New optical rebrightening of the young eruptive object V2492 Cyg (IRAS 20496+4354)
ATel #4180; E. Semkov, S. Peneva (Institute of Astronomy and NAO, Sofia, Bulgaria)
on 16 Jun 2012; 13:30 UT
Credential Certification: E. Semkov (esemkov@astro.bas.bg)
Subjects: Optical, Variables, Pre-Main-Sequence Star
We report results from VRI optical observations of the recently discovered PMS eruptive star V2492 Cyg in the region of Pelican Nebula (Itagaki and Yamaoka, CBET #2426, Munari et al. CBET #2428 Covey et al. 2011, AJ, 141, 40).
Starting from the mid-2009 the object shows a strong outburst by ~6 mag, which reaches its maximum in the summer of 2010.
Such large amplitude eruptions are very rare phenomenon and they can be grouped into two main types, named FUors and EXors.
The nature of the outburst occurred in V2492 Cyg is still controversial, as the star shows some photometric and spectral properties typical for both types of PMS eruptive objects (Covey et al. 2011, AJ, 141, 40, Kospal et al. 2011, A&A 527, A133, Aspin 2011, AJ, 141, 196).
The data from our photometric monitoring indicate that after several months near the quiescence level (I~19-20 mag) a new increase in brightness is observed during the last days.
The photometric observations obtained with the 2-m telescope of the National Astronomical Observatory Rozhen (Bulgaria) on the night of June 14/15, 2012 gives the following magnitudes:
I=15.92, R=17.61, V~20.0
As references, we used the VRI comparison sequence reported in Kospal et al. 2011, A&A 527, A133.
This repeated outbursts within two years indicate a similarity with the photometric variability of another eruptive PMS object V1647 Ori.
