  We present the results of the spectroscopic monitoring of the FU Orionis type
star V960 Mon. Spectroscopic variations of a FU Orionis type star will provide
valuable information of its physical nature and the mechanism of the outburst.
We conducted medium-resolution (R~10000) spectroscopic observations of V960 Mon
with 2m Nayuta telescope at the Nishi-Harima Astronomical Observatory, from
2015 January to 2017 January for 53 nights in total. We focused on H alpha line
and nearby atomic lines, and detected the strength variations in both
absorption and emission lines. The observed variation in the equivalent width
of the absorption lines correspond to a decrease in effective temperature and
increase in surface gravity. These variations were likely to originate from the
luminosity fading of the accretion disk due to the decrease in mass accretion
rate.
