Abstract
At the time of stellar evolution, young stellar objects go through processes of increased activity and instability. Star formation takes place in several stages during which the star accumulates enough mass to initiate thermonuclear reactions in the nucleus. A significant percentage of the mass of Sun-like stars accumulates during periods of increased accretion known as FUor outbursts. Since we know only about two dozen stars of this type, the study of each new object is very important for our knowledge. In this paper, we present data from photometric monitoring on a FUor object V2493 Cyg discovered in 2010. Our data were obtained in the optical region with BVRI Johnson–Cousins set of filters during the period from November 2016 to February 2021. The results of our observations show that during this period no significant changes in the brightness of the star were registered. We only detect variations with a small amplitude around the maximum brightness value. Thus, since 2013 V2493 Cyg remains at its maximum brightness, without a decrease in brightness. Such photometric behavior is not typical of other stars from FUor type. Usually, the light curves of FUors are asymmetrical, with a very rapid rise and gradual decline of the brightness. V2493 Cyg remains unique in this respect with a very rapid rise in brightness and prolonged retention in maximum light. Our period analysis made for the interval February 2013–February 2021 reveals a well-defined period of 914 ± 10 days. Such periodicity can be explained by dust structures remaining from star formation in orbit around the star.
Highlights
The main characteristic of the young stellar objects is their photometric and spectral variability
We present recent BVRI data from photometric observations of the star obtained during the period November 2016–February 2021
We used the BVRI comparison sequence of fifteen stars in the field around V2493 Cyg published in Semkov et al [15]. In this way we provided a maximum consistency of the photometric results obtained during the various stages of the photometric observations
Summary
The main characteristic of the young stellar objects is their photometric and spectral variability. Most often the variability is observed as transient increases in brightness, outbursts, temporary drops in brightness (eclipses), irregular or regular variations for a short or long time scales. Stars that undergo episodic outbursts with large amplitudes can be divided into two types FUors and EXors [1]. These two types of eruptive stars seem to be related to the low-mass PMS objects (T Tauri stars), which have massive circumstellar disks [2,3,4]. First Ambartsumian [6] draws attention to this object by linking it to the evolution of the young stellar objects and proposes the abbreviation FUor
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