On the nature of V1647 Ori

Details On the nature of V1647 Ori On the nature of V1647 Ori

Oct 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006coska..36..149c&link_type=abstract

Contributions of the Astronomical Observatory Skalnaté Pleso, vol. 36, no. 3, p. 149-157.

Astronomy and Astrophysics

Astronomy

2

Techniques: Photometric, Stars: Pre-Main Sequence, Stars: Variables, Stars: Individual: V1647 Ori

Scientific paper

V1647 Ori is a young eruptive star which brightened by ≈ 5 mag in the IC passband during its outburst, started in November 2003. We present our (RI)C CCD photometric observations of V1647 Ori spanning from October 28, 2004, till October 31, 2005, which cover the light curve during the outburst at a prolonged brightness maximum of ˜ 14.5 mag and a rapid decline for about 3.5 mag. The regions B and C in McNeil's nebula reflect the radiation from V1647 Ori (region A) with the time delay of 59 and 85 days, respectively. 2-year duration and 37-year recurrence allow us to classify the outburst of V1647 Ori as intermediate between FU Orionis (FUor) and EX Lupi (EXor) type events. Distinct IR spectroscopic behaviour suggests that V1647 Ori can be the prototype of a new class of objects.

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