J/ApJS/197/8 Kepler's candidate multiple transiting planets (Lissauer+, 2011)
Architecture and dynamics of Kepler's candidate multiple transiting planet
systems.
Lissauer J.J., Ragozzine D., Fabrycky D.C., Steffen J.H., Ford E.B.,
Jenkins J.M., Shporer A., Holman M.J., Rowe J.F., Quintana E.V.,
Batalha N.M., Borucki W.J., Bryson S.T., Caldwell D.A., Carter J.A.,
Ciardi D., Dunham E.W., Fortney J.J., Gautier III T.N., Howell S.B.,
Koch D.G., Latham D.W., Marcy G.W., Morehead R.C., Sasselov D.
<Astrophys. J. Suppl. Ser., 197, 8 (2011)>
=2011ApJS..197....8L 2011ApJS..197....8L
ADC_Keywords: Planets ; Stars, double and multiple
Keywords: celestial mechanics - planets and satellites: dynamical evolution and
stability - planets and satellites: fundamental parameters -
planets and satellites: general - planetary systems
Abstract:
About one-third of the ∼1200 transiting planet candidates detected in
the first four months of Kepler data are members of multiple candidate
systems. There are 115 target stars with two candidate transiting
planets, 45 with three, 8 with four, and 1 each with five and six. We
characterize the dynamical properties of these candidate multi-planet
systems. The distribution of observed period ratios shows that the
vast majority of candidate pairs are neither in nor near low-order
mean-motion resonances. Nonetheless, there are small but statistically
significant excesses of candidate pairs both in resonance and spaced
slightly too far apart to be in resonance, particularly near the 2:1
resonance. We find that virtually all candidate systems are stable, as
tested by numerical integrations that assume a nominal mass-radius
relationship. Several considerations strongly suggest that the vast
majority of these multi-candidate systems are true planetary systems.
We provide constraints on the true multiplicity and mutual inclination
distribution of the multi-candidate systems, revealing a population of
systems with multiple super-Earth-size and Neptune-size planets with
low to moderate mutual inclinations.
Description:
Our analysis is based on the data presented by Borucki et al. (2011,
Cat. J/ApJ/736/19).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 31 115 Characteristics of systems with two transiting
planets
table2.dat 52 45 Characteristics of systems with three transiting
planets
table3.dat 71 8 Characteristics of systems with four transiting
planets
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See also:
V/133 : Kepler Input Catalog (Kepler Mission Team, 2009)
J/ApJ/736/19 : Kepler planetary candidates. II. (Borucki+, 2011)
J/ApJ/728/117 : Kepler planetary candidates. I. (Borucki+, 2011)
J/ApJS/197/2 : Transit timing observations from Kepler. I. (Ford+, 2011)
J/A+A/529/A89 : Kepler satellite variability study (Debosscher+, 2011)
J/A+A/517/A3 : Stellar parameters of Kepler early-type targets (Catanzaro+,
2010)
Byte-by-byte Description of file: table1.dat table2.dat table3.dat
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Bytes Format Units Label Explanations
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1- 4 I4 --- KOI Kepler Object Identification number
6- 10 F5.2 --- Rp1 Planet 1 radius in R⊕ (1)
12- 16 F5.2 --- Rp2 Planet 2 radius in R⊕ (1)
18- 26 F9.6 --- P2/P1 Period ratio P2/P1
28- 31 F4.1 --- Del1_2 Nominal dynamical separation Δ1,2 (2)
33- 37 F5.2 --- Rp3 ? Planet 3 radius in R⊕
(not for table 1) (1)
39- 47 F9.6 --- P3/P2 ? Period ratio P3/P2 (not for table 1)
49- 52 F4.1 --- Del2_3 ? Nominal dynamical separation Δ2,3
(not for table 1) (2)
54- 57 F4.2 --- Rp4 ? Planet 4 radius in R⊕
(only for table 3) (1)
59- 66 F8.6 --- P4/P3 ? Period ratio P4/P3 (only for table 3)
68- 71 F4.1 --- Del3_4 ? Nominal dynamical separation Δ3,4
(only for table 3) (2)
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Note (1): Planet indices given in these tables signify orbit order, with
one being the planet with the shortest period. These do not always
correspond to the post-decimal point portion (.01,.02, etc.) of the
KOI number designation of these candidates given in Borucki et al.,
2011, Cat. J/ApJ/736/19, for which the numbers signify the order in
which the candidates were identified.
Note (2): the dynamical separation is the difference of the orbital
semi-major axes (ai+1-ai) if the semi-major axes are measured in
units of their mutual Hill sphere radius
Rh=[(Mi+Mj)/(3M*)]1/3.(ai+aj)/2
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History:
From electronic version of the journal
(End) Emmanuelle Perret [CDS] 05-Dec-2011