Stellar-wind feedback and magnetic fields around young compact star clusters: 3D magnetohydrodynamics simulations

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Table B.1

Parameters of the stars in our model cluster. Shown are stellar mass, M; effective temperature, T_eff; radius, R; main-sequence lifetime, t_MS; mass-loss rate, $\dot{M}$ $\[\dot{M}\]$ ; terminal wind velocity, u_∞; and wind power, $L_{w} = 0.5 \dot{M} u_{\infty}^{2}$ $\[L_{\mathrm{w}}=0.5 \dot{M} u_{\infty}^{2}\]$ .

Nr.	M	T_eff	R	t_MS	$\dot{M}$ $\[\dot{M}\]$	u_∞	L_w
	M_⊙	K	R_⊙	kyr	10⁻⁶ M_⊙ yr⁻¹	km/s	10³⁶ erg s⁻¹
1^a,b	40.2	45,519	11.4	4591	0.74	2632	1.61
2	40.7	45,708	11.5	4548	0.77	2635	1.69
3	41.2	45,899	11.6	4506	0.81	2637	1.77
4	41.7	46,094	11.7	4463	0.85	2640	1.86
5^b	42.3	46,291	11.8	4421	0.89	2643	1.95
6	42.8	46,491	12.0	4379	0.93	2647	2.05
7	43.4	46,694	12.1	4337	0.97	2650	2.15
8	44.0	46,901	12.2	4295	1.02	2653	2.26
9	44.6	47,111	12.3	4254	1.07	2656	2.38
10^b	45.2	47,324	12.5	4212	1.12	2659	2.50
11^a	45.9	47,541	12.6	4170	1.17	2663	2.62
12	46.5	47,761	12.8	4129	1.23	2666	2.76
13	47.2	47,984	12.9	4088	1.29	2670	2.90
14^b	47.9	48,212	13.1	4047	1.36	2673	3.06
15	48.6	48,443	13.2	4006	1.43	2677	3.22
16	49.4	48,679	13.4	3965	1.50	2681	3.39
17	50.2	48,919	13.6	3924	1.57	2685	3.57
18	51.0	49,163	13.7	3883	1.65	2688	3.76
19^b	51.8	49,411	13.9	3843	1.74	2692	3.96
20	52.7	49,664	14.1	3803	1.83	2696	4.18
21^a	53.6	49,921	14.3	3762	1.92	2701	4.41
22	54.6	50,184	14.5	3722	2.02	2705	4.65
23	55.6	50,451	14.8	3682	2.12	2709	4.91
24^b	56.6	50,724	15.0	3642	2.23	2714	5.18
25	57.7	51,003	15.2	3602	2.35	2718	5.47
26	58.8	51,286	15.5	3563	2.48	2723	5.78
27	60.0	51,576	15.7	3523	2.61	2728	6.11
28^b	61.2	51,872	16.0	3484	2.74	2733	6.46
29	62.5	52,174	16.3	3445	2.89	2738	6.82
30	63.8	52,482	16.6	3406	3.04	2743	7.21
31^a	65.3	52,798	17.0	3367	3.20	2749	7.63
32^b	66.8	53,120	17.3	3328	3.37	2754	8.06
33	68.3	53,450	17.7	3289	3.55	2760	8.53
34	70.0	53,787	18.1	3250	3.74	2766	9.02
35	71.7	54,133	18.5	3212	3.94	2772	9.54
36	73.6	54,487	18.9	3174	4.15	2779	10.08
37	75.6	54,849	19.4	3135	4.36	2785	10.66
38	77.7	55,220	19.9	3097	4.59	2792	11.27
39^b	79.9	55,601	20.4	3059	4.82	2799	11.91
40	82.3	55,992	21.0	3022	5.07	2807	12.58
41^a,b	84.8	56,393	21.6	2984	5.32	2814	13.28
42	87.5	56,805	22.3	2947	5.58	2822	14.00
43	90.4	57,227	23.0	2909	5.85	2831	14.76
44	93.6	57,662	23.8	2872	6.12	2839	15.54
45	97.0	58,109	24.7	2835	6.39	2849	16.33
46	100.7	58,568	25.7	2798	6.66	2858	17.14

Notes. Stars with superscript a are magnetic stars. Their dipole field strength is B_s = 1 kG in runs with standard magnetic field (clusters I–III in Table 1) and 100 G in low B case. In the high B case, the number of magnetic stars is doubled, but individual stars still have B_s = 1 kG (superscript b). In the simulation, the main-sequence phase is shortened. The most massive star (Nr. 46) enters the WR phase at 200 kyr, followed by stars Nr. 45–42, enter with a time delay according to their difference in lifetime to star Nr. 46.

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