We present a detailed analysis of a long , 100 ksec , observation of NGC 4151 by ASCA , contemporaneous with an observation by the CGRO /OSSE .
We fit the data with physical models including an Fe K line and Compton reflection both relativistically broadened and coupled according to theoretical results .
The model also includes a narrow Fe K component , which is emitted by both an extended plasma region and the X-ray absorber .
Our study of the absorber shows strong evidence for the presence of more than one partial-covering cloud in the line of sight .
Taking these points into account , our best intrinsic model includes a Comptonization continuum with an X-ray slope of \Gamma \simeq 1.9 from a thermal plasma with an electron kT \sim 70 keV and a disk line with an equivalent width of \sim 70 eV .
The broadening of the line and reflection indicate their origin from innermost parts of an accretion disk .
Our results indicate that NGC 4151 has an intrinsic X-ray spectrum and variability properties similar to those of average Seyfert 1s .