J/AJ/168/109 Resonant and ultra-short-period planet systems (Schmidt+, 2024)
Resonant and ultra-short-period planet systems are at opposite ends of the
exoplanet age distribution.
Schmidt S.P., Schlaufman K.C., Hamer J.H.
<Astron. J., 168, 109 (2024)>
=2024AJ....168..109S 2024AJ....168..109S
ADC_Keywords: Exoplanets; Radial velocities; Stars, double and multiple;
Velocity dispersion; Stars, ages
Keywords: Exoplanet astronomy ; Exoplanet dynamics ; Exoplanet evolution ;
Exoplanet formation ; Exoplanet migration ; Exoplanet systems ;
Exoplanet tides ; Exoplanets ; Star-planet interactions ;
Stellar ages ; Stellar kinematics ; Tidal interaction
Abstract:
Exoplanet systems are thought to evolve on secular timescales over
billions of years. This evolution is impossible to directly observe on
human timescales in most individual systems. While the availability of
accurate and precise age inferences for individual exoplanet host
stars with ages τ in the interval 1Gyr≲τ≲10Gyr would
constrain this evolution, accurate and precise age inferences are
difficult to obtain for isolated field dwarfs like the host stars of
most exoplanets. The Galactic velocity dispersion of a thin-disk
stellar population monotonically grows with time, and the relationship
between age and velocity dispersion in a given Galactic location can
be calibrated by a stellar population for which accurate and precise
age inferences are possible. Using a sample of subgiants with precise
age inferences, we calibrate the age-velocity dispersion relation in
the Kepler field. Applying this relation to the Kepler field's planet
populations, we find that Kepler-discovered systems plausibly in
second-order mean-motion resonances have 1Gyr≲τ≲2Gyr. The same
is true for systems plausibly in first-order mean-motion resonances,
but only for systems likely affected by tidal dissipation inside their
innermost planets. These observations suggest that many planetary
systems diffuse away from initially resonant configurations on secular
timescales. Our calibrated relation also indicates that
ultra-short-period (USP) planet systems have typical ages in the
interval 5Gyr≲τ≲6Gyr. We propose that USP planets tidally
migrated from initial periods in the range 1day≲P≲2days to their
observed locations at P<1day over billions of years and trillions of
cycles of secular eccentricity excitation and inside-planet damping.
Description:
From Hamer & Schlaufman (2024, J/AJ/167/55), we obtain samples of
multiple-planet systems as well as plausibly first- and second-order
mean-motion resonant systems defined using their δres-based
criterion.
We obtain our sample of ultra-short-period (USP) planet systems from
Sanchis-Ojeda+ 2014, J/ApJ/787/47
We also define a sample of planets we term proto-USP planets as
confirmed planets from the Kepler cumulative planet catalog with
planet radii Rp<2R⊕ and orbital periods 1day<P<2days that
would have place them close to their parent protoplanetary disk's
magnetospheric truncation radii. We prefer the cumulative Kepler
Objects of Interest (KOI) list over the Data Release 25 KOI list due
to the extra level of scrutiny provided by the human vetting that
produced the cumulative catalog.
See Section 2.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 83 683 Ultra-short-period (USP) planet, proto-USP planet,
and plausibly/implausibly resonant system samples
table2.dat 33 3682 Kepler field age-velocity dispersion relation
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See also:
VII/233 : 2MASS All-Sky Extended Source Catalog (XSC) (IPAC/UMass, 2003-2006)
V/133 : Kepler Input Catalog (Kepler Mission Team, 2009)
I/350 : Gaia EDR3 (Gaia Collaboration, 2020)
III/284 : APOGEE-2 data from DR16 (Johnsson+, 2020)
III/286 : APOGEE-2 DR17 final allStar catalog (Abdurro'uf+, 2022)
J/A+A/506/303 : CoRoT-7 radial velocities (Queloz+, 2009)
J/AJ/142/112 : KIC photometric calibration (Brown+, 2011)
J/ApJS/197/8 : Kepler's cand. mult. transiting planets (Lissauer+, 2011)
J/ApJ/787/47 : 106 Kepler ultra-short-period planets (Sanchis-Ojeda+, 2014)
J/ApJ/790/146 : Planets in Kepler's multi-transiting systems (Fabrycky+, 2014)
J/ApJS/221/24 : SDSS-III APOGEE H-band spectral line lists (Shetrone+, 2015)
J/AJ/151/144 : ASPCAP weights for APOGEE chemical elements (Garcia+, 2016)
J/A+A/588/L6 : WASP-12 transit light curves (Maciejewski+ 2016)
J/AJ/153/136 : Planets & host stars with Gaia parallaxes (Stassun+, 2017)
J/AJ/154/4 : Times of transits and occultations of WASP-12b (Patra+, 2017)
J/AJ/154/107 : California-Kepler Survey (CKS). I. 1305 stars (Petigura+, 2017)
J/AJ/154/108 : California-Kepler Survey (CKS). II. Properties (Johnson+, 2017)
J/AJ/154/237 : HARPS-N radial velocities of WASP-47 (Vanderburg+, 2017)
J/A+A/619/A1 : 55 Cnc radial velocities and photometry (Bourrier+, 2018)
J/AJ/155/107 : HARPS-N obs. of K2-141 planetary system (Malavolta+, 2018)
J/AJ/155/196 : K2 LCs for members of USco & ρ Oph (Rebull+, 2018)
J/A+A/631/A77 : Low-mass stellar models and isochrones (Amard+, 2019)
J/AJ/158/190 : Hot Jupiter hosts with good astrometry (Hamer+, 2019)
J/AJ/159/273 : Taurus members & nonmembers with K2 data (Rebull+, 2020)
J/AJ/160/138 : 68 Gaia DR2 ultra-short-period planet host stars (Hamer+, 2020)
J/ApJ/888/L5 : Transits, occultation times and RVs of WASP-12b (Yee+, 2020)
J/ApJ/890/L31 : Rotational periods and J2 of Kepler stars (Li+, 2020)
J/AJ/159/19 : SOAR TESS survey. I. (Ziegler+, 2020)
J/A+A/649/A3 : Gaia Early Data Release 3 photometric passbands (Riello+, 2021)
J/A+A/650/A64 : Mars moon ephemerides from Mars Express 14yrs (Lainey+, 2021)
J/AJ/161/72 : Transit and occultation times for WASP-12b (Turner+, 2021)
J/AJ/164/26 : Hot Jupiters isochrones & stellar modeling (Hamer+, 2022)
J/other/Nat/603.599 : 247014 subgiant stars data (Xiang+, 2022)
J/AJ/165/88 : Radial velocity follow up of TOI-561 b (Brinkman+, 2023)
J/AJ/167/55 : Multiple-planet system resonances (Hamer+, 2024)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 8 I8 --- KIC [1432789/12600735] Kepler identifier
10- 28 I19 --- Gaia Gaia DR3 Source identifier
30- 35 F6.1 km/s RV [-225/69] Radial velocity
37- 40 F4.1 km/s e_RV [0/12] Uncertainty in RV
42- 47 A6 --- Source Radial velocity source ("CKS", "APOGEE"
or "Gaia")
49- 53 A5 --- Multi In a multiple-planet system? (1)
55- 59 A5 --- First In a plausibly first-order resonant system? (2)
61- 65 A5 --- Second In a plausibly second-order resonant system?
67- 71 A5 --- Tidal In a tidally-affected plausibly first-order
resonant system? (2)
73- 77 A5 --- USP In an ultra-short-period planet system?
79- 83 A5 --- Proto In a proto-ultra-short-period planet system?
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Note (1): The Kepler multiple-planet system sample contains all plausibly
resonant systems.
Note (2): Tidally-affected first-order resonant systems are included in the
sample of all first-order resonant systems.
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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 F8.5 Gyr Age [2/10.02] Average age
10- 16 F7.5 km/s e_sigma [0.5/2] Lower uncertainty in sigma (1)
18- 25 F8.5 km/s sigma [33.3/70] Velocity dispersion
27- 33 F7.5 km/s E_sigma [0.5/2] Upper uncertainty in sigma (2)
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Note (1): Lower uncertainty refers to the difference between the 50th and 16th
percentiles.
Note (2): Upper uncertainty refers to the difference between the 84th and 50th
percentiles.
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 27-Nov-2024