Stellar Wind of Components of Detached Binary Systems

Abstract

The paper is devoted to the consideration of the role of the donor stellar wind in the matter exchange between the components of detached binary systems. A classification of close binary systems with interacting components is proposed. A list of potential donors and accretors of such systems, including X-ray binary and symbiotic stars, is given. Analytical tasks have been completed to evaluate the conditions and efficiency of interaction through the stellar wind, a criterion was found for maintaining the self-induced stellar wind of X-ray binaries, and a condition for the formation of an accretion disk during accretion of stellar wind matter by a compact accretor. Three-dimensional gas dynamic models of component interaction are constructed for the five initial velocities of the stellar wind using the example of Sco X-1 type systems. The simulation results are illustrated by pictures of streamlines, temperature distribution, and wind gas densities in the orbital and frontal planes. Model focusing of the donor wind flow by the accretor is confirmed by the observed phase X-ray light curve of Vela X-1.

Figures (20)

• Figure 1: Classification of binary stars: contact (a), semi-detached (b), detached (c), and with a common envelope (d).
• Figure 2: Classification of detached interacting binaries: quasi-conservative (a), semi-open (b), and open (c).
• Figure 3: Classification of donor stellar winds in close binaries. The semi-major axis A is taken equal to the solar radius. The plot accounts for cooling of wind gas due to radiation. The red dashed line shows the dependence defined by (Eq. \ref{['eq-7']}); the blue dashed line indicates the transparency condition (Eq. \ref{['eq-8']}). Blue dots mark calculation variants of the binary system modeled in this study.
• Figure 4: Coordinate system and computational grid used in the model.
• Figure 5: Formation of a quasi-stationary state of gas flows in the binary system within the computational domain for a wind temperature $T_{\text{w}} = 3 \times 10^5$ K over the time interval $0.2 - 1.0 P_{\text{orb}}$.