  Recently Tsuji & Nakajima (2914) and Tsuji, Nakajima & Takeda (2015) have
developed a method of molecular line spectroscopy of M dwarfs with which Carbon
and oxygen abundances are derived respectively from CO and H2O lines in the K
band. They applied this method to Gl229A, the primary star of the brown dwarf
companion, Gl229B. The derived abundances of Gl229A are logAc=-3.27+/-0.07 and
logAo=-3.10+/-0.02, which are close to the classical values of the solar
abundances of carbon and oxygen. We generate model spectra of Gl229B for the
metallicity of Gl229A as well as for the classical solar metallicity. We find
that the differences of the resulting spectra are not so large for the
differences of the metallicity of 0.1 dex or so, but we now discuss the
spectrum of Gl229B on the basis of the reliable metallicity. From the
literature, the lower limit to the age of Gl229A is found to be 0.3Gyr. From
the kinematics of Gl229A, we evaluate the upper limit to the age of Gl229A to
be 3.0Gyr. The observed and model spectra are compared and goodness of fit is
obtained 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 of
model parameters are (Teff,logg)=(800K,47.5) and (850K,5.0), while acceptable
combinations are (750K,4.75),(850K,4.75) and (900K,5.0).
