  We present the results of a systematic analysis of Fe K emission lines in
low-luminosity AGNs (LLAGNs) observed with ASCA. We used a sample of LLAGNs
with small intrinsic absorption to compare with luminous AGNs and accretion
models. Some objects show an Fe line at 6.4 keV or 6.7 keV, and the rest of the
objects show no significant Fe K emission line. We made a composite spectrum of
sources without detected Fe emission lines to search for weak lines and
obtained an upper limit on the equivalent width (EW) of a narrow line at 6.4
keV of 145 eV, which is marginally consistent with EWs seen in Seyfert 1s. Even
in those objects with detected Fe lines, a skewed broad component, typically
observed in Seyfert 1s, is not seen. The weakness of the Fe line is consistent
with the absence of an optically thick disk in the vicinity of a central black
hole. Alternatively, it might be due to the ionization of a standard disk. The
lack of big blue bump favors the former.
