A Multi-Wavelength Study of the 2003-2006 Outburst of V1647 Orionis

Details A Multi-Wavelength Study of the 2003-2006 Outburst of V1647 Orionis A Multi-Wavelength Study of the 2003-2006 Outburst of V1647 Orionis

Mar 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008msngr.131...20v&link_type=abstract

The Messenger, vol. 131, p. 20-24

Computer Science

Scientific paper

The birth of a star is accompanied by the formation of a circumstellar disc which interacts with the star, but most young stars accrete matter at rates that do not influence the mass of the disc on short timescales. However, in so-called FU Orionis stars, a significant fraction of the total disc mass is accreted onto the central star within a short time. During these FU Orionis events, the light generated by accretion outshines the star by up to 6 magnitudes for a period of several years to decades. The star, V1647 Orionis, underwent such an event. We have used FORS2 and NACO on the VLT and TIMMI2 at the ESO 3.6-m telescope to monitor V1647 Orionis from four months after outburst until the system returned to its pre-outburst brightness level, nearly three years later. Our optical photometry and spectroscopy confirm that V1647 Orionis has indeed undergone an outburst whose characteristics resemble those of the FU Orionis stars.

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