卷 102, 编号 10 (2025)

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.

The results of absorption modeling in the hydrogen H_α 6563 Å and helium 10830 Å lines for the hot Jupiter HAT-P-32 b are presented. The modeling was performed using a three-dimensional hydrodynamic code together with the Monte Carlo model of Ly_α photon transport. A wide range of stellar radiation and atmospheric parameters was considered. It was found that the measured spectrally resolved transit absorption in both lines can be well described by model calculations with the stellar radiation in the XUV range limited to 200 erg/cm²/s per 1 AU, the helium content in the planet's atmosphere He/H=2/98 and metallicity [Fe/H] = -1. It is shown that absorption in the helium line occurs uniformly in a large volume of the outflowing atmosphere, and in the hydrogen line — in a layer of 1.5–2.75 planet radii.

By a new method we study the actual variant of the two-planet problem on the secular evolution of planetary orbits with small eccentricities and mutual inclination, having arbitrary orientation with respect to the main (picture) plane. A model has been developed that describes a wide class of exoplanetary systems with an orbital inclination angle different from π / 2. The orbits of the planets are modeled by Gaussian rings, the perturbing function is represented by the mutual gravitational energy of these rings in the form of a series up to terms of second order of smallness. To describe the evolution of orbits, instead of osculating Keplerian elements, a new set of variables is introduced: the unit vector R of normal to the plane of the ring and two Poincaré variables (p,q); for eight independent variables, a system of differential equations is obtained and analytically solved. The method is applied to study the secular evolution of the two-planet system Kepler-117 (KOI-209) with non-resonant orbits of exoplanets. It has been established that in this system the oscillations of the components of the orientation vector R of the same name for each of the orbits, as well as the values (e,i,Ω), occur strictly in the opposite phase. The eccentricities of both orbits oscillate with a period of Tk = 182.3 years, and the inclinations of the orbits and the longitudes of the ascending nodes change in the libration mode with the same period Tg = 174.5 years. The lines of the orbital angles rotate unevenly counterclockwise with periods of secular rotation Tg2 = 178.3 years (for a light planet), and Tg1 = 8140 years (for a more massive planet).