Resonant and ultra-short-period planet systems are at opposite ends of the exoplanet age distribution. (2024)
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 {tau} in the interval 1Gyr<~{tau}<~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
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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 {delta}_res_-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_{Earth}_ and orbital periods 1day
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