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The Ages and Orbital Dynamics of Planetary Systems

Presentation #607.09 in the session Population Statistics and Mass-Radius Relations.

Published onApr 03, 2024
The Ages and Orbital Dynamics of Planetary Systems

The Gaia data releases have enabled a better understanding of planetary occurrence within a broader galactic context. Whether planetary systems are impacted by galactic dynamics is newly testable: historical trends with metallicity, for example, may instead serve as proxies for galactic trends over long timescales. M dwarf planet host stars are a particularly useful tracer here, as their long lifetimes and abundance of planetary systems make them effective probes of galactic planet formation. However, their slow evolution makes it particularly difficult to constrain the stellar age. In this study, we describe a two-pronged effort to understand the architectures of M dwarf planetary systems within a wider galactic framework. First, we describe an open-source tool to obtain kinematic age estimates of stars, calibrated on the relatively precise asteroseismic ages for red giant branch stars and their vertical actions (an integral of galactic motion). This tool relies upon a purely kinematic, hierarchical stellar age-vertical action relation that can be applied even to low-mass stars. Secondly, we employ the resulting age constraints on M dwarfs in the Kepler sample to investigate the evolution of orbital eccentricity over time. This analysis relies upon a previous study in which we constrained eccentricity for the same set of planets using Kepler light curves and Gaia DR3 stellar properties.

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