J/AJ/165/125 Planetary Orbit Eccentricity Trends (POET). I. (An+, 2023)
Planetary Orbit Eccentricity Trends (POET).
I. The Eccentricity-Metallicity Trend for Small Planets Revealed by the
LAMOST-Gaia-Kepler Sample.
An D.-S., Xie J.-W., Dai Y.-Z., Zhou J.-L.
<Astron. J., 165, 125 (2023)>
=2023AJ....165..125A 2023AJ....165..125A
ADC_Keywords: Exoplanets; Stars, masses; Stars, diameters; Abundances, [Fe/H];
Effective temperatures; Optical
Keywords: Exoplanets ; Planet hosting stars
Abstract:
Orbital eccentricity is one of the basic planetary properties, whose
distribution may shed light on the history of planet formation and
evolution. Here, in a series of works on Planetary Orbit Eccentricity
Trends (dubbed POET), we study the distribution of planetary
eccentricities and their dependence on stellar/planetary properties.
In this paper, the first work of the POET series, we investigate
whether and how the eccentricities of small planets depend on stellar
metallicities (e.g., [Fe/H]). Previous studies on giant planets have
found a significant correlation between planetary eccentricities and
their host metallicities. Nevertheless, whether such a correlation
exists for small planets (e.g., super-Earths and sub-Neptunes) remains
unclear. Here, benefiting from the large and homogeneous LAMOST-Gaia-
Kepler sample, we characterize the eccentricity distributions of 244
(286) small planets in single (multiple) transiting systems with the
TDR method. We confirm the eccentricity-metallicity trend whereby the
eccentricities of single small planets increase with stellar
metallicities. Interestingly, a similar trend between eccentricity and
metallicity is also found in the radial velocity sample. We also found
that the mutual inclination of multiple transiting systems increases
with metallicity, which predicts a moderate eccentricity-metallicity
rising trend. Our results of the correlation between eccentricity
(inclination) and metallicity for small planets support the core
accretion model for planet formation, and they could be footprints of
self (and/or external) excitation processes during the history of
planet formation and evolution.
Description:
We started our sample selection from the Kepler DR25, NASA Exoplanet
Archive. To obtain a precise and homogeneous sample of metallicity, we
then cross-matched the Kepler DR25 with LAMOST Data Release 8 (DR8).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 199 244 *Kepler single planet systems analyzed in this work
table3.dat 199 286 *Kepler multiple planet systems analyzed in this work
table4.dat 124 18 *RVel single planet systems analyzed in this work
table5.dat 124 29 *RVel multiple planet systems analyzed in this work
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Note on table2.dat and table3.dat: Planetary parameters, stellar
parameters (except [Fe/H]) and [Fe/H] are from Kepler DR25 (NASA
Exoplanet Archive 2020), Berger+, 2020AJ....159..289B 2020AJ....159..289B and LAMOST DR8,
respectively.
Note on table4.dat and table5.dat: Planetary and stellar parameters
are from NASA Exoplanet Archive.
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See also:
I/345 : Gaia DR2 (Gaia Collaboration, 2018)
J/ApJ/622/1102 : The planet-metallicity correlation. (Fischer+, 2005)
J/ApJ/709/168 : Eccentric orbits in exoplanets (Anglada-Escude+, 2010)
J/ApJ/736/19 : Kepler planetary candidates. II. (Borucki+, 2011)
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/220/19 : LAMOST obs. in the Kepler field. I. (De Cat+, 2015)
J/AJ/152/187 : Planet occurrence & stellar metallicity KOIs (Mulders+, 2016)
J/AJ/154/107 : California-Kepler Survey. I. 1305 stars (Petigura+, 2017)
J/ApJS/235/38 : Kepler planetary cand VIII. DR25 reliability (Thompson+, 2018)
J/AJ/159/280 : Gaia-Kepler stellar properties cat.I KIC stars (Berger+, 2020)
J/AJ/162/100 : PAST. II. LAMOST-Gaia-Kepler cat. of 35835 stars (Chen+, 2021)
J/ApJS/255/6 : Warm Jupiter TESS FFIs 1st year (2018-2019 July) (Dong+, 2021)
http://exoplanetarchive.ipac.caltech.edu/ : NASA exoplanets archive
Byte-by-byte Description of file: table[23].dat
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Bytes Format Units Label Explanations
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1- 9 A9 --- Kepler Name Kepler identifier
11- 18 F8.4 d Per Orbital period
20- 28 E9.3 d E_Per Upper uncertainty in Per
30- 38 E9.3 d e_Per Lower uncertainty in Per
40- 47 F8.6 --- Rrot Planet-star radius ratio
49- 56 F8.6 --- E_Rrot Upper uncertainty in Rrot
58- 65 F8.6 --- e_Rrot Lower uncertainty in Rrot
67- 73 F7.4 h Dur Transit duration
75- 80 F6.4 h E_Dur Upper uncertainty in Dur
82- 87 F6.4 h e_Dur Lower uncertainty in Dur
89- 93 F5.1 --- SNR Transit model signal-to-noise ratio
95-100 F6.4 --- RUWE Re-normalized unit-weight error
102-107 F6.1 K Teff Effective temperature
109-113 F5.1 K E_Teff Upper uncertainty in Teff
115-119 F5.1 K e_Teff Lower uncertainty in Teff
121-125 F5.3 cm/s2 logg Surface gravity
127-131 F5.3 cm/s2 E_logg Upper uncertainty in logg
133-137 F5.3 cm/s2 e_logg Lower uncertainty in logg
139-144 F6.4 --- GOF Combined likelihood goodness-of-fit
146-150 F5.3 Msun Mass Stellar mass
152-156 F5.3 Msun E_Mass Upper uncertainty in Mass
158-162 F5.3 Msun e_Mass Lower uncertainty in Mass
164-168 F5.3 Rsun Rad Stellar radius
170-174 F5.3 Rsun E_Rad Upper uncertainty in Rad
176-180 F5.3 Rsun e_Rad Lower uncertainty in Rad
182-187 F6.3 [Sun] [Fe/H] log metallicity
189-193 F5.3 [Sun] E_[Fe/H] Upper uncertainty in [Fe/H]
195-199 F5.3 [Sun] e_[Fe/H] Lower uncertainty in [Fe/H]
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Byte-by-byte Description of file: table[45].dat
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Bytes Format Units Label Explanations
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1- 17 A17 --- Name Planet identifier
19- 23 F5.3 Rgeo Rad ? Planet radius
25- 29 F5.3 Rgeo E_Rad ? Upper uncertainty in Rad
31- 35 F5.3 Rgeo e_Rad ? Lower uncertainty in Rad
37- 43 F7.4 Mgeo Mass Planet mass or mass*sin(i)
45- 52 F8.5 Mgeo E_Mass ? Upper uncertainty in Mass
54- 61 F8.5 Mgeo e_Mass ? Lower uncertainty in Mass
63- 67 F5.3 --- e Planet eccentricity
69- 73 F5.3 --- E_e Upper uncertainty in e
75- 79 F5.3 --- e_e Lower uncertainty in e
81- 85 F5.2 [Sun] [Fe/H] log stellar metallicity
87- 90 F4.2 [Sun] E_[Fe/H] ? Upper uncertainty in [Fe/H]
92- 95 F4.2 [Sun] e_[Fe/H] ? Lower uncertainty in [Fe/H]
97-104 F8.4 d Per Orbital period
106-114 F9.7 d E_Per Upper uncertainty in Per
116-124 F9.7 d e_Per Lower uncertainty in Per
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History:
From electronic version of the journal
(End) Prepared by [AAS], Coralie Fix [CDS], 30-Jun-2023