  We test the hypothesis that (3) Juno is a parent body of the H chondrites
with dynamical modeling of an asteroid-family-forming impact and comparison to
current observational data. Using a dynamical model that includes the Yarkovsky
force on a simulated Juno family and a simplified cosmic ray exposure age model
we examine the expected distribution of Juno family members in both the main
belt and near-Earth orbits over 300 Myrs and the cosmic ray exposure
distribution for fragments exiting the main belt via the 3:1J, 5:2J, and 8:3J
mean motion resonances. We find that the smallest modeled ($D<$10 m) family
members of (3) Juno cannot be directly responsible for the observed H chondrite
flux and that the breakup of larger family members creates an CRE distribution
that resembles the measured H chondrite CRE distribution but is still unable to
adequately explain the significant number of H chondrites with CRE ages of 6-8
Myrs. A similar model was performed for the asteroid (6) Hebe, another parent
body candidate, and produced a CRE age distribution that is inconsistent with
the measured H chondrite CRE ages. We also find from our dynamical models that
we can expect $<$7 km-scale Juno family members in near-Earth orbits in the
present day, consistent with the recent discovery of the shock-darkened H
chondrite-like asteroid (52768) 1998 OR$_{2}$.
