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We present the results of the high-resolution spectroscopy of the FUOrionis-type star V960 Mon. The brightness of V960 Mon decreased continuouslyafter the outburst was detected in 2014 November. During this dimming event, wehave carried out medium-resolution spectroscopic monitoring observations andfound that the equivalent width of the absorption features showed variations.To further investigate the spectroscopic variations, we conducted ahigh-resolution spectroscopic observation of V960 Mon with the Subaru Telescopeand the High Dispersion Spectrograph on 2018 January 8 and 2020 February 1. Bycomparing this spectrum with the archival data of the Keck Observatory and theHigh Resolution Echelle Spectrometer taken between 2014 and 2017, we found thatthe absorption profiles changed as V960 Mon faded. The line profile ofabsorption lines such as Fe I and Ca I can be explained by a sum of the spectraof the disk atmosphere and the central star. The model spectrum created toexplain the variations of the line profiles suggests that the effectivetemperature of the central star is $\sim$5500 K, which is comparable to that ofthe pre-outburst phase with a distance of 1.6 kpc with Gaia. The spectrum alsoshows that the effective temperature of the disk atmosphere decreased as V960Mon faded. The variations of the H$\alpha$ and Ca II lines (8498.0 A, 8542.1 A)also show that the V960 Mon spectrum became central-star dominant.

Revealing the spectroscopic variations of FU Orionis object V960 Mon with high-resolution spectroscopy