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 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:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 73 939 Characteristics of Planets in Systems with
Multiple Transiting Planets
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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
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Bytes Format Units Label Explanations
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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)
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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.
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History:
From electronic version of the journal
References:
Lissauer et al., Paper I, 2011Natur.470...53L 2011Natur.470...53L
(End) Prepared by [AAS], Tiphaine Pouvreau [CDS] 22-Mar-2017