The variation of the orbital periods found in high-mass X-ray binaries occurring over time can be explained by two models. According to the first model, orbital decay occurs due to dynamic tidal forces. The second model shows that the change occurs due to the inertia moments of a massive star during its evolution. These models are applied to LMC X-4 and Cen X-3.
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The author acknowledges the referee for a number of useful comments.
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This study was supported by the Russian Foundation for Basic Research (contract no. 19-02-00199-a), RAS project KP 19-270 “Investigation of the problems of the origin and evolution of the Universe using observations from the Earth and space” and State order for the science program of experimental and construction studies “Millimetron.”
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Chernov, S.V. Orbital Decay in High-Mass X-Ray Binaries. Astron. Rep. 64, 425–433 (2020). https://doi.org/10.1134/S1063772920050017
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DOI: https://doi.org/10.1134/S1063772920050017