Flickering in FU Orionis

Abstract

We analyze new and published optical photometric data of FU Orionis, an eruptive pre-main sequence star. The outburst consists of a 5.5 mag rise at B with an e-folding timescale of roughly 50 days. The rates of decline at B and V are identical, 0.015 +- 0.001 mag per yr. Random fluctuations superimposed on this decline have an amplitude of 0.035 +- 0.005 mag at V and occur on timescales of 1 day or less. Correlations between V and the color indices U-B, B-V, and V-R indicate that the variable source has the optical colors of a G0 supergiant. We associate this behavior with small amplitude flickering of the inner accretion disk.

19 pages of text, 3 tables, and 6 figures to be published in the Astrophysical Journal, 10 March 2000

References in corpus (2)

• The Instability Strip for Pre--Main-Sequence Stars
• Spectra and Line Profiles of FU Orionis Objects: Comparisons Between Boundary Layer Models and Observations

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