Fig. 11.
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Orbital period versus the spectroscopic mass of the primary, ℳ1. The colors are based on the minimum mass of the secondary star, ℳ2, min. The boundaries for potential Type Ia SNe progenitors in red giant stars and white dwarf binaries from Liu et al. (2019) and Ablimit et al. (2022) are shown as solid and dashed lines. The ellipsoidal binaries with a ℳ2, max ≤ 1.2 M⊙ are marked with black pentagons.
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