Mark C. Wyatt

TL;DR: In this article, a review describes the theoretical framework within which debris disk evolution takes place and shows how that framework has been constrained by observations, including infrared photometry of large numbers of debris disks, providing snapshots of the dust present at different evolutionary phases.

TL;DR: In this paper, the authors show how the gravitational influence of a second body in the system with an eccentric orbit would cause a brightness asymmetry in a disk by imposing a forced eccentricity on the orbits of the constituent dust particles, thus shifting the center of symmetry of the disk away from the star and causing the dust near the forced pericenter of the perturbed disk to glow.

TL;DR: In this article, a simple model for the steady state evolution of debris disks due to collisions is developed and confronted with the properties of the emerging population of seven Sun-like stars that have hot dust at 10 AU (η Corvi and HD 72905); one has three Neptune mass planets at < 1 AU (HD 69830); all exhibit strong mid-IR silicate features.

TL;DR: In this paper, a simple analytical model for the steady-state evolution of debris disks due to collisions is confronted with Spitzer observations of dust around main sequence A stars, and the detection statistics and trends seen at both 24 and 70 µm can be fitted well by the model.

TL;DR: In this paper, the authors made use of data from the first public release of the WASP data (Butters et al. 2010) as provided by the NASA Exoplanet Archive, which is operated by the California Institute of Technology under contract with the National Aeronautics and Space Administration under the ERC grant number 279973.