  Jupiter and Saturn formed early, before the gas disk dispersed. The presence
of gap-opening planets affects the dynamics of the gas and embedded solids and
halts the inward drift of grains above a certain size. A drift barrier can
explain the absence of calcium aluminium rich inclusions (CAIs) in chondrites
originating from parent bodies that accreted in the inner solar system.
Employing an interdisciplinary approach, we use a $\mu$-X-Ray-fluorescence
scanner to search for large CAIs and a scanning electron microscope to search
for small CAIs in the ordinary chondrite NWA 5697. We carry out long-term,
two-dimensional simulations including gas, dust, and planets to characterize
the transport of grains within the viscous $\alpha$-disk framework exploring
the scenarios of a stand-alone Jupiter, Jupiter and Saturn \textit{in situ}, or
Jupiter and Saturn in a 3:2 resonance. In each case, we find a critical grain
size above which drift is halted as a function of the physical conditions in
the disk. From the laboratory search we find four CAIs with a largest size of
$\approx$200$\,\mu$m. \Combining models and data, we provide an estimate for
the upper limit of the $\alpha$-viscosity and the surface density at the
location of Jupiter, using reasonable assumptions about the stellar accretion
rate during inward transport of CAIs, and assuming angular momentum transport
to happen exclusively through viscous effects. Moreover, we find that the
compound gap structure in the presence of Saturn in a 3:2 resonance favors
inward transport of grains larger than CAIs currently detected in ordinary
chondrites.
