  Chondrule formation remains one of the most elusive early Solar System
events. Here, we take the novel approach of employing numerical simulations to
investigate chondrule origin beyond purely cosmochemical methods. We model the
transport of generically-produced chondrules and dust in a 1D viscous
protoplanetary disk model, in order to constrain the chondrule formation
events. For a single formation event we are able to match analytical
predictions of the memory chondrule and dust populations retain of each other
(complementarity), finding that a large mass accretion rate ($\gtrsim
10^{-7}$~M$_\odot$~yr$^{-1}$) allows for delays on the order of the disk's
viscous timescale between chondrule formation and chondrite accretion. Further,
we find older disks to be severely diminished of chondrules, with accretion
rates $\lesssim 10^{-9}$~M$_\odot$~yr$^{-1}$ for nominal parameters. We then
characterize the distribution of chondrule origins in both space and time, as
functions of disk parameters and chondrule formation rates, in runs with
continuous chondrule formation and both static and evolving disks. Our data
suggest that these can account for the observed diversity between distinct
chondrite classes, if some diversity in accretion time is allowed for.
