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Super-orbital variability in Cygnus X-1

Super-orbital variability in Cygnus X-1. ISSI, Bern, Switzerland March 3-7, 2008. J. Poutanen, A. Zdziarski, A. Ibragimov MNRAS, submitted. Accretion via Roche lobe and focused wind. Stream trajectory and disk formation for the case of equal masses.

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Super-orbital variability in Cygnus X-1

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  1. Super-orbital variability in Cygnus X-1 ISSI, Bern, Switzerland March 3-7, 2008 J. Poutanen, A. Zdziarski, A. Ibragimov MNRAS, submitted

  2. Accretion via Roche lobe and focused wind • Stream trajectory and disk formation for the case of equal masses. • Coriolis force shifts the stream from the line connecting the stars.

  3. Superorbital variability Radio X-rays

  4. Dips distribution

  5. Orbital profiles as a function of superorbital phase

  6. (c) A view from the top bulge b disc supergiant  =0.5 =0

  7. (a) A view along the orbital plane, =0 observer i bulge  supergiant  black hole disc  =0.5 =0

  8. (b) A view along the orbital plane, =0.5 observer disc supergiant black hole bulge  =0.5 =0

  9. Model • Bulge • Wind • Parameters: inclination i=40 deg • Precession angle  Precession angle  Optical depths: bulge b,0 , wind w,0 Bulge azimuth b

  10. Model • Emissivity profile of the accretion disk • For the jet/ outflow

  11. Orbital profiles as a function of superorbital phase

  12. Results

  13. PDS of the model flux

  14. Conclusions • Discovery of orbital modulation strength on superorbital phase of Cyg X-1 • Effect can be explained by the bulge displaced from the line connecting the stars by 25 deg. • Distribution of dips is consistent with the model • Beat-frequencies should be observed, with the stronger lower one.

  15. Log-normal flux distribution

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