摘要：Exoplanets residing close to their stars can experience evolution of both their physical structures and their orbits due to the influence of their host stars.In this work, we present a coupled analysis of dynamical tidal dissipation and atmospheric mass loss for exoplanets in X-ray and ultraviolet (XUV) irradiated environments.As our primary application, we use this model to study the TRAPPIST-1 system and place constraints on the interior structure and orbital evolution of the planets.We start by reporting on an ultraviolet continuum flux measurement (centered around ~1900 Å) for the star TRAPPIST-1, based on 300 ks of Neil Gehrels Swift Observatory data, and which enables an estimate of the XUV-driven thermal escape arising from XUV photodissociation for each planet.We find that the X-ray flaring luminosity, measured from our X-ray detections, of TRAPPIST-1 is 5.6 × 10−4 L*, while the full flux including non-flaring periods is 6.1 × 10−5 L*, when L* is TRAPPIST-1's bolometric luminosity.We then construct a model that includes both atmospheric mass loss and tidal evolution and requires the planets to attain their present-day orbital elements during this coupled evolution.We use this model to constrain the ratio $Q^{\prime} =3Q/2{k}_{2}$ for each planet.Finally, we use additional numerical models implemented with the Virtual Planet Simulator VPLanet to study ocean retention for these planets using our derived system parameters.
