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Three-Dimensional Doppler Tomography of the X-ray Binary Cyg X-1статья
- Авторы: Sharova O.I., Agafonov M.I., Karitskaya E.A., Bochkarev N.G., Zharikov S.V., Butenko G.Z., Bondar’ A.V.
- Сборник: Variable Stars, the Galactic halo and Galaxy Formation
- Год издания: 2010
- Первая страница: 212
- Последняя страница: 212
- Аннотация: 2D and 3D Doppler tomograms of the X-ray binary system Cygnus X-1 (V1357 Cyg) were reconstructed based on the spectral data in the HeII λ 4686Å line obtained with the 2-m telescope of the Peak Terskol Observatory (Russia) and 2.1-m telescope of the Mexican National Astronomical Observatory in June 2007. For the first time, information about gas motions in the directions out of the orbital plane was acquired. The realization of the 3D Doppler tomography became possible due to the developed Radioastronomical Approach to the reconstruction in the few projections tomography (Agafonov \amp Sharova 2005). The comparison of the observed line profiles to the computed ones (calculated from the reconstructed tomograms) carried out with the use of the χ-square method shows a good quality of reconstruction. The 2D tomograms for June 2007 are similar to the tomograms reconstructed earlier (for 1997, 2003 and 2004). They give the evidences that the emission component of the HeII λ 4686Å line is generated mainly in the external parts of the Cyg X-1 accretion structure closest to the donor star (O-supergiant), and the absorption component is formed in the atmosphere of the supergiant. The 3D Doppler tomograms reconstructed in the velocity space (V_x,V_y,V_z) also show that the formation of the line profiles of HeII λ 4686Å is connected both with the donor star and the area of interaction of the flow matter with the accretion structure around the compact object. The first of the structural components associated with the supergiant is visible in absorption. The maximum of the absorption is located in the central plane (V_x,V_y), with V_z=0. The structure component of the line profiles belonging to the accretion structure is also visible in emission. Its intensity is maximal near V_z=0. However, it consists of separate fragments with different V_z mainly in the range from -180 to +130 km s\^$$-1$$. We also revealed a surprising emission component identified with the supergiant with the velocity component V_z\ap 300 km s\^$$-1$$ that may be related to the gas stream from the star. However, this finding requires further confirmation.
- Добавил в систему: Бочкарев Николай Геннадиевич