  We model in simple terms the angular momentum (J) problem of galaxy formation
in CDM, and identify the key elements of a scenario that can solve it. The
buildup of J is modeled via dynamical friction and tidal stripping in mergers.
This reveals how over-cooling in incoming halos leads to transfer of J from
baryons to dark matter (DM), in conflict with observations. By incorporating a
simple recipe of supernova feedback, we match the observed J distribution in
disks. Gas removal from small incoming halos, which make the low-J component of
the product, eliminates the low-J baryons. Partial heating and puffing-up of
the gas in larger incoming halos, combined with tidal stripping, reduces the J
loss of baryons. This implies a higher baryonic spin for lower mass halos. The
observed low baryonic fraction in dwarf galaxies is used to calibrate the
characteristic velocity associated with supernova feedback, yielding v_fb sim
100 km/s, within the range of theoretical expectations. The model then
reproduces the observed distribution of spin parameter among dwarf and bright
galaxies, as well as the J distribution inside these galaxies. This suggests
that the model captures the main features of a full scenario for resolving the
spin crisis.
