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Stellar Wind as a Stimulator of Accretion Activity in Young Binary Systems

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Abstract

A young binary system is considered, having a mass ratio of components M 2/M 1 ≪ 1, in which the low-velocity part of the stellar wind of the low-mass component (the so-called disk wind) can be partially captured by the gravitation of the primary component. It is shown that a large-scale redistribution of matter and angular momentum between the inner and outer parts of the gas-dust disk surrounding the binary system occurs as a result, with a consequent increase in the rate of accretion onto the primary component. In cases in which the orbital eccentricity of the secondary component is nonzero, modulation of the rate of accretion onto the primary component should be observed with a period equal to the orbital period, while in the case of a highly elongated orbit the mass accretion acquires a pulsed character. Since dust may be present in the disk wind from the secondary component, the capture of stellar wind will result in an increase in the effective geometrical thickness of the gas-dust disk. For this reason, the infrared (IR) emission excesses of such stars (especially in the near-IR range) and their intrinsic polarization can be considerably greater than in the case of a single star surrounded by a circumstellar disk of the same mass, and a periodic component may also be present in their behavior with time. Moreover, because of disruption of the axial symmetry in the dust distribution in the vicinity of the young binary system, the orbital period may also be present in its brightness variations. The role of these effects in the physics of young stars is discussed.

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  1. Crimean Astrophysical Observatory, Ukraine

    V. P. Grinin

  2. St. Petersburg University, Russia

    V. P. Grinin

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Grinin, V.P. Stellar Wind as a Stimulator of Accretion Activity in Young Binary Systems. Astrophysics 43, 446–457 (2000). https://doi.org/10.1023/A:1010971009185

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