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Recently Tsuji & Nakajima (2914) and Tsuji, Nakajima & Takeda (2015) havedeveloped a method of molecular line spectroscopy of M dwarfs with which Carbonand oxygen abundances are derived respectively from CO and H2O lines in the Kband. They applied this method to Gl229A, the primary star of the brown dwarfcompanion, Gl229B. The derived abundances of Gl229A are logAc=-3.27+/-0.07 andlogAo=-3.10+/-0.02, which are close to the classical values of the solarabundances of carbon and oxygen. We generate model spectra of Gl229B for themetallicity of Gl229A as well as for the classical solar metallicity. We findthat the differences of the resulting spectra are not so large for thedifferences of the metallicity of 0.1 dex or so, but we now discuss thespectrum of Gl229B on the basis of the reliable metallicity. From theliterature, the lower limit to the age of Gl229A is found to be 0.3Gyr. Fromthe kinematics of Gl229A, we evaluate the upper limit to the age of Gl229A tobe 3.0Gyr. The observed and model spectra are compared and goodness of fit isobtained in the range of model parameters, 750<Teff<1000K, and 4.5<logg<5.5.Among the candidates that satisfy the age constraint, the best combinations ofmodel parameters are (Teff,logg)=(800K,47.5) and (850K,5.0), while acceptablecombinations are (750K,4.75),(850K,4.75) and (900K,5.0).

Physical Properties of Gliese 229B Based on Newly Determined Carbon and Oxygen Abundances of Gliese 229A