  We model the spectral energy distribution (SED) from the mid-infrared to
submillimeter of the ring-like disk of HR 4796A, the dustiest A-type star. We
consider dust made either of coagulated but otherwise unaltered protostellar
interstellar grains, or grains that are highly-processed in a
protostellar/protoplanetary nebula with silicate dust annealed and carbon dust
oxidized. Both types of dust are successful in reproducing the observed SED,
provided that the grains are highly fluffy, with a vacuum volume fraction of
\~90%. We find no evidence for the existence of a hot ``zodiacal dust''
component a few AU from the star, which was suggested by previous workers to
account for the 10 micron-wavelength emission.
