J/AJ/167/55 Multiple-planet system resonances (Hamer+, 2024)
Kepler-discovered multiple-planet systems near period ratios suggestive of mean-
motion resonances are young.
Hamer J.H., Schlaufman K.C.
<Astron. J., 167, 55 (2024)>
=2024AJ....167...55H 2024AJ....167...55H
ADC_Keywords: Exoplanets; Optical
Keywords: Exoplanet dynamics ; Exoplanet tides ; Exoplanet evolution ;
Exoplanet systems ; Exoplanets ; Stellar ages ; Stellar kinematics ;
Tidal interaction
Abstract:
Before the launch of the Kepler Space Telescope, models of low-mass
planet formation predicted that convergent type I migration would
often produce systems of low-mass planets in low-order mean-motion
resonances. Instead, Kepler discovered that systems of small planets
frequently have period ratios larger than those associated with
mean-motion resonances and rarely have period ratios smaller than
those associated with mean-motion resonances. Both short-timescale
processes related to the formation or early evolution of planetary
systems and long-timescale secular processes have been proposed as
explanations for these observations. Using a thin disk stellar
population's Galactic velocity dispersion as a relative age proxy, we
find that Kepler-discovered multiple-planet systems with at least one
planet pair near a period ratio suggestive of a second-order
mean-motion resonance have a colder Galactic velocity dispersion and
are therefore younger than both single-transiting and multiple-planet
systems that lack planet pairs consistent with mean-motion resonances.
We argue that a nontidal secular process with a characteristic
timescale no less than a few hundred Myr is responsible for moving
systems of low-mass planets away from second-order mean-motion
resonances. Among systems with at least one planet pair near a period
ratio suggestive of a first-order mean-motion resonance, only the
population of systems likely affected by tidal dissipation inside
their innermost planets has a small Galactic velocity dispersion and
is therefore young. We predict that period ratios suggestive of
mean-motion resonances are more common in young systems with
10Myr≲τ≲100Myr and become less common as planetary systems age.
Description:
Our sample includes all confirmed and candidate planets with a
disposition of "P" in the Lissauer+ (2024PSJ.....5..152L 2024PSJ.....5..152L) catalog.
See Section 2.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 91 1319 Separations from resonances in libration widths
table2.dat 141 1340 *Separations from resonance in units of |δ_res|
(Equation 6)
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Note on table2.dat: We define the parameter
|δres|=1/pres(Pout/Pin-pres_)
where and pres=(j+i)/j and i∈(1,2) and Pout/Pin is the ratio
of the outer planet period to the inner planet period.
See Section 3.1.
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See also:
V/133 : Kepler Input Catalog (Kepler Mission Team, 2009)
I/350 : Gaia EDR3 (Gaia Collaboration, 2020)
III/286 : APOGEE-2 DR17 final allStar catalog (Abdurro'uf+, 2022)
J/ApJS/197/8 : Kepler's multiple transiting planets (Lissauer+, 2011)
J/A+A/537/A146 : Stellar models with rot. 0.8<M<120, Z=0.014 (Ekstrom+, 2012)
J/MNRAS/420/L23 : Non-resonant Kepler planetary systems (Veras+, 2012)
J/ApJ/790/146 : Planets in Kepler's multi-transiting syst. (Fabrycky+, 2014)
J/ApJS/215/19 : APOKASC catalog of Kepler red giants (Pinsonneault+, 2014)
J/MNRAS/448/1044 : Simulation data for 50 planetary model syst. (Hansen+, 2015)
J/AJ/151/144 : ASPCAP weights for APOGEE chemical elements (Garcia+, 2016)
J/AJ/154/107 : California-Kepler Survey (CKS). I. (Petigura+, 2017)
J/AJ/154/108 : California-Kepler Survey (CKS). II. (Johnson+, 2017)
J/ApJ/855/115 : Lithium abundances of KOIs from CKS spectra (Berger+, 2018)
J/ApJS/237/38 : Extended abundance analysis of KOIs (Brewer+, 2018)
J/AJ/156/264 : CKS. VII. Planet radius gap (Fulton+, 2018)
J/ApJS/235/38 : Kepler planets. VIII. DR25 reliability (Thompson+, 2018)
J/AJ/158/190 : MS hot Jupiter hosts with good astrometry (Hamer+, 2019)
J/AJ/159/280 : Gaia-Kepler stellar properties cat. I. (Berger+, 2020)
J/AJ/160/138 : Gaia DR2 ultra-short-period planet host stars (Hamer+, 2020)
J/ApJ/909/115 : Planets Across Space and Time (PAST). I. (Chen+, 2021)
J/AJ/162/100 : PAST. II. LAMOST-Gaia-Kepler catalog (Chen+, 2021)
J/A+A/649/A3 : Gaia EDR3 photometric passbands (Riello+, 2021)
J/ApJ/921/24 : Planetary masses and radii (Schlaufman+, 2021)
J/AJ/164/26 : Hot Jupiters isochrone analyse (Hamer+, 2022)
Byte-by-byte Description of file: table1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
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1- 8 I8 --- KIC [1432789/12600735] Kepler Input Catalog
number for host star
10- 16 F7.2 --- KOI-in [41.01/7685.02] Kepler Object of Interest
number assigned to inner planet
18- 24 F7.2 --- KOI-out [41.01/7685.01] Kepler Object of Interest
number assigned to outer planet
26- 30 A5 --- Adjacent Boolean denoting if the two planets are
adjacent
32- 41 F10.5 --- 2:1Dist [0.03/1396] Distance in units of libration
widths from the 2:1 resonance
43- 52 F10.5 --- 3:2Dist [0.096/1355] Distance in units of libration
widths from the 3:2 resonance
54- 63 F10.5 --- 4:3Dist [0.036/1284] Distance in units of libration
widths from the 4:3 resonance
65- 74 F10.5 --- 5:4Dist [0.11/1219] Distance in units of libration
widths from the 5:4 resonance
76- 85 F10.5 --- 6:5Dist [0.057/1170] Distance in units of libration
widths from the 6:5 resonance
87- 91 A5 --- Res Boolean denoting if the two planets are
plausibly first-order resonant
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 8 I8 --- KIC [1432789/12600735] Kepler Input Catalog
number for host star
10- 16 F7.2 --- KOI-in [41.01/7685.02] Kepler Object of Interest
number assigned to inner planet
18- 24 F7.2 --- KOI-out [41.01/7685.01] Kepler Object of Interest
number assigned to outer planet
26- 30 A5 --- Adjacent Boolean denoting if the two planets are
adjacent
32- 40 F9.5 --- 2:1Dist [0.0003/121] Distance in units of |d_res|
from the 2:1 resonance
42- 50 F9.5 --- 3:2Dist [0.00027/162] Distance in units of |d_res|
from the 3:2 resonance
52- 60 F9.5 --- 4:3Dist [0.0002/182] Distance in units of |d_res|
from the 4:3 resonance
62- 70 F9.5 --- 5:4Dist [0.0003/195] Distance in units of |d_res|
from the 5:4 resonance
72- 80 F9.5 --- 6:5Dist [0.0001/203] Distance in units of |d_res|
from the 6:5 resonance
82- 89 F8.5 --- 3:1Dist [0.003/81] Distance in units of |d_res| from
the 3:1 resonance
91- 99 F9.5 --- 5:3Dist [6e-05/146] Distance in units of |d_res| from
the 5:3 resonance
101- 109 F9.5 --- 7:5Dist [0.0027/174] Distance in units of |d_res|
from the 7:5 resonance
111- 119 F9.5 --- 9:7Dist [0.00046/189] Distance in units of |d_res|
from the 9:7 resonance
121- 129 F9.5 --- 11:9Dist [0.002/199] Distance in units of |d_res| from
the 11:9 resonance
131- 135 A5 --- Res1O Boolean denoting if the two planets are
plausibly first-order resonant
137- 141 A5 --- Res2O Boolean denoting if the two planets are
plausibly second-order resonant
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 06-Feb-2025