J/AJ/167/271 List of 213 planetary systems architectures (Volk+, 2024)
Differences between Stable and Unstable Architectures of Compact Planetary
Systems.
Volk K., Malhotra R.
<Astron. J., 167, 271 (2024)>
=2024AJ....167..271V 2024AJ....167..271V
ADC_Keywords: Exoplanets; Stars, double and multiple
Keywords: Exoplanets ; Exoplanet dynamics ; Exoplanet systems ; Orbital
evolution
Abstract:
We present a stability analysis of a large set of simulated planetary
systems of three or more planets based on architectures of multiplanet
systems discovered by Kepler and K2. We propagated 21400 simulated
planetary systems up to 5 billion orbits of the innermost planet;
approximately 13% of these simulations ended in a planet-planet
collision within that time span. We examined trends in dynamical
stability based on dynamical spacings, orbital period ratios, and mass
ratios of nearest-neighbor planets as well as the system-wide planet
mass distribution and the spectral fraction describing the system's
short-term evolution. We find that instability is more likely in
planetary systems with adjacent planet pairs that have period ratios
less than 2 and in systems of greater variance of planet masses.
Systems with planet pairs at very small dynamical spacings (less than
∼10-12 mutual Hill radii) are also prone to instabilities, but
instabilities also occur at much larger planetary separations. We find
that a large spectral fraction (calculated from short integrations) is
a reasonable predictor of longer-term dynamical instability; systems
that have a large number of Fourier components in their eccentricity
vectors are prone to secular chaos and subsequent eccentricity growth
and instabilities.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 380 213 *List of system architectures in this work
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Note on table2.dat: In all cases except one (Kepler-271; see notes for
that system), the orbital periods for all planets were taken to be the
default value and uncertainties in the Exoplanet Archive composite
planet table
(http://exoplanetarchive.ipac.caltech.edu/cgi-bin/TblView/
nph-tblView?app=ExoTbls&config=PSCompPars). In almost all cases, the
orbital periods for each planet from different lightcurve analyses
agree within uncertainties. Unless otherwise indicated in the notes
column, inclinations and eccentricities for all planets were assigned
from the Rayleigh distributions described in Section 2. MR masses are
generated from the statistical mass-radius relationship from Wolfgang
et al. (2016) for planets with radii of 4REarth or smaller. For
planets exceeding that size limit, we either use a TTV/RV mass
measurement (indicated in the notes column) or we use the mass and
uncertainty given in the Exoplanet Archive Composite data table, which
is based on the mass-radius relationship from Chen & Kipping (2017),
see http://exoplanetarchive.ipac.caltech.edu/docs/composite_calc.html.
For systems where we used this mass estimate, the specific planet is
indicated in the notes column as coming from an alternate MR
relationship.
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See also:
J/ApJS/197/8 : Keplers candidate multiple transiting planet (Lissauer+, 2011)
J/ApJ/750/114 : Kepler TTVs. IV. 4 multiple-planet systems (Fabrycky+, 2012)
J/ApJ/750/113 : Kepler TTVs. II. Confirmed multiplanet systems (Ford+, 2012)
J/ApJS/204/24 : Kepler planetary candidates. III. (Batalha+, 2013)
J/ApJ/767/127 : Asteroseismic solutions for 77 Kepler stars (Huber+, 2013)
J/ApJS/208/22 : Transit timing variation for 12 planetary pairs (Xie, 2013)
J/ApJ/790/146 : Planets in Kepler's multi-transiting systems (Fabrycky+, 2014)
J/ApJ/787/80 : 139 Kepler planets transit time variations (Hadden+, 2014)
J/ApJS/210/20 : Small Kepler planets radial velocities (Marcy+, 2014)
J/ApJ/784/45 : Kepler's multiple planet candidates. III. (Rowe+, 2014)
J/ApJ/795/167 : Transits of PH3 b, c, & d through January 19 (Schmitt+, 2014)
J/ApJ/783/4 : Properties Kepler multi-planet candidate systems (Wang+, 2014)
J/ApJS/210/25 : Transit timing variation for 15 planetary pairs II (Xie, 2014)
J/MNRAS/452/2127 : Fundamental parameters Kepler stars (Silva Aguirre+, 2015)
J/AJ/152/160 : HARPS-N radial velocities of KOI-70 (Buchhave+, 2016)
J/AJ/152/105 : Kepler-80 transit timing observations (MacDonald+, 2016)
J/A+A/587/A64 : Physical properties of giant exoplanets (Santerne+, 2016)
J/ApJ/834/17 : Mass & radius of planets, moons, low mass stars (Chen+, 2017)
J/AJ/154/207 : K2 planetary systems orbiting low-mass stars (Dressing+, 2017)
J/AJ/154/5 : Transit timing variations 145 Kepler planets (Hadden+, 2017)
J/AJ/153/136 : Planets & host stars with Gaia parallaxes (Stassun+, 2017)
J/ApJ/866/99 : Radii of KIC stars & planets using Gaia DR2 (Berger+, 2018)
J/A+A/615/A69 : K2-3 system characterized with HARPSN & HARPS (Damasso+, 2018)
J/AJ/155/136 : Planets orbiting bright stars K2 campaigns 0-10 (Mayo+, 2018)
J/A+A/628/A108 : Photometry of Kepler-82b and c transits (Freudenthal+, 2019)
J/AJ/157/97 : Radial velocity measurements K2-3 & GJ3470 (Kosiarek+, 2019)
J/A+A/631/A90 : K2-138 HARPS radial velocities (Lopez+, 2019)
J/AJ/157/145 : HIRES RVs of three compact, multiplanet systems (Mills+, 2019)
J/A+A/624/A15 : Kepler-411 mid-transit times (Sun+, 2019)
J/A+A/640/A48 : K2-32 and K2-233 light and RV curves (Lillo-Box+, 2020)
J/AJ/159/2 : K2-19b & c transit times & radial velocities (Petigura+, 2020)
J/AJ/161/246 : Transit time variations 12 exoplanets (Jontof-Hutter+, 2021)
J/A+A/670/A68 : Architecture of exoplanetary systems (Mishra+, 2023)
Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 11 A11 --- Name System name
13- 13 I1 --- Npl [3/8] Number of planets in simulation
15- 15 A1 --- f_Npl Flag on Npl (1)
17- 19 I3 --- Num [0/100] Number of unstable simulations
21- 21 I1 --- MMR [0/2]? Mean Motion Resonances (2)
23-380 A358 --- notes Additional notes (3)
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Note (1): Flag as follows:
* = At least one additional planet was detected in that system since its
data was queried for the initial set of simulations. In these cases
the system has a second entry in the table/simulation set with the
additional planet included. (3 occurrences)
Note (2): MMR as follows:
0 = no planets are near strong MMRs (mean motion resonances);
1 = one or more pair of planets is in or very close to a strong MMR;
2 = one or more pair of planets is close enough to a strong MMR that
resonant interactions cannot entirely be ruled out (especially if
simulated planets evolve to large eccentricities).
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Cabrera et al. (2014) = 2014ApJ...781...18C 2014ApJ...781...18C
Shallue & Vanderburg (2018) = 2018AJ....155...94S 2018AJ....155...94S
Lopez et al. (2019) = 2019A&A...631A..90L 2019A&A...631A..90L
Christiansen et al. (2018) = 2018AJ....155...57C 2018AJ....155...57C
Lissauer et al. (2013) = 2013ApJ...770..131L 2013ApJ...770..131L
Buchhave et al. (2016) = 2016AJ....152..160B 2016AJ....152..160B
Morton et al. (2016) = 2016ApJ...822...86M 2016ApJ...822...86M
MacDonald et al. (2016) = 2016AJ....152..105M 2016AJ....152..105M
de Leon et al. (2021) = 2021MNRAS.508..195D 2021MNRAS.508..195D
Christiansen et al. (2022) = 2022AJ....163..244C 2022AJ....163..244C
Marcy et al. (2014) = 2014ApJS..210...20M 2014ApJS..210...20M
Wang et al. (2014) = 2014ApJ...783....4W 2014ApJ...783....4W
Rowe et al. (2014) = 2014ApJ...784...45R 2014ApJ...784...45R
Torres et al. (2015) = 2015ApJ...800...99T 2015ApJ...800...99T
Xie (2014) = 2014ApJS..210...25X 2014ApJS..210...25X
Barclay et al. (2015) = 2015ApJ...809....7B 2015ApJ...809....7B
Fabrycky et al. (2012) = 2012ApJ...750..114F 2012ApJ...750..114F
Hadden & Lithwick (2014) = 2014ApJ...787...80H 2014ApJ...787...80H
Hadden & Lithwick (2016) = 2016ApJ...828...44H 2016ApJ...828...44H
Lissauer et al. (2012) = 2012ApJ...750..112L 2012ApJ...750..112L
Campante et al. (2015) = 2015ApJ...799..170C 2015ApJ...799..170C
Steffen et al. (2013) = 2013MNRAS.428.1077S 2013MNRAS.428.1077S
Borucki et al. (2013) = 2013Sci...340..587B 2013Sci...340..587B
Freudenthal et al. (2019) = 2019A&A...628A.108F 2019A&A...628A.108F
Berger et al. (2018) = 2018ApJ...866...99B 2018ApJ...866...99B
Xie (2013) = 2013ApJS..208...22X 2013ApJS..208...22X
Mayo et al. (2018) = 2018AJ....155..136M 2018AJ....155..136M
Rodriguez et al. (2018) = 2018AJ....156..245R 2018AJ....156..245R
Palle et al. (2019) = 2019A&A...623A..41P 2019A&A...623A..41P
Lillo-Box et al. (2020) = 2020A&A...640A..48L 2020A&A...640A..48L
Dressing et al. (2017) = 2017AJ....154..207D 2017AJ....154..207D
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Bonomo et al. (2019) = 2019NatAs...3..416B 2019NatAs...3..416B
Kipping et al. (2016) = 2016ApJ...820..112K 2016ApJ...820..112K
Mills et al. (2016) = 2016Natur.533..509M 2016Natur.533..509M
Torres et al. (2017) = 2017AJ....154..264T 2017AJ....154..264T
Ford et al. (2012) = 2012ApJ...750..113F 2012ApJ...750..113F
Jontof-Hutter et al. (2016) = 2016ApJ...820...39J 2016ApJ...820...39J
Batalha et al. (2013) = 2013ApJS..204...24B 2013ApJS..204...24B
Valizadegan et al. (2022) = 2022ApJ...926..120V 2022ApJ...926..120V
Jontof-Hutter et al. (2021) = 2021AJ....161..246J 2021AJ....161..246J
Stassun et al. (2017) = 2017AJ....153..136S 2017AJ....153..136S
Sun et al. (2019) = 2019A&A...624A..15S 2019A&A...624A..15S
Mills et al. (2019) = 2019AJ....157..145M 2019AJ....157..145M
Chaplin et al. (2013) = 2013ApJ...766..101C 2013ApJ...766..101C
Jontof-Hutter et al. (2014) = 2014ApJ...785...15J 2014ApJ...785...15J
Hadden & Lithwick (2017) = 2017AJ....154....5H 2017AJ....154....5H
Weiss et al. (2013) = 2013ApJ...768...14W 2013ApJ...768...14W
Albrecht et al. (2013) = 2013ApJ...771...11A 2013ApJ...771...11A
Wells et al. (2018) = 2018MNRAS.473L.131W 2018MNRAS.473L.131W
Mann et al. (2018) = 2018AJ....155....4M 2018AJ....155....4M
Hirano et al. (2018) = 2018AJ....155..127H 2018AJ....155..127H
Diez Alonso et al. (2018) = 2018MNRAS.476L..50D 2018MNRAS.476L..50D
Petigura et al. (2020) = 2020AJ....159....2P 2020AJ....159....2P
Sinukoff et al. (2016) = 2016ApJ...827...78S 2016ApJ...827...78S
David et al. (2018) = 2018AJ....155..222D 2018AJ....155..222D
Damasso et al. (2018) = 2018A&A...615A..69D 2018A&A...615A..69D
Crossfield et al. (2016) = 2016ApJS..226....7C 2016ApJS..226....7C
Kosiarek et al. (2019) = 2019AJ....157...97K 2019AJ....157...97K
Silva Aguirre et al. (2015) = 2015MNRAS.452.2127S 2015MNRAS.452.2127S
Jontof-Hutter et al. (2015) = 2015Natur.522..321J 2015Natur.522..321J
Malavolta et al. (2017) = 2017AJ....153..224M 2017AJ....153..224M
Ballard et al. (2011) = 2011ApJ...743..200B 2011ApJ...743..200B
Schmitt et al. (2014) = 2014ApJ...795..167S 2014ApJ...795..167S
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Muirhead et al. (2012) = 2012ApJ...747..144M 2012ApJ...747..144M
Everett et al. (2015) = 2015AJ....149...55E 2015AJ....149...55E
Muirhead et al. (2015) = 2015ApJ...801...18M 2015ApJ...801...18M
Huber et al. (2013) = 2013ApJ...767..127H 2013ApJ...767..127H
Holman et al. (2010) = 2010Sci...330...51H 2010Sci...330...51H
Torres et al. (2011) = 2011ApJ...727...24T 2011ApJ...727...24T
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(End) Prepared by [AAS], Coralie Fix [CDS], 23-Aug-2024