J/ApJ/880/L1 Kepler planet masses, radii and orbital periods (Armstrong+, 2019)
A gap in the mass distribution for warm Neptune and terrestrial planets.
Armstrong D.J., Meru F., Bayliss D., Kennedy G.M., Veras D.
<Astrophys. J., 880, L1 (2019)>
=2019ApJ...880L...1A 2019ApJ...880L...1A
ADC_Keywords: Exoplanets; Stars, masses; Models
Keywords: planets and satellites: detection ;
planets and satellites: dynamical evolution and stability ;
planets and satellites: formation ; planets and satellites: general ;
planets and satellites: physical evolution
Abstract:
Structure in the planet distribution provides an insight into the
processes that shape the formation and evolution of planets. The
Kepler mission has led to an abundance of statistical discoveries in
regards to planetary radius, but the number of observed planets with
measured masses is much smaller. By incorporating results from recent
mass determination programs, we have discovered a new gap emerging in
the planet population for sub-Neptune-mass planets with orbital
periods less than 20 days. The gap follows a slope of decreasing mass
with increasing orbital period, has a width of a few M⊕, and
is potentially completely devoid of planets. Fitting Gaussian mixture
models to the planet population in this region favors a bimodel
distribution over a unimodel one with a reduction in Bayesian
information criterion of 19.9, highlighting the gap significance. We
discuss several processes that could generate such a feature in the
planet distribution, including a pileup of planets above the gap
region, tidal interactions with the host star, dynamical interactions
with the disk, with other planets, or with accreting material during
the formation process.
Description:
We use the confirmed planet sample from the NASA Exoplanet Archive
as of the 2019 May 24.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 169 143 Planet sample
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See also:
IV/34 : K2 Ecliptic Plane Input Catalog (EPIC) (Huber+, 2017)
J/ApJ/787/80 : 139 Kepler planets transit time variations (Hadden+, 2014)
J/ApJ/821/89 : 12yrs of RVel obs. of exoplanet systems (Bryan+, 2016)
J/A+A/602/A107 : 231 transiting planets eccentricity and mass (Bonomo+, 2017)
J/AJ/154/109 : California-Kepler Survey. III. Planet radii (Fulton+, 2017)
J/ApJS/239/2 : Simulated exoplanets from TESS list of targets (Barclay+, 2018)
J/ApJS/235/38 : Kepler planetary cand. VIII. DR25 reliability (Thompson+, 2018)
J/ApJS/239/32 : APOKASC-2 catalog of Kepler evolved stars (Pinsonneault+, 2018)
J/AJ/155/48 : California-Kepler Survey. V. Masses and radii (Weiss+, 2018)
J/AJ/156/264 : CKS. VII. Planet radius gap (Fulton+, 2018)
J/AJ/157/116 : RVels of K2-291 with HIRES & HARPS-N (Kosiarek+, 2019)
J/AJ/158/38 : New substellar discoveries from Kepler & K2 (Carmichael+, 2019)
J/AJ/160/90 : Stellar parameters for 13196 Kepler dwarfs (Angus+, 2020)
http://exoplanetarchive.ipac.caltech.edu/ : NASA exoplanet archive
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 13 A13 --- Planet Planet identifier
15- 16 A2 --- Set Sample identifier (1)
18- 24 F7.4 d Period [0.28/19.73] Period
26- 32 F7.4 Mgeo Mp [0.68/24.6] Planet mass
34- 39 F6.4 Mgeo E_Mp [0.09/6.4] Upper uncertainty in Mp
41- 46 F6.4 Mgeo e_Mp [0.09/6.4] Lower uncertainty in Mp
48- 53 F6.4 Rgeo Rp [1/7.1]? Planet radius
55- 60 F6.3 g/cm3 rho [0.27/11.82]? Planet density
62- 68 F7.5 --- ecc [0/0.47]? Planet eccentricity
70- 73 F4.2 Msun M* [0.08/1.4]? Stellar mass
75- 75 I1 --- Np [1/7] Number of known planets
77-120 A44 --- Obs Discovery facility
122-149 A28 --- Auth Authors and year of the reference
151-169 A19 --- BibCode ADS style bibcode of the reference
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Note (1): Our prime sample (P1) consists of all transiting planets with
measured masses Mp, radii Rp, and hence inclination, within the limits
Mp<25M⊕ and orbital period P<20d. These are all transiting
planets with masses determined through radial velocities (RVs) or
transit timing variations (TTVs).
Our second wider sample (P2) consists of all planets with Mp or
Mpsin(i) within the same limits and additionally contains planets
with no measured inclination.
Only planets with mass measurements better than 3σ were included
in either sample.
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 21-Jan-2021