  Evidence suggests that the gamma-ray burst (GRB) ejecta is likely magnetized,
although the degree of magnetization of the ejecta is unknown. We derive a
rigorous analytical solution for the relativistic 90 degree shocks under the
ideal MHD condition, and use them to study the reverse shock emission
properties of an arbitrarily magnetized ejecta. Contrary to the previous
belief, we find that strong relativistic shocks still exist in the high-sigma
limit. Assuming a constant density of the circumburst medium, we study the
shell-medium interaction in detail and categorize various critical radii for
shell evolution. With typical GRB parameters, a reverse shock exists when sigma
is less than a few tens or a few hundreds. The shell evolution can be still
categorized into the thick and thin shell regimes, but the separation between
the two regime now depends on sigma and the thick shell regime greatly shrinks
at high-sigma. The early optical afterglow lightcurves are calculated for GRBs
with a wide range of the sigma values. We find that the reverse shock emission
level increases steadily with sigma initially, but starts to decline when sigma
becomes larger than unity. In the high-sigma regime the reverse shock peak is
usually broadened due to the separation of the shock crossing radius and the
deceleration radius in the thin shell regime. The early afterglow data and
tight upper limits of known GRBs could be understood within the theoretical
framework developed in this paper, with the inferred sigma value varying in a
wide range.
