Binary evolution pathways to blue large-amplitude pulsators: Insights from HD 133729

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Table 5.

Parameters for stable mass transfer at q = 0.30.

M_1,i (M_⊙)	M_2,i (M_⊙)	P_i (days)	M_1,f (M_⊙)	$P_{f} (day)$ $P_{\mathrm{f}}\ (\rm day)$
2.23	0.67	1.3–2.5	0.259–0.284	12.28–20.38
2.31	0.69	1.3–2.5	0.266–0.293	13.48–20.13
2.38	0.72	1.3–2.8	0.272–0.304	14.14–22.91
2.46	0.74	1.3–3.1	0.278–0.316	14.33–24.80
2.54	0.76	1.6–3.4	0.305–0.328	14.95–26.45
2.62	0.78	1.6–3.7	0.314–0.339	14.89–28.25

Notes. q = M_2, i/M_1, i = 0.30. P_i is the range of initial orbital periods that enables stable mass transfer. M_1, f is the final mass of the primary star after mass transfer. P_f is the orbital period at the end of mass transfer.

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