Abstract:
We present here the results of 8 yr of our near-simultaneous optical–near-infrared spectro-photometric monitoring
of the bona fide FU Ori (FUor)-type candidate V2493 Cygnus (V2493 Cyg) starting from 2013 September to 2021
June. During our optical monitoring period (between 2015 October 16 and 2019 December 30), the V2493 Cyg is
slowly dimming with an average dimming rate of ∼26.6 ± 5.6 mmag yr−1 in the V band. Our optical photometric
colors show a significant reddening of the source post the second outburst pointing toward a gradual expansion of
the emitting region post the second outburst. The mid-infrared colors, on the contrary, exhibit a blueing trend,
which can be attributed to the brightening of the disk due to the outburst. Our spectroscopic monitoring shows a
dramatic variation of the Hα line as it transitioned from absorption feature to the emission feature and back. Such
transition can possibly be explained by the variation in the wind structure in combination with accretion.
Combining our time evolution spectra of the Ca II infrared triplet lines with the previously published spectra of
V2493 Cyg, we find that the accretion region has stabilized compared to the early days of the outburst. The
evolution of the O I λ7773 Å line also points toward the stabilization of the circumstellar disk post the second
outburst.
