A new deep minimum in the light curve of the PMS star V1647 Ori

ATel #12012; Evgeni Semkov (Institute of Astronomy and National Astronomical Observatory, Bulgarian Academy of Sciences), Sunay Ibryamov (Department of Theoretical and Applied Physics, Faculty of Natural Sciences, University of Shumen)
on 5 Sep 2018; 20:30 UT
Credential Certification: E. Semkov (esemkov@astro.bas.bg)

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The PMS object V1647 Ori is located in the dark cloud Lynds 1630 - a region of active star formation in the Orion B complex. The first outburst of V1647 Ori was registered on 2004 by McNeil (McNeil, J. W., 2004, IAU Circ., 8284) and it continues until the end of 2006. From the spring of 2006 to the autumn of 2008, the star is at a very low level of brightness, with no photometric data about it. A second outburst of V1647 Ori was registered in 2008, when its brightness increased again to the level of the first eruption (Kun 2008, IBVS, 5850). Our photometric data obtained during the second outburst show that the star's brightness drops gradually by about 1 mad. (I-band) in the period from the end of 2008 to the beginning of 2018. Our observations were made with the telescopes of the National Astronomical Observatory Rozhen (Bulgaria). We observed the position of V1647 Ori during the night of September 3, 2018 with the 50/70 cm Schmidt telescope, and during the night of September 4, 2018, with the 2-m RCC telescope at the Rozhen Observatory. Our photometric data indicates that the star is below the registration limit in I and R bands. Therefore, the star's brightness is less than 19.5 mag. in I-band and less than 20 mag. in R-band respectively. This means that we record a second dramatic drop in brightness, similar to that observed in 2006-2008. Classification of V1647 Ori variability remains questionable. Whether it is a FUor or an EXor or maybe an intermediate object between the two classes.