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 $0.2sim 0.3$ solar at $10$ from the galaxy center. Dilution due to an extended hot gas is suggested.
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