Volume 447, Number 2, February IV 2006
|Page(s)||545 - 551|
|Section||Interstellar and circumstellar matter|
|Published online||07 February 2006|
Broad band variability of SS433: accretion disk at work?
Max-Planck-Institute für Astrophysik, Karl-Schwarzschild-Str. 1, 85740 Garching bei München, Germany e-mail: email@example.com
2 Space Research Institute, Russian Academy of Sciences, Profsoyuznaya 84/32, 117810 Moscow, Russia
3 Special Astrophysical Observatory, Nizhnij Arkhyz, Karachaevo-Cherkesiya 369167, Russia
4 Sternberg Astronomical Institute, 119992 Moscow, Russia
5 University of Oulu, Finland
6 Kazan State University, Kremlevskaya Str. 18, 420008 Kazan, Russia
7 Academy of Sciences of Tatarstan, Bauman Str. 20, 420111 Kazan, Russia
8 TUBITAK National Observatory, Akdeniz Universitesi Yerleskesi, 07058 Antalya, Turkey
Accepted: 8 September 2005
We present broad band power spectra of variations of SS433 in radio, optical and X-ray spectral bands. We show that at frequencies lower than 10-5 Hz the source demonstrates the same variability pattern in all these bands. The broad band power spectrum can be fitted by one power law down to frequencies ~ 10-7 Hz with flattening afterwards. Such a flattening means that on time scales longer than ~ 107 s the source variability becomes uncorrelated. This naturally leads to the appearance of quasi-poissonian flares in the source light curve, which have been regularly observed in radio and optical spectral bands. The radio flux power spectrum appears to have a second break at Fourier frequencies ∼10-5 Hz which can be caused by the smearing of the intrinsic radio variability on timescale of the light-crossing time of the radio emitting region. We find a correlation of the radio and optical fluxes of SS433 and the radio flux is delayed by about ∼2 days with respect to the optical one. Power spectra of optical and X-ray variabilities continue with the same power law from 10-7 Hz up to ~ Hz. The broad band power spectrum of SS433 can be interpreted in terms of self-similar accretion rate modulations in the accretion disk proposed by Lyubarskii (1997, MNRAS, 292, 679) and elaborated by Churazov et al. (2001, MNRAS, 321, 759). We discuss a viscous time-scale in the accretion disk of SS433 with reference to the observed broad band power spectrum.
Key words: accretion, accretion disks / black hole physics / instabilities / stars: binaries: general / X-rays: general / X-rays: stars
© ESO, 2006
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