In this paper, within the popular internal shock scenario of GRBs, we
calculate the early optical afterglow lightcurves of a neutron-fed GRB fireball
for different assumed neutron fractions in the fireball and for both ISM- and
wind-interaction models. The cases for both long and short GRBs are considered.
We show that as long as the neutron fraction is significant (e.g. the number of
neutrons is comparable to that of protons), rich afterglow signatures would
show up. For a constant density (ISM) model, a neutron-rich early afterglow is
characterized by a slowly rising lightcurve followed by a sharp re-brightening
bump caused by collision between the leading neutron decay trail ejecta and the
trailing ion ejecta. For a massive star stellar-wind model, the neutron-rich
early afterglow shows an extended plateau lasting for about 100 seconds before
the lightcurve starts to decay. The plateau is mainly attributed to the
emission from the unshocked neutron decay trail. When the overlapping of the
initial prompt γ−rays with the shocks and the trail is important, as is
common for the wind model and is also possible in the ISM model under some
conditions, the IC cooling effect suppresses the very early optical afterglow
significantly, making the neutron-fed signature dimmer. For short GRBs powered
by compact star mergers, a neutron-decay-induced step-like re-brightening is
predicted, although the amplitude is not large. All these neutron-fed
signatures are likely detectable by the Ultraviolet Optical Telescope (UVOT) on
board the {\em Swift} observatory if GRB fireballs are indeed baryonic and
neutron-rich. Close monitoring of early afterglows from 10s to 1000s of
seconds, when combined with detailed theoretical modeling, could be used to
potentially diagnose the existence of the neutron component in GRB fireballs.Comment: 17 pages (6 figures), accepted for publication in ApJ. Several
figures are revised, the IC cooling due to the prompt gamma-rays overlap with
the shocked regions (stellar wind model) has been taken into account. The
possible evidence for the neutron-rich internal shocks (i.e., the prompt
optical and near IR flash accompanying GRB 041219a) has been mentioned
briefl