Fig. 6.
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Orbital period (Porb) just after the CE evolution as a function of the WD mass (MWD) from the post-CE population synthesis carried out by Belloni et al. (2024a), assuming αCE = 1.0. We show only systems with companion masses of 1.33 ± 0.24 M∗ < 106 M⊙ to be consistent with observations. The blue star indicates the initial post-CE orbital period and WD mass that are required to explain FN Sgr.
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