We describe planetesimal accretion calculations for the dusty ring observed
in the nearby AO star HR 4796A. Models with initial masses of 10-20 times
the minimum-mass solar nebula produce a ring with a width of 7-15 AU and a
height of 0.3-0.6 AU at 70 AU in similar to 10 Myr. The ring has a radial o
ptical depth of similar to 1. These results agree with limits derived from
infrared images and from the excess infrared luminosity.