  We present an analysis of the Fe K line profile of NGC 4151 by using long
ASCA observation data obtained in May 1995. The unprecedented good data
quality, which is much better in the energy band around 6.4 keV than that of
the famous 4.2-day ASCA observation of MCG -6-30-15 in July 1994, offers a
unique opportunity to study the details of Fe K line profile. Apart from those
characteristics already noticed in earlier ASCA observations on this object
(Yaqoob et al. 1995): a broad and skewed profile, with a strong peak at about
6.4 keV and a large red wing extending to $\sim$4 - 5 keV, which is remarkably
similar to that of MCG -6-30-15, we also find a weak blue wing extending to
about 8 keV, thanks to the good quality of the data. When fitted by a
relativistic accretion disk line plus a narrow core at 6.4 keV, the data
constrain the accretion disk to be nearly face-on, contrary to the edge-on
geometry inferred from optical and UV observations. However, the extended blue
wing can not be well fitted even after we include corresponding Fe K$\beta$
components. Ni K$\alpha$ line emission by an amount of 12% of Fe K$\alpha$ is
statistically required. An alternative explanation is a model consisting of a
narrow core and two disk lines with inclinations of 58$^{\rm o}$ and 0$^{\rm
o}$, respectively. We suppose that the component with inclination of 58$^{\rm
o}$ was observed directly, consistent with its edge-on geometry, and the
component with inclination of 0$^{\rm o}$ was scattered into our line of sight
by a Compton mirror, which might be the cool accretion disk corona proposed by
Poutanen et al. (1996).
