Flickering in FU Orionis
Scott J. KenyonHarvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138E. A. KolotilovCrimean Laboratory, Sternberg State Astronomical Institute, p/o Nauchny, 334413, CrimeaМ. А. ИбрагимовUlugh Beg Astronomical Institute, Academy of Sciences of Uzbekistan, Astronomicheskaya ul. 33, Tashkent, 700052, UzbekistanJ. A. MatteiAmerican Association of Variable Star Observers, 25 Birch Street, Cambridge, MA 02138
ABI
Аннотация
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.
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