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J/ApJ/790/146    Planets in Kepler's multi-transiting systems  (Fabrycky+, 2014)

Architecture of Kepler's multi-transiting systems. II. New investigations with twice as many candidates. Fabrycky D.C., Lissauer J.J., Ragozzine D., Rowe J.F., Steffen J.H., Agol E., Barclay T., Batalha N., Borucki W., Ciardi D.R., Ford E.B., Gautier T.N., Geary J.C., Holman M.J., Jenkins J.M., Li J., Morehead R.C., Morris R.L., Shporer A., Smith J.C., Still M., Van Cleve J. <Astrophys. J., 790, 146 (2014)> =2014ApJ...790..146F (SIMBAD/NED BibCode)
ADC_Keywords: Stars, double and multiple ; Planets ; Ephemerides ; Stars, masses ; Stars, diameters Keywords: methods: statistical - planetary systems - planets and satellites: detection - planets and satellites: dynamical evolution and stability 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, J/ApJS/204/24). 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. Description: Our sample of planet candidates is based on the Kepler object of interest (KOI) list in the Appendix by Batalha et al. 2013, J/ApJS/204/24) (Table 9). System numbers are denoted by the integer part, and individual planets within these systems are denoted by the decimal part, of KOI numbers. To study these systems' dynamics, we adopt stellar masses obtained from the surface gravity (its logarithm is denoted log g) and stellar radius reported by Batalha et al. 2013, J/ApJS/204/24. The planet candidate systems are 1409 targets with a single candidate, 243 double systems, 85 triple systems, 28 quadruple systems, 8 quintuple systems, and 1 sextuple system. This implies a total of 365 candidate multiple-planet systems with 899 candidate planets. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 73 939 Characteristics of Planets in Systems with Multiple Transiting Planets
See also: V/133 : Kepler Input Catalog (Kepler Mission Team, 2009) J/ApJS/197/2 : Transit timing observations from Kepler. I. (Ford+, 2011) J/ApJS/204/24 : Kepler planetary candidates. III. (Batalha+, 2013) J/ApJ/821/47 : KOI transit probabilities of multi-planet syst. (Brakensiek+, 2016) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 8 F8.2 --- KOI Kelper Object of Interest identifier (1) 10- 19 F10.6 d Period Orbital period 21- 29 F9.5 d T0 Barycentric Julian Date of minimum; BJD-2454900.0 31- 37 F7.4 h Tdur Eclipse duration 39- 43 F5.2 Rgeo Rp Planetary radius; Earth radii 45- 49 F5.1 --- S/N Signal-to-Noise 51- 54 F4.2 Msun M* Stellar mass 56- 59 F4.2 Rsun R* Stellar radius 61- 68 F8.5 --- P/P- ? Ratio of orbital periods (2) 70- 73 F4.1 --- Delta- ? Orbital separation (3)
Note (1): Systems (integer part of KOI numbers) ordered by increasing multiplicity, then numerically. Within each system, planets are ordered by increasing orbital period. The decimal part of KOI numbers (".01", ".02", etc.) refers to the order of discovery. Note (2): Between this planet and the adjacent planet with a smaller period. Note (3): Between this planet and the adjacent planet with a smaller period. In units of Hill radii, see Equ. 3.
History: From electronic version of the journal References: Lissauer et al., Paper I, 2011Natur.470...53L
(End) Prepared by [AAS], Tiphaine Pouvreau [CDS] 22-Mar-2017
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