The i-processes nucleosynthesis during the formation of He-rich hot-subdwarf stars

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Table 1.

Properties of the evolutionary sequences computed in this work.

Name	z_ini	y_ini	PIE?	M_⋆/M_⊙	$log {(\frac{M_{H}}{M_{⊙}})}_{L_{He} = 1}$ $\log\left(\frac{M_{\mathrm{H}}}{M_{\odot}}\right)_{L_{\mathrm{He}} = 1}$	$log {(\frac{L_{CNO}}{L_{⊙}})}_{L_{He} = 1}$ $\log\left(\frac{L_{\mathrm{CNO}}}{L_{\odot}}\right)_{L_{\mathrm{He}} = 1}$	$Δ S_{\max of L_{He}}^{[N_{A} k_{B} / μ]}$ $\Delta S_{\mathrm{max~of}\,L_{\mathrm{He}}}^{[N_{\!\rm A}k_{\mathrm{B}}/\mu]}$	t_split − t_PIE	N_n,max [cm⁻³]	τ_n, max [mb⁻¹]
01-1	0.01	0.265	Yes	0.4667	−3.4728	−1.442	1.31	∼26 d	1.2 × 10¹⁰	1.9 × 10⁻⁴
01-2	0.01	0.265	Yes	0.4720	−3.4887	−0.849	1.63	∼110 d	4.6 × 10⁹	1.5 × 10⁻⁴
01-3	0.01	0.265	Yes	0.4745	−3.4158	3.016	2.24	∼193 yr	4.2 × 10⁹	9.9 × 10⁻⁴
01-4	0.01	0.265	Yes	0.4747	−3.3760	3.103	2.32	∼620 yr	7.4 × 10⁸	8.9 × 10⁻⁴
01-5	0.01	0.265	No	0.4748	−3.3128	3.191	2.55	–	–	–
01-6	0.01	0.265	No	0.4749	−3.2951	3.211	2.75	–	–	–
01-7	0.01	0.265	No	0.4751	−3.1960	3.287	4.14	–	–	–

001-1	0.001	0.246	Yes	0.4821	−3.2958	−0.443	0.91	∼28 d	1.6 × 10¹²	7.4 × 10⁻³
001-2	0.001	0.246	Yes	0.4835	−3.2956	1.511	1.09	∼172 d	4.9 × 10¹¹	6.1 × 10⁻³
001-3	0.001	0.246	Yes	0.4836	−3.2772	2.674	1.16	∼1 yr	8.0 × 10¹¹	9.8 × 10⁻³
001-4	0.001	0.246	Yes	0.4838	−3.2593	2.794	1.21	∼400 yr	3.0 × 10¹³	2.21
001-5	0.001	0.246	Yes	0.4839	−3.2220	2.919	1.46	∼670 yr	1.7 × 10¹²	5.12
001-6	0.001	0.246	No	0.4840	−3.1903	2.986	1.97	–	–	–
001-7	0.001	0.246	No	0.4843	−3.1215	3.081	2.44	–	–	–

0001-1	0.0001	0.2451	Yes	0.4900	−3.1305	−0.790	1.03	∼0.9 d, 17 d	1.2 × 10¹⁵	2.98
0001-2	0.0001	0.2451	Yes	0.4912	−3.1338	−0.682	1.02	∼1.6 d	5.5 × 10¹⁴	3.57
0001-3	0.0001	0.2451	Yes	0.4926	−3.1345	−0.481	1.23	∼1.6 d	1.0 × 10¹⁵	3.74
0001-4	0.0001	0.2451	Yes	0.4939	−3.1411	−0.227	1.46	∼2.7 d	8.2 × 10¹⁴	2.40
0001-5	0.0001	0.2451	Yes	0.4946	−3.1421	0.083	1.48	∼4.6 d	8.6 × 10¹⁴	1.61
0001-6	0.0001	0.2451	Yes	0.4948	−3.1422	0.271	1.53	∼6 d	7.7 × 10¹⁴	1.59
0001-7	0.0001	0.2451	Yes	0.4951	−3.1306	0.702	1.60	∼9 d	6.4 × 10¹⁴	1.76
0001-8	0.0001	0.2451	Yes	0.4953	−3.1395	2.402	1.73	∼17 d	4.9 × 10¹⁴	2.09
0001-9	0.0001	0.2451	Yes	0.4956	−3.1159	2.630	2.05	∼117 d	2.2 × 10¹⁴	2.86
0001-10	0.0001	0.2451	Yes	0.4957	−3.1027	2.682	2.57	∼264 yr	1.6 × 10¹³	8.41
0001-11	0.0001	0.2451	No	0.4958	−3.0862	3.25	2.744	–	–	–
0001-12	0.0001	0.2451	No	0.4965	−2.9714	3.62	2.974	–	–	–

Notes. In order the columns are: name of the evolutionary sequence, initial metallicity, initial He content, if they experience or not a PIE, remnant mass, hydrogen mass, and CNO burning luminosity at the moment when the He-burning luminosity reaches the value log(L_He/L_⊙) = 1, specific entropy barrier at the peak of the He flash, time span between the onset of the PIE and the splitting of the convective zone, maximum neutron density and maximum neutron exposure reached during the evolution.

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