  If X-ray flashes (XRFs) and X-ray rich Gamma-ray Bursts(XRRGs) have the same
origin with Gamma-ray Bursts (GRBs) but are viewed from larger angles of
structured jets, their early afterglows may differ from those of GRBs. When the
ultra-relativistic outflow interact with the surrounding medium, there are two
shocks formed, one is a forward shock, the other is a reverse shock. In this
paper we calculate numerically the early afterglow powered by uniform jet,
Gaussian jet and power-law jet in the forward-reverse shock scenario. A set of
differential equations are used to govern the dynamical evolution and
synchrotron self-Compton effect has been taken into account to calculate the
emission. In uniform jets, the very early afterglows of XRRGs and XRFs are
significantly lower than GRBs and the observed peak times of RS emission are
longer in interstellar medium environment. The RS components in XRRGs and XRFs
are difficult to be detected. But in stellar wind, the reduce of very early
flux and the delay of RS peak time are not so remarkable. In nonuniform
jet(Gaussian jet and power-law jet), where there are emission materials on the
line of sight, the very early light curve resembles isotropic-equivalent ejecta
in general although the RS flux decay index shows notable deviation if the RS
is relativistic(in stellar wind).
