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Abstract <p>Numerous observational data indicate the presence of a tilted accretion disk in the Her X-1 system. Due to this tilt, the donor star experiences enhanced radiative heating, causing its surface to heat up and altering the direction of plasma flow across its surface as the accretion disk’s shadow moves. These phenomena—the tilt and the changes in flow on the donor’s surface—are mutually consistent (self-consistent). Furthermore, the accretion disk precesses with a period of 35 days. This work presents a model for the formation of the tilted accretion disk in Her X-1. The tilt is attributed to the upward and downward displacement of the mass transfer stream relatively to the inner Lagrangian point (<InlineEquation ID="IEq1"> <EquationSource Format="TEX">\(L_{1}\)</EquationSource> <!--LobJMat2561472Lukin-m1--> </InlineEquation>), a phenomenon demonstrated in previous simulations of the shadow motion’s impact on the outflow from the donor star’s surface. The mathematical model comprises a system of equations describing the dynamics of an ideal, partially ionized, radiating gas within the gravitational field of the binary star system. A numerical code has been developed, enabling simulations of accretion disk flows on distributed-memory cluster computing systems. The simulation results demonstrate the formation of a tilted accretion disk, with the tilt angle matching the previously specified shadow pattern on the donor star’s surface. This result validates the self-consistency of the mass outflow and disk formation model.</p>

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Mathematical Modeling of the Coupling Between Tilted Disk Precession and Shadow Motion Across the Donor Star’s Surface in Her X-1

  • 期刊论文

  • 发表日期：

    2026年1月1日

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  • Vladimir Lukin,
  • Konstantin Postnov,
  • Nikolai Shakura

摘要

Abstract

Numerous observational data indicate the presence of a tilted accretion disk in the Her X-1 system. Due to this tilt, the donor star experiences enhanced radiative heating, causing its surface to heat up and altering the direction of plasma flow across its surface as the accretion disk’s shadow moves. These phenomena—the tilt and the changes in flow on the donor’s surface—are mutually consistent (self-consistent). Furthermore, the accretion disk precesses with a period of 35 days. This work presents a model for the formation of the tilted accretion disk in Her X-1. The tilt is attributed to the upward and downward displacement of the mass transfer stream relatively to the inner Lagrangian point ( \(L_{1}\) ), a phenomenon demonstrated in previous simulations of the shadow motion’s impact on the outflow from the donor star’s surface. The mathematical model comprises a system of equations describing the dynamics of an ideal, partially ionized, radiating gas within the gravitational field of the binary star system. A numerical code has been developed, enabling simulations of accretion disk flows on distributed-memory cluster computing systems. The simulation results demonstrate the formation of a tilted accretion disk, with the tilt angle matching the previously specified shadow pattern on the donor star’s surface. This result validates the self-consistency of the mass outflow and disk formation model.