  The protoplanetary disks of Herbig Ae stars eventually dissipate leaving a
tenuous debris disk comprised of planetesimals and dust, as well as possibly
gas and planets. This paper uses the properties of 10-20Myr A star debris disks
to consider the protoplanetary to debris disk transition. The physical
distinction between these two classes is argued to rest on the presence of
primordial gas in sufficient quantities to dominate the motion of small dust
grains (not the secondary nature of the dust or its level of stirring). This
motivates an observational classification based on the dust spectrum,
empirically defined so that A star debris disks require fractional excesses <3
at 12um and <2000 at 70um. We also propose a hypothesis to test, that the main
sequence planet/planetesimal structures are already in place (but obscured)
during the protoplanetary disk phase. This may be only weakly true if planetary
architectures change until frozen during disk dispersal, or completely false if
planets and planetesimals form during disk dispersal. Five steps in the
transition are discussed: (i) carving an inner hole to form a transition disk;
(ii) depletion of mm-sized dust in outer disk, noting the importance of
determining whether this mass ends up in planetesimals or is collisionally
depleted; (iii) final clearing of inner regions, noting that many mechanisms
replenish moderate hot dust levels at later phases, and likely also operate in
protoplanetary disks; (iv) disappearence of gas, noting recent discoveries of
primordial and secondary gas in debris disks that highlight our ignorance and
its impending enlightenment by ALMA; (v) formation of ring-like planetesimal
structures, noting these are shaped by interactions with planets, and that the
location of planetesimals in protoplanetary disks may be unrelated to the dust
concentrations therein that are set by gas interactions.
