Deep 10 and 18 Micron Imaging of the HR 4796A Circumstellar Disk: Transient Dust Particles and Tentative Evidence for a Brightness Asymmetry

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We present new 10.8 and 18.2 km images of HR 4796A, a young A0 V star that was recently dis- covered to have a spectacular, nearly edge-on, circumstellar disk prominent at D20 km (Jayawardhana and coworkers ; Koerner and coworkers). These new images, obtained with OSCIR (the University of Florida Observatory Spectrometer/Camera for the Infrared) at Keck II, show that the disks size at 10 km is comparable to its size at 18 km. Therefore, the 18 kmemitting dust may also emit some, or all, of the 10 km radiation. Using these multiwavelength images, we determine a ii characteristic ˇˇ diameter of 2¨3 km for the mid-infraredemitting dust particles if they are spherical and composed of astronomical silicates. Particles this small are expected to be blown out of the system by radiation pressure in a few hundred years, and therefore these particles are unlikely to be primordial. Rather, as inferred in a com- panion paper (Wyatt and coworkers), they are probably products of collisions that dominate both the creation and the destruction of dust in the HR 4796A disk. Dynamical modeling of the disk, the details of which are presented in the companion paper, indicates that the disk surface density is relatively sharply peaked near 70 AU, which agrees with the mean annular radius deduced by Schneider and coworkers from their NICMOS images. Interior to 70 AU, the model density drops steeply by a factor of 2 between 70 and 60 AU, falling to zero by 45 AU, which corresponds to the edge of the previously discovered central hole ; in the context of the dynamical models, this ii soft ˇˇ edge for the central hole occurs because the dust particle orbits are noncircular. The optical depth of mid-infraredemitting dust in the hole is D3% of the optical depth in the disk, and the hole is therefore relatively very empty. We present evidence (D1.8p signi—cance) for a brightness asymmetry that may result from the presence of the hole and the gravitational perturbation of the disk particle orbits by the low-mass stellar companion or a planet. This ii pericenter glow,ˇˇ which must still be con—rmed, results from a very small (a few AU) shift of the disks center of symmetry relative to the central star HR 7496A ; one side of the inner bound- ary of the annulus is shifted toward HR 4796A, thereby becoming warmer and more infrared-emitting. The possible detection of pericenter glow implies that the detection of even complex dynamical eUects of planets on disks is within reach. Subject headings : circumstellar matterinfrared : starsstars : individual (HR 4796A)