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Among the low-mass pre-main sequence stars, a small group called FUOrionis-type objects (FUors) are notable for undergoing powerful accretionoutbursts. V1057 Cyg, a classical example of an FUor, went into outburst around1969-1970, after which it faded rapidly, making it the fastest fading FUorknown. Around 1995, a more rapid increase in fading occurred. Since that time,strong photometric modulations have been present. We present nearly 10 years ofsource monitoring at Piszk\'estet\H{o} Observatory, complemented withoptical/near-infrared photometry and spectroscopy from the Nordic OpticalTelescope, Bohyunsan Optical Astronomy Observatory, Transiting Exoplanet SurveySatellite, and the Stratospheric Observatory for Infrared Astronomy. Our lightcurves show continuation of significant quasi-periodic variability inbrightness over the past decade. Our spectroscopic observations show strongwind features, shell features, and forbidden emission lines. All of thesespectral lines vary with time. We also report the first detection of [S II], [NII], and [O III] lines in the star.

A study of the photometric and spectroscopic variations of the prototypical FU Orionis-type star V1057 Cyg