  High quality X-ray spectra of NGC 4636 are obtained with ASCA. Theoretical
models are found unable to reproduce the data in the Fe-L line region. Spectral
data above 1.4 keV indicate that Mg to Si abundance ratio is $\sim 1$ solar.
Assuming that the abundance ratios among $\alpha$-elements are the same with
the solar ratios, spectral fit with increased systematic error in the 0.4--1.6
keV range gives abundances of $\alpha$-elements and Fe to be both $\sim$ 1
solar by taking one solar of Fe to be 3.24$\times 10^{-5}$ by number. These new
abundance results solve discrepancy between stellar and hot-gas metallicity,
but still a low supernova rate is implied. We also detect strong abundance
gradients for both $\alpha$-elements and iron in a similar fashion. The
abundance is $\sim 1$ solar within $4'$, and decreases outerwards down to
$0.2\sim 0.3$ solar at $10'$ from the galaxy center. Dilution due to an
extended hot gas is suggested.
