High Cadence Time-Series Photometry of V1647 Orionis

Details High Cadence Time-Series Photometry of V1647 Orionis High Cadence Time-Series Photometry of V1647 Orionis

Jan 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21542911b&link_type=abstract

American Astronomical Society, AAS Meeting #215, #429.11; Bulletin of the American Astronomical Society, Vol. 42, p.351

Astronomy and Astrophysics

Astronomy

Scientific paper

We present high cadence time-series photometry of the 2003-2004 and 2008-2009 FUor/EXor outbursts of V1647 Orionis, the star illuminating McNeil's Nebula. The first dataset was taken as the object was most steeply increasing in brightness while the second was presumably taken after its luminosity had plateaued. We detect two significant periods in our 2003 lightcurve superimposed on a flicker-noise spectrum, while the power spectrum of our 2009 lightcurve is devoid of significant structure. We find that neither of these periods can be attributed to the star's rotation. The dominant period is 4.3d, and we find that it may be akin to the dwarf-nova oscillations observed around cataclysmic variable stars. This 4.3d period would suggest that the inner edge of the star's Keplerian accretion disk was located 2.5 stellar radii away from the star before its luminosity had reached its peak and that, considered together with the flickering, the stellar magnetosphere was interacting with the disk during this phase of the outburst. The second period of 0.13d is consistent with the star's theoretical radial pulsation timescale, and, given that this period is not detected in 2009, we propose that the very high accretion rate at the time of our 2003 observations induced short-term radial pulsations in the star.

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