Nazarenko V.V., Nazarenko S.V. «3D numerical hydrodynamical models of the precessing thick accretion disk and on- and off-state generations in microquasars» Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 113-116 (2017)

DOI: https://doi.org/10.18524/1810-4215.2017.30.114365 The thick accretion disk and donor’s wind on the example of CYG X-1 are computed. The main aim of the present simulations is to calculate the precessing thick accretion disk and ON- and OFF-state generation by the methods of 3D numerical hydrodynamics. The main task of the present research is to investigate the dependencies of the central disk temperature and mass accretion rate versus time. Non-stationary Euler’s hydrodynamical equations are resolved by astrophysical variant of large-particle method by Belotserkovskii–Davydov. The ON- and OFF-state generation for the precessing thick accretion disk was setting. The correlation between radio flux and X-ray was setting. Our present calculations also show that in the cases of the thick accretion disk the jet velocities will be close to 0.24–0.26 of light speed (see for instance SS433) and on contrary in the cases of a thin accretion disk jet velocities will be close to 0.98–99 of light speed (see for instance CYG X-1).

Nazarenko V.V., Nazarenko S.V. «3D numerical hydrodynamical models of the precessing thick accretion disk and on- and off-state generations in microquasars» Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 113-116 (2017)

DOI: https://doi.org/10.18524/1810-4215.2017.30.114365 The thick accretion disk and donor’s wind on the example of CYG X-1 are computed. The main aim of the present simulations is to calculate the precessing thick accretion disk and ON- and OFF-state generation by the methods of 3D numerical hydrodynamics. The main task of the present research is to investigate the dependencies of the central disk temperature and mass accretion rate versus time. Non-stationary Euler’s hydrodynamical equations are resolved by astrophysical variant of large-particle method by Belotserkovskii–Davydov. The ON- and OFF-state generation for the precessing thick accretion disk was setting. The correlation between radio flux and X-ray was setting. Our present calculations also show that in the cases of the thick accretion disk the jet velocities will be close to 0.24–0.26 of light speed (see for instance SS433) and on contrary in the cases of a thin accretion disk jet velocities will be close to 0.98–99 of light speed (see for instance CYG X-1).

Kondratyev V.N., Nurtayeva U.M., Zhomartova A.Zh., Mishenina T.V. «Synthesis of magnetized nuclei at supernova explosion» Публикации Одесской астрономической обсерватории (Odessa Astronomical Publications, Украина), 30, с. 91-92 (2017)

DOI: https://doi.org/10.18524/1810-4215.2017.30.114335 Influence of magnetorotational instabilities in astrophysical plasma at supernova explosion on synthesis of chemical elements is investigated. At field strength less than 10 teratesla nuclear magnetic susceptibility exhibits linear regime with enhanced nuclear binding energy for open shell nuclei. Effects of ultra-strong nuclear magnetization are demonstrated to enhance the portion of titanium product. The relation to an excess of titanium isotopes revealed from the Integral mission data and galactic chemical evolution is discussed.