  This paper reports results of a Suzaku observation of the supernova remnant
(SNR) Kes 79 (G33.6+0.1). The X-ray spectrum is best fitted by a
two-temperature model: a non-equilibrium ionization (NEI) plasma and a
collisional ionization equilibrium (CIE) plasma. The NEI plasma is spatially
confined within the inner radio shell with kT~0.8 keV, while the CIE plasma is
found in more spatially extended regions associated with the outer radio shell
with kT~0.2 keV and solar abundance. Therefore, the NEI plasma is attributable
to the SN ejecta and the CIE plasma is forward shocked interstellar medium. In
the NEI plasma, we discovered K-shell line of Al, Ar and Ca for the first time.
The abundance pattern and estimated mass of the ejecta are consistent with the
core-collapse supernova explosion of a ~30-40 solar mass progenitor star. An Fe
line with center energy of ~6.4 keV is also found in the southeast (SE) portion
of the SNR, a close peripheral region around dense molecular clouds. One
possibility is that the line is associated with the ejecta. However, the
centroid energy of ~6.4 keV and the spatial distribution of enhancement near
the SE peripheral do not favor this scenario. Since the ~6.4 keV emitting
region coincides to the molecular clouds, we propose another possibility that
the Fe line is due to K-shell ionization of neutral Fe by the interaction of
locally accelerated protons (LECRp) with the surrounding molecular cloud. Both
these possibilities, heated ejecta or LECRp origin, are discussed based on the
observational facts.
