Photometric and spectroscopic variability of the FUor star V582 Aurigae

Abstract

Aims. We present results from optical photometric and spectroscopic observations of the eruptive pre-main sequence star V582 Aur. Variability of the star was reported a few years ago when it was suspected as a possible FU Orionis object. Due to the small number of currently known FUors, a new object of this type is ideal target for follow-up photometric and spectroscopic observations. Methods. We carried out BVRI CCD photometric observations in the field of V582 Aur from 2009 August to 2013 February. We acquired high-, medium-, and low-resolution spectroscopy of V582 Aur during this period. To study the pre-outburst variability of the target and construct its historical light curve, we searched for archival observations in photographic plate collections. Both CCD and photographic observations were analyzed using a sequence of 14 stars in the field of V582 Aur calibrated in BVRI. Results. The pre-outburst photographic observations of V582 Aur show low-amplitude light variations typical of T Tauri stars. Archival photographic observations indicate that the increase in brightness began in late 1984 or early 1985 and the star reached the maximum level of brightness at 1986 January. The spectral type of V582 Aur can be defined as G0I with strong P Cyg profiles of Hα and Na I D lines, which are typical of FU Orionis objects. Our BVRI photometric observations show large amplitude variations (ΔV ∼ 2. m 8) during the 3.5 year period of observations. Most of the time, however, the star remains in a state close to the maximum brightness. The deepest drop in brightness was observed in the spring of 2012, when the brightness of the star fell to a level close to the pre-outburst. The multicolor photometric data show a color reversal during the minimum in brightness, which is typical of UX Ori variables. The corresponding spectral observations show strong variability in the profiles and intensities of the spectral lines (especially Hα), which indicate significant changes in the accretion rate. On the basis of photometric monitoring performed over the past three years, the spectral properties of the maximal light, and the shape of the long-term light curve, we confirm the affiliation of V582 Aur to the group of FU Orionis objects.

Optical photometric and spectral study of the new FU Orionis object V2493 Cygni (HBC 722)

“…For some years, we have made efforts to construct the historical light curves of several other FUor and FUor-like objects such as: V1735 Cyg (Peneva et al 2009), Parsamian 21 (Semkov & Peneva 2010c), V733 Cep , and V582 Aur (Semkov et al 2011). Our results suggest that each object of this type has a characteristic long-term light curve, which distinguishes it from other objects.…”

Near-Ir Photometric and Optical Spectroscopic Study of the Fu Orionis Object V582 Aurigae

“…The slope of profile becomes steeper and the width of profile narrowed over time. This feature could be interpreted as the evidence of a strong and time-variable outflow driven by the central FUor object (Semkov et al, 2013).…”

An UXor among FUors: extinction-related brightness variations of the young eruptive star V582 Aur

“…As a continuation of our efforts on physical analysis of FUor and EXor light curves, here we present a study of the multiwavelength light variations of the young eruptive star V582 Aur. The object went into outburst at some time between 1980 and 1985 (Samus 2009), and was spectroscopically confirmed to belong to the FUor class by Semkov et al (2013). It is located close to the Galactic plane, and Kun et al (2017) argued that V582 Aur, together with a group of newly discovered low-mass young stellar objects (YSO), is related to the Aur OB 1 association at a distance of 1.32 kpc from the Sun.…”