Formation of black holes from He stars | Astronomy & Astrophysics (A&A)

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Table 1.

Dependence of pre-SN properties on physical parameters.

$M_{He}^{i}$ $Mathematical equation: $ M_{\mathrm{He}}^{\mathrm{i}} $$	Z	f_ov	M_CO	X_C	M_C-free	ξ_2.5	μ₄	M₄	s_c	M_Fe	M_f	log( − E_bind)	E_exp	Fate	M_rm, grav
[M_⊙]			[M_⊙]		[M_⊙]				[N_Ak_B]	[M_⊙]	[M_⊙]	[erg]	[10⁵¹erg]		[M_⊙]
15.0	0.0088	0.01	9.25	0.247	1.92	0.145	0.05	1.67	0.87	1.56	11.5	51.49	0.24	NS	1.46
15.0	0.02	0.01	7.51	0.254	3.28	0.571	0.16	2.32	1.14	1.85	8.79	51.70	⋯	BH	8.79
15.0	0.03	0.01	6.45	0.259	2.07	0.163	0.07	1.77	0.92	1.54	7.82	51.58	0.56	NS	1.54
15.0	0.04	0.01	5.81	0.262	2.16	0.189	0.08	1.82	0.95	1.60	7.14	51.56	0.77	NS	1.58

15.0	0.02	0.0	7.70	0.253	3.35	0.597	0.17	2.37	1.13	1.89	8.96	51.72	⋯	BH	8.96
15.0	0.02	0.016	7.43	0.255	3.07	0.535	0.15	2.29	1.12	1.85	8.70	51.67	⋯	BH	8.70
15.0	0.02	0.027	7.34	0.256	2.67	0.444	0.13	2.14	1.08	1.79	8.57	51.61	⋯	BH	8.57

Notes. Same as Table A.1, but for the representative model $M_{He}^{i} = 15 M_{⊙}$ $Mathematical equation: $ M_{\mathrm{He}}^{\mathrm{i}}=15 \, M_{\odot} $$ , with variations in the physical parameters. We used different metallicities, Z = 0.0088, 0.02, 0.03, 0.04, and explored a range of convective overshooting parameters, f_ov = 0.0, 0.01, 0.016, 0.027. The case with Z = 0.02 and f_ov = 0.01 serves as the fiducial model.

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