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The 2D and 3D Doppler tomograms of X-ray binary system Cyg X-1 (V1357 Cyg) were reconstructed from spectral data for the line HeII 4686Å obtained with 2-m telescope of the Peak Terskol Observatory (Russia) and 2.1-m telescope of the Mexican National Observatory in June, 2007. Information about gas motions outside the orbital plane, using all of the three velocity components Vx, Vy, Vz, was obtained for the first time. The tomographic reconstruction was carried out for the system inclination angle of 45°. The equal resolution (50 × 50 × 50 km/s) is realized in this case, in the orbital plane (Vx, Vy) and also in the perpendicular direction Vz. The checkout tomograms were realized also for the inclination angle of 40° because of the angle uncertainty. Two versions of the result showed no qualitative discrepancy. Details of the structures revealed by the 3D Doppler tomogram were analyzed.
VLT FORS 1 observations indicate the presence of a variable significant magnetic field in the X-ray binary Cyg X-1. The importance of this investigation comes from the fact that it rules one of the most significant BH manifestations: the X-ray millisecond flickering, usually related to reconnection of magnetic lines in the innermost part of the accretion disc.
In our paper (Sharova, 1995) a method of determining the distances to galactic planetary nebulae has been based on the recently established (Sharova, 1992) regression relationship between the central stars radius and the temperature. Now our scale is compared to 18 other scales, in four of which the central stars parameters also are used, instead of nebulae ones. The scale distance estimations DS are compared with independently known individual distance D. The values log(DS/D) and their dependence on radius of the nebulae are analysed. Each scale is described by two parameters: a geometrical average value < log DS/D > and the relation ρ/ρc, where ρ is the correlation coefficient for log DS/D — log RN, and ρc is its critical value. If ρ/ρc > 1, the correlation is significant with the confidence probability 95%. For example we obtained the following results: ρ/ρc = 0.153, 0.494, 2.126, 2.228; < DS/D >=0.999, 2.145, 2.126, 1.414 for our scale and for widely known MKH, CKL, VdSZ scales respectively. By both criteria our scale achieves better agreements, on average, with individual estimations of distances than others.
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