J/A+A/687/L1 Resonant sub-Neptunes are puffier (Leleu+, 2024)
Resonant sub-Neptunes are puffier.
Leleu A., Delisle J.-B., Burn R., Izidoro A., Udry S., Dumusque X.,
Lovis C., Millholland S., Parc L., Bouchy F., Bourrier V., Alibert Y.,
Faria J., Mordasini C., Segransan D.
<Astron. Astrophys. 687, L1 (2024)>
=2024A&A...687L...1L 2024A&A...687L...1L (SIMBAD/NED BibCode)
ADC_Keywords: Stars, double and multiple ; Exoplanets ; Radial velocities ;
Stars, ages ; Effective temperatures
Keywords: techniques: photometric - techniques: radial velocities -
planets and satellites: composition -
planets and satellites: dynamical evolution and stability -
planets and satellites: fundamental parameters
Abstract:
A systematic, population-level discrepancy exists between the
densities of exoplanets whose masses have been measured with transit
timing variations (TTVs) versus those measured with radial velocities
(RVs). Since the TTV planets are predominantly nearly resonant, it is
still unclear whether the discrepancy is attributed to detection
biases or to astrophysical differences between the nearly resonant and
non resonant planet populations. We defined a controlled, unbiased
sample of 36 sub-Neptunes characterised by Kepler, TESS, HARPS, and
ESPRESSO. We found that their density depends mostly on the resonant
state of the system, with a low probability (of 0.002-0.001+0.010)
that the mass of (nearly) resonant planets is drawn from the same
underlying population as the bulk of sub-Neptunes. Increasing the
sample to 133 sub-Neptunes reveals finer details: the densities of
resonant planets are similar and lower than non-resonant planets, and
both the mean and spread in density increase for planets that are away
from resonance. This trend is also present in RV-characterised planets
alone. In addition, TTVs and RVs have consistent density distributions
for a given distance to resonance. We also show that systems closer to
resonances tend to be more co-planar than their spread-out
counterparts. These observational trends are also found in synthetic
populations, where planets that survived in their original resonant
configuration retain a lower density; whereas less compact systems
have undergone post-disc giant collisions that increased the
planet's density, while expanding their orbits. Our findings
reinforce the claim that resonant systems are archetypes of planetary
systems at their birth.
Description:
Full sample, with robust masses from Hadden & Lithwick
(2017AJ....154....5H 2017AJ....154....5H, Cat. J/AJ/154/5) and Leleu et al.
(2023A&A...669A.117L 2023A&A...669A.117L, Cat. J/A+A/669/A117) when available.
For this sample, the probability that the mass of the (nearly)
resonant and non-resonant population is drawn form the same underlying
population drops to pvalue=2.3e-06+2.7e-05-2.1e-06, while the
rest of the explored parameters are consistent between the two
sub-population.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
sample.dat 312 133 Full sample used in section 3 of the paper
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See also:
J/AJ/154/5 : 145 Kepler planets transit timing variations (Hadden+, 2017)
J/A+A/669/A117 : Mass-radius relationship of 34 Kepler planets (Leleu+, 2023)
Byte-by-byte Description of file: sample.dat
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Bytes Format Units Label Explanations
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1- 16 A16 --- Name Planet name
18- 35 F18.15 d Per Orbital period
37- 57 E21.16 d e_Per Orbital period mean error
59- 77 F19.16 Mgeo Massp Planetary mass
79- 97 F19.16 Mgeo e_Massp Planetary mass mean error
99-116 F18.16 Rgeo Radp Planetary radius
118-135 F18.16 Rgeo e_Radp Planetary radius mean error
137-156 F20.16 --- Distres Distance to the resonance following
eq. (1) of the paper
159-177 A19 --- BibCode BibCode of reference paper
179-202 A24 --- Aut Author's name of reference paper
204-222 F19.14 K Teq Equilibrium temperature
224-241 F18.15 K e_Teq Equilibrium temperature mean error
243-248 F6.1 K Teff Stellar effective temperature
250-255 F6.2 K e_Teff Stellar effective temperature mean error
257-262 F6.3 --- [Fe/H] Stellar metallicity
264-281 F18.16 --- e_[Fe/H] Stellar metallicity mean error
283-287 F5.2 Gyr Age Stellar age
289-306 F18.16 Gyr e_Age Stellar age mean error
308-312 F5.3 Rsun Rad Stellar radius
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Acknowledgements:
Adrien Leleu, Adrien.Leleu(at)unige.ch
(End) Patricia Vannier [CDS] 04-Jul-2024