Fig. 13.
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Orbital period-white dwarf mass relation from a sample of 60 Ba stars analyzed by Escorza & De Rosa (2023). The factor (1−e)3/2 has little impact and is introduced to determine the orbital period if the system had a separation given by the periastron distance where RLOF is most likely to occur. No clear correlation is present unlike in sdB and He white dwarf binary systems.
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