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<p>This paper investigates the motion of a rotating test body in the Schwarzschild space-time. Previously, it was shown that this problem reduces to investigating a two-dimensional Poincaré map. The paper presents a detailed analysis of bifurcations of periodic solutions using this map. In the Poincaré map, as the energy of the body increases, one can observe two pitchfork bifurcations that follow one after the other: a supercritical and a subcritical one. This gives rise to five fixed points in the Poincaré map. In addition, new circular orbits are found for which the total angular momentum is not parallel to the angular momentum of the test body. For these circular orbits, the radial coordinate satisfies the condition <InlineEquation ID="IEq1"> <EquationSource Format="TEX">\(r \geqslant 3\)</EquationSource> <EquationSource Format="MATHML"><math> <mrow> <mi>r</mi> <mo>⩾</mo> <mn>3</mn> </mrow> </math></EquationSource> </InlineEquation> (in units of the mass of a black hole). For values of the total angular momentum of the test body that corresponds to neutron stars or black holes, these asymmetric circular orbits turn out to be unstable.</p>

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Dynamics of spinning test bodies in the Schwarzschild space-time: reduction and circular orbits

  • 期刊论文

  • 发表日期：

    2026年7月23日

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  • Ivan Bizyaev

摘要

This paper investigates the motion of a rotating test body in the Schwarzschild space-time. Previously, it was shown that this problem reduces to investigating a two-dimensional Poincaré map. The paper presents a detailed analysis of bifurcations of periodic solutions using this map. In the Poincaré map, as the energy of the body increases, one can observe two pitchfork bifurcations that follow one after the other: a supercritical and a subcritical one. This gives rise to five fixed points in the Poincaré map. In addition, new circular orbits are found for which the total angular momentum is not parallel to the angular momentum of the test body. For these circular orbits, the radial coordinate satisfies the condition \(r \geqslant 3\) r ⩾ 3 (in units of the mass of a black hole). For values of the total angular momentum of the test body that corresponds to neutron stars or black holes, these asymmetric circular orbits turn out to be unstable.