Fig. 5.

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Amount of mass lost by the primary star during stable Case C mass transfer as a function of the envelope mass prior to Case C RLOF. Models with different initial orbital periods are shown in different colors, as in Fig. 2. Models with qi = 0.95 are marked with a star, and models with smaller initial mass ratios are shown with smaller square markers. The gray horizontal lines mark the maximum mass that the secondaries accrete during the first (right) or second (left) phase of mass transfer.
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