Still, Martin
- van Cleve, Jeffrey
Abstract
We report on the orbital architectures of Kepler systems having multiple-planet candidates identified in the analysis of data from the first six quarters of Kepler data and reported by Batalha et al. (2013). These data show 899 transiting planet candidates in 365 multiple-planet systems and provide a powerful means to study the statistical properties of planetary systems. Using a generic mass–radius relationship, we find that only two pairs of planets in these candidate systems (out of 761 pairs total) appear to be on Hill-unstable orbits, indicating ~96% of the candidate planetary systems are correctly interpreted as true systems. We find that planet pairs show little statistical preference to be near mean-motion resonances. We identify an asymmetry in the distribution of period ratios near first-order resonances (e.g., 2:1, 3:2), with an excess of planet pairs lying wide of resonance and relatively few lying narrow of resonance. Finally, based upon the transit duration ratios of adjacent planets in each system, we find that the interior planet tends to have a smaller transit impact parameter than the exterior planet does. This finding suggests that the mode of the mutual inclinations of planetary orbital planes is in the range 1°.0–2°.2, for the packed systems of small planets probed by these observations.
Additional Information
© 2014 The American Astronomical Society. Received 2012 February 28; accepted 2014 June 9; published 2014 July 16. Funding for this mission is provided by NASA's Science Mission Directorate. We thank the entire Kepler team for the many years of work that is making the Kepler mission so successful. We thank Emily Fabrycky, Doug Lin, Man-Hoi Lee, Scott Tremaine, and TseviMazeh for helpful conversations and insightful comments. D.C.F. acknowledges support for this work was provided by NASA through Hubble Fellowship grant No. HF-51272.01-A awarded by the Space Telescope Science Institute,which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. E.A.was supported byNSF Career grant 0645416. E.B.F acknowledges support by the National Aeronautics and Space Administration under grant NNX08AR04G issued through the Kepler Participating Scientist Program, and the Center for Exoplanets and Habitable Worlds, which is supported by the Pennsylvania State University, the Eberly College of Science, and the Pennsylvania Space Grant Consortium. This material is based upon work supported by the National Science Foundation under grant No. 0707203. R.C.M. was support by the National Science Foundation Graduate Research Fellowship under grant No. DGE-0802270. Facilities: KeplerAttached Files
Published - 0004-637X_790_2_146.pdf
Submitted - 1202.6328v3.pdf
Files
Name | Size | Download all |
---|---|---|
md5:50f8425748b0491bd87a7e338dac8736
|
569.1 kB | Preview Download |
md5:0d4badca157293338caa7471b5e52a3f
|
676.7 kB | Preview Download |
Additional details
- Eprint ID
- 48599
- Resolver ID
- CaltechAUTHORS:20140815-092737225
- HF-51272.01-A
- NASA Hubble Fellowship
- NAS 5-26555
- NASA
- AST-0645416
- NSF
- NNX08AR04G
- NASA
- AST-0707203
- NSF
- DGE-0802270
- NSF Graduate Research Fellowship
- Created
-
2014-08-15Created from EPrint's datestamp field
- Updated
-
2021-11-10Created from EPrint's last_modified field
- Caltech groups
- Infrared Processing and Analysis Center (IPAC)