Constraining the Movement of the Spiral Features and the Locations of   Planetary Bodies within the AB Aur System
  We present new analysis of multi-epoch, H-band, scattered light images of the AB Aur system. We used a Monte Carlo, radiative transfer code to simultaneously model the system's SED and H-band polarized intensity imagery. We find that a disk-dominated model, as opposed to one that is envelope dominated, can plausibly reproduce AB Aur's SED and near-IR imagery. This is consistent with previous modeling attempts presented in the literature and supports the idea that at least a subset of AB Aur's spirals originate within the disk. In light of this, we also analyzed the movement of spiral structures in multi-epoch H-band total light and polarized intensity imagery of the disk. We detect no significant rotation or change in spatial location of the spiral structures in these data, which span a 5.8 year baseline. If such structures are caused by disk-planet interactions, the lack of observed rotation constrains the location of the orbit of planetary perturbers to be >47 AU. 
Jamie R. Lomax, John P. Wisniewski, Carol A. Grady, Michael W.   McElwain, Jun Hashimoto, Tomoyuki Kudo, Nobuhiko Kusakabe, ...
astro-ph.SR astro-ph.EP