Abstract. In a preceding paper a simple model for contact binaries has been proposed, based on the usual assumption that the energy sources/sinks caused by the interaction of the components occur only in the secondary's/primary's outer layers. Here the model is applied to a typical late-type system. First we imposed the restriction that the fractional extent in mass of the sources/sinks in the layers above the critical surface is the same in both components, and found solutions evolving in thermal cycles. If the energy transfer is assumed to be sufficiently effective, loss of contact is avoided. Otherwise the cycle consists of a long quiet phase in good contact and a short violent phase with rapid changes between contact, semidetached, and detached configurations. In both cases there are cycles in which the temperatures of the components are similar in the largest part of the time. Other observational tests are also passed. Next we removed the restriction. In the resulting model with three free parameters we found (besides cycles) a large range of solutions in stable thermal equilibrium which are compatible with the observations. From a theoretical viewpoint however all these solutions are unsatisfactory since suffering from several inconsistencies. This result shows that the usual assumption on the energy sources and sinks is too restrictive. We are led to look for modifications of the model which remove the inconsistencies. This will be done in a forthcoming paper.
Abstract. The structure equations of contact binaries are discussed. An equation for the transfer of mass between the components is derived. Serious uncertainties concern only the transfer of energy. They are expressed as unknown functions. An evolution code for contact binaries is presented. The restrictions imposed by a spherically averaged treatment of the components are discussed. Apart from these restrictions the code can be adapted to any choice of the functions describing the energy transfer. A simple tentative choice for these functions is proposed.
Half a centry ago Henry Norris Russell and Heinrich Vogt independently made a conjecture concerning the structure of spherical stars which are in hydrostatic and thermal equilibrium (Russell, 1927; Vogt, 1926). This conjecture has later come to be known as the Vogt-Russell theorem and is usually formulated as follows: The structure of a star is uniquely determined by the mass and the composition. In other words, the statement claims the existence and uniqueness of a stellar equilibrium configuration for given parameters mass and composition, and you may find what is called a mathematical proof in many textbooks on stellar structure.
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