TY - JOUR
T1 - The Orbital Eccentricity of Small Planet Systems
AU - Eylen, Vincent Van
AU - Albrecht, Simon
AU - Huang, Xu
AU - Macdonald, Mariah G.
AU - Dawson, Rebekah I.
AU - Cai, Maxwell X.
AU - Foreman-Mackey, Daniel
AU - Lundkvist, Mia S.
AU - Aguirre, Victor Silva
AU - Snellen, Ignas
AU - Winn, Joshua N.
N1 - Funding Information:
We are grateful to the anonymous referee for helpful comments and suggestions which have improved this manuscript. V.V.E. and S.A. acknowledge support from the Danish Council for Independent Research, through a DFF Sapere Aude Starting grant No. 4181-00487B. R.I.D. gratefully acknowledges support from NASA XRP 80NSSC18K0355. M.S.L. is supported by The Independent Research Fund Denmarks Sapere Aude program (grant agreement no.: DFF5051-00130). V.S.A. acknowledges support from the Villum Foundation (Research grant 10118). J.N.W. thanks the Heising-Simons Foundation for supporting his work. This material is based upon work supported by the National Science Foundation Graduate Research Fellowship Program under grant No. DGE1255832. Any opinions, findings, and conclusions or recommendations expressed in this material are those of the author and do not necessarily reflect the views of the National Science Foundation. This research has made use of the NASA Exoplanet Archive, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. This research made use of the Grendel HPC-cluster for computations. Funding for the Stellar Astrophysics Centre is provided by The Danish National Research Foundation (grant agreement no.: DNRF106). The research was supported by the ASTERISK project (ASTER-oseismic Investigations with SONG and Kepler), which is funded by the European Research Council (grant agreement no.: 267864).
Publisher Copyright:
© 2019. The American Astronomical Society. All rights reserved.
PY - 2019/2
Y1 - 2019/2
N2 - We determine the orbital eccentricities of individual small Kepler planets, through a combination of asteroseismology and transit light-curve analysis. We are able to constrain the eccentricities of 51 systems with a single transiting planet, which supplement our previous measurements of 66 planets in multi-planet systems. Through a Bayesian hierarchical analysis, we find evidence that systems with only one detected transiting planet have a different eccentricity distribution than systems with multiple detected transiting planets. The eccentricity distribution of the single-transiting systems is well described by the positive half of a zero-mean Gaussian distribution with a dispersion σ e = 0.32 ± 0.06, while the multiple-transit systems are consistent with . A mixture model suggests a fraction of of single-transiting systems have a moderate eccentricity, represented by a Rayleigh distribution that peaks at . This finding may reflect differences in the formation pathways of systems with different numbers of transiting planets. We investigate the possibility that eccentricities are self-excited in closely packed planetary systems, as well as the influence of long-period giant companion planets. We find that both mechanisms can qualitatively explain the observations. We do not find any evidence for a correlation between eccentricity and stellar metallicity, as has been seen for giant planets. Neither do we find any evidence that orbital eccentricity is linked to the detection of a companion star. Along with this paper, we make available all of the parameters and uncertainties in the eccentricity distributions, as well as the properties of individual systems, for use in future studies.
AB - We determine the orbital eccentricities of individual small Kepler planets, through a combination of asteroseismology and transit light-curve analysis. We are able to constrain the eccentricities of 51 systems with a single transiting planet, which supplement our previous measurements of 66 planets in multi-planet systems. Through a Bayesian hierarchical analysis, we find evidence that systems with only one detected transiting planet have a different eccentricity distribution than systems with multiple detected transiting planets. The eccentricity distribution of the single-transiting systems is well described by the positive half of a zero-mean Gaussian distribution with a dispersion σ e = 0.32 ± 0.06, while the multiple-transit systems are consistent with . A mixture model suggests a fraction of of single-transiting systems have a moderate eccentricity, represented by a Rayleigh distribution that peaks at . This finding may reflect differences in the formation pathways of systems with different numbers of transiting planets. We investigate the possibility that eccentricities are self-excited in closely packed planetary systems, as well as the influence of long-period giant companion planets. We find that both mechanisms can qualitatively explain the observations. We do not find any evidence for a correlation between eccentricity and stellar metallicity, as has been seen for giant planets. Neither do we find any evidence that orbital eccentricity is linked to the detection of a companion star. Along with this paper, we make available all of the parameters and uncertainties in the eccentricity distributions, as well as the properties of individual systems, for use in future studies.
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U2 - 10.3847/1538-3881/aaf22f
DO - 10.3847/1538-3881/aaf22f
M3 - Article
AN - SCOPUS:85062898646
SN - 0004-6256
VL - 157
JO - Astronomical Journal
JF - Astronomical Journal
IS - 2
M1 - 61
ER -