Evolution and final fate of massive post-common-envelope binaries

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Volume 688 (August 2024)

A&A, 688 (2024) A87

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Table 1.

Properties of post-CE binaries just after the CE phase (marked by “i”), and prior to core collapse (indicated by “f”).

Binary systems	M_1, i	P_orb, i	$M_{core, i}^{CO}$ $M_{\mathrm{core,i}}^{\mathrm{CO}}$	M_1, f	P_orb, f	$M_{core, f}^{CO}$ $M_{\mathrm{core,f}}^{\mathrm{CO}}$	$M_{He, f}^{env}$ $M_{\mathrm{He,f}}^{\mathrm{env}}$	ΔM_{NS or BH}	SNe type	τ_grw	f_merger	f_bound	f_disrupt
	(M_⊙)	(days)	(M_⊙)	(M_⊙)	(days)	(M_⊙)	(M_⊙)	(M_⊙)		(Gyr)	(%)	(%)	(%)
2.85 M_⊙ + BH	2.85	4.39	1.45	2.48	5.76	1.57	0.91	1.04e-2	Ib/c	2952	5	21	79
2.85 M_⊙ + NS	2.85	1.25	1.45	1.85	0.94	1.56	0.29	1.00e-3	Ib/c	61	20	35	65
2.80 M_⊙ + BH	2.80	1.98	1.45	2.05	3.87	1.56	0.48	9.66e-3	Ib/c	763	9	27	73
2.80 M_⊙ + NS	2.80	0.53	1.45	1.79	0.41	1.56	0.23	1.00e-3	Ib/c	6	44	48	52
2.75 M_⊙ + BH	2.75	0.74	1.45	1.88	1.69	1.56	0.31	2.68e-3	Ib/c	74	21	41	59
2.75 M_⊙ + NS	2.75	0.19	1.45	1.71	0.15	1.54	0.16	4.96e-4	Ultra-stripped	0.37	64	64	36

Notes. Initial properties of post-CE binary: M_1, i – initial mass of the RSG remnant, P_orb, i – initial orbital period, $M_{core, i}^{CO}$ $M_{\mathrm{core,i}}^{\mathrm{CO}}$ – initial CO core mass of the RSG remnant. Final properties prior to core collapse: M_1, f – final mass of the RSG remnant, P_orb, f – final orbital period, $M_{core, f}^{CO}$ $M_{\mathrm{core,f}}^{\mathrm{CO}}$ – final CO core mass of the RSG remnant, $M_{He, f}^{env}$ $M_{\mathrm{He,f}}^{\mathrm{env}}$ – final mass of the He-rich envelope, ΔM_{NS or BH} – the total amount mass accreted by the compact companion, SNe type – the SNe type when the star explodes, τ_grw – GW merger timescale of final double compact objects without NS kicks, f_merger – GW-induced merger fraction of final double compact objects within a Hubble time considering NS kicks, f_bound – fraction of bound binary systems after NS kicks, f_disrupt – fraction of disrupted binary systems after NS kicks.

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