Abstract
Three situations involving mass loss from binary systems are discussed. (1) Non-conservative mass exchange in semi-detached binaries. No quantitative estimate of this mechanism is possible at present. (2) Common envelope binaries. There are both theoretical and observational indications that this phase of evolution happens to many systems, even to some that are not very close initially (orbital periods ~ years). (3) Stellar winds in binaries. Observational evidence suggests that stellar winds from components of close binaries (especially semi-detached) are significantly stronger than from single stars at the same location in the H-R diagram. Theoretical arguments indicate that in some cases stellar wind may stabilize the component of a binary against the Roche lobe overflow. In some cases there is weak evidence of an anisotropy in the stellar wind.
There are two major mechanisms of mass loss from O-type binaries. One of them is non-conservative mass exchange between the components after one of the components overflew its critical Roche lobe. The second mechanism is strong stellar wind from one or both components. The first mechanism can probably operate in any close binary, independent of its mass. The second mechanism is efficient only for massive systems, which practically limits its importance to only O-type binaries (at least one of the components has to be initially an O-type star). A special and very important case of the first mechanism occurs if a common envelope binary is formed during the process of mass exchange. In this paper we shall briefly discuss all three situations: (1) non-conservative mass exchange in semi-detached systems, (2) mass loss from common envelope binaries, (3) stellar winds in binaries.
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Ziółkowski, J. (1979). Evolution of Binary Stars with Mass Loss. In: Conti, P.S., De Loore, C.W.H. (eds) Mass Loss and Evolution of O-Type Stars. International Astronomical Union/Union Astronomique Internationale, vol 83. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-9452-2_55
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