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Variability in the light curve of tidal disruption events

  • Zu-Jia Lu (a1) (a2), Da-Bin Lin (a1) (a2), Ling-Hua Xie (a1) (a2) and En-Wei Liang (a1) (a2)

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The X-ray light curve of Sw~J1644+57 indicates this event would be due to a tidal disruption. The lightcurve shows large amplitude fluctuation. As proposed by Lyubarskii (1997), the aperiodic variability observed in the Galactic X-ray binaries and active galactic nuclei is likely from the fluctuation of the viscous parameter in their disks. We explain the significant fluctuation of the late X-ray lightcurve (t>106 seconds) of Sw J1644+57 with this model. We assume the stochastic variations in the viscous parameter featuring as α(R,t) = α0 [1+β(R,t)], where the time-scale for varying β(R,t) is set as ten times of the dynamic time-scale for disk at the radius R (Janiuk & Misra 2012). Based on the simulation results of Lodato et al. (2009), we describe the fallback behavior of the tidal disruption as fb ∝ {[(t - t b )/t fb ]κ n + [(t - t b )/t fb ]5n/3}−1/n for t > t b and fb=0 for other situations, where κ=10.0, n=0.5, t fb=103τ, and t b =102τ in which τ=2π(R f 3/GM BH)1/2 and R f =5r g is the pericentre distance. Figure 1 compare the power-density spectra (PDS) derived from the observed and our simulated lightcurves. It is found the our simulations are well consistent with the observations.

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Supported by the National Basic Research Program (973 Programme) of China (Grant No. 2014CB845800), the National Natural Science Foundation of China (Grant Nos. 11533003, 11403005), the Guangxi Science Foundation (2013GXNSFFA019001 and 2014GXNSFBA118004), the Strategic Priority Research Program “The Emergence of Cosmological Structures” (Grant No. XDB09000000).

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References

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Janiuk, A., & Misra, R., 2012, A&A, 540, A114
Lyubarskii, Y. E., 1997, MNRAS, 292, 679
Lodato, G., King, A. R., Pringle, J. E., 2009, MNRAS, 332, 340
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Keywords

Variability in the light curve of tidal disruption events

  • Zu-Jia Lu (a1) (a2), Da-Bin Lin (a1) (a2), Ling-Hua Xie (a1) (a2) and En-Wei Liang (a1) (a2)

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