  Deriving stellar atmospheric parameters and chemical abundances from stellar
spectra is crucial for understanding the evolution of the Milky Way. By
performing a fitting with MARCS model atmospheric theoretical synthetic spectra
combined with a domain-adaptation method, we estimate the fundamental stellar
parameters (Teff, log g, [Fe/H], vmic, and vmac) and 11 chemical abundances for
1.38 million FGKM-type stars of the Medium-Resolution Spectroscopic Survey
(MRS) from LAMOST-II DR8. The domain-adaptation method, Cycle-StarNet, is
employed to reduce the gap between observed and synthetic spectra, and the
L-BFGS algorithm is used to search for the best-fit synthetic spectra. By
combining the 2MASS photometric survey data, Gaia EDR3 parallax, and MIST
isochrones, the surface gravities of the stars are constrained after estimating
their bolometric luminosities. The accuracy of Teff, log g, and [Fe/H] can
reach 150 K, 0.11 dex, and 0.15 dex, evaluated by the PASTEL catalog,
asteroseismic samples, and other spectroscopic surveys. The precision of these
parameters and elemental abundances ([C/Fe], [Na/Fe], [Mg/Fe], [Si/Fe],
[Ca/Fe], [Ti/Fe], [Cr/Fe], [Mn/Fe], [Co/Fe], [Ni/Fe], and [Cu/Fe]) is assessed
by repeated observations and validated by cluster members. For spectra with
signal-to-noise (S/N) ratios greater than 10, the precision of the three
stellar parameters and elemental abundances can achieve 76 K, 0.014 dex, 0.096
dex, and 0.04-0.15 dex. For spectra with S/N ratios higher than 100, the
precision stabilizes at 22 K, 0.006 dex, 0.043 dex, and 0.01-0.06 dex. The full
LAMOST MRS stellar properties catalog is available online.
