Fig. 6.
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Values of MMMR for a range of secondary masses, assuming a 1 M⊙ primary star and an edge-on inclination. Tracks are plotted for the period range in which neither star fills its Roche lobe. Even for unusually high-mass secondaries, MMMR > 1 is only possible for a Sun-like primary star over a narrow range of periods 0.37 ≲ Porb ≲ 0.44 days.
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