Stellar winds on the main-sequence - II. The evolution of rotation and winds

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Table 2

Statistical properties of our composite cluster at different ages.

Stellar mass ( M_⊙)	(Ω_⊙)	σ_Ω (Ω_⊙)	Ω₁₀ (Ω_⊙)	Ω₅₀ (Ω_⊙)	Ω₉₀ (Ω_⊙)	Ṁ₁₀ (Ṁ_⊙)	Ṁ₅₀ (Ṁ_⊙)	Ṁ₉₀ (Ṁ_⊙)

100 Myr

All	27.43	44.62	3.24	8.49	78.79	–	–	–
0.5	32.39	35.09	3.88	18.05	85.25	11.84	11.84	11.84
0.6	29.04	35.28	3.12	11.13	88.65	8.49	14.36	14.36
0.7	27.22	42.93	3.02	6.52	82.76	6.26	17.42	17.72
0.8	25.44	52.11	3.07	5.20	69.82	5.08	10.21	21.13
0.9	22.65	54.66	3.23	5.64	53.11	4.50	9.48	25.20
1.0	23.71	51.17	3.76	7.15	60.10	4.45	10.46	28.02

250 Myr

All	16.43	28.08	2.67	5.19	50.29	–	–	–
0.5	23.00	26.70	2.73	12.11	62.18	10.29	11.88	11.88
0.6	19.07	24.65	2.51	6.35	60.91	6.37	14.38	14.38
0.7	15.62	27.11	2.56	3.89	45.81	5.02	8.78	17.76
0.8	13.56	32.32	2.62	3.77	34.54	4.11	6.67	21.18
0.9	11.07	30.92	2.82	4.24	16.39	3.78	6.52	25.30
1.0	10.74	23.39	3.25	5.03	14.74	3.74	6.69	27.94

500 Myr

All	7.56	12.68	2.11	3.28	19.24	–	–	–
0.5	12.47	15.90	1.96	5.77	33.83	6.63	11.94	11.94
0.6	9.11	12.26	1.96	3.04	28.13	4.58	8.21	14.41
0.7	6.05	11.03	2.08	2.69	13.93	3.84	5.39	17.82
0.8	5.23	12.41	2.19	2.82	6.82	3.25	4.57	14.75
0.9	4.47	9.67	2.37	3.16	4.77	3.02	4.43	7.66
1.0	4.12	2.88	2.69	3.64	4.98	3.00	4.49	6.81

750 Myr

All	4.10	5.82	1.74	2.52	7.43	–	–	–
0.5	6.60	8.87	1.57	2.84	17.12	4.99	10.96	12.00
0.6	4.48	5.45	1.61	2.16	11.89	3.55	5.22	14.43
0.7	3.00	3.73	1.79	2.17	4.34	3.15	4.07	10.22
0.8	2.84	3.56	1.91	2.37	3.55	2.73	3.62	6.21
0.9	2.82	2.00	2.08	2.62	3.34	2.55	3.48	4.80
1.0	2.98	0.61	2.36	2.93	3.57	2.59	3.45	4.50

1000 Myr

All	2.66	2.82	1.48	2.08	3.49	–	–	–
0.5	3.60	4.74	1.32	1.89	8.33	3.96	6.41	12.06
0.6	2.57	2.19	1.41	1.78	4.70	2.97	4.05	14.46
0.7	2.11	0.99	1.58	1.88	2.82	2.67	3.36	5.77
0.8	2.16	0.81	1.71	2.06	2.67	2.36	3.01	4.28
0.9	2.29	0.45	1.88	2.27	2.71	2.25	2.88	3.66
1.0	2.51	0.37	2.10	2.50	2.93	2.28	2.86	3.55

1500 Myr

All	1.66	0.72	1.16	1.60	2.08	–	–	–
0.5	1.56	1.21	1.00	1.27	2.22	2.75	3.79	7.98
0.6	1.48	0.36	1.15	1.38	1.96	2.28	2.90	4.63
0.7	1.56	0.26	1.31	1.53	1.91	2.09	2.57	3.45
0.8	1.68	0.24	1.43	1.67	1.95	1.87	2.30	2.83
0.9	1.82	0.22	1.59	1.83	2.07	1.82	2.20	2.58
1.0	1.98	0.20	1.76	1.98	2.22	1.88	2.19	2.56

2000 Myr

All	1.33	0.30	0.96	1.34	1.67	–	–	–
0.5	1.09	0.32	0.82	1.04	1.41	2.15	2.93	4.39
0.6	1.19	0.18	0.98	1.16	1.45	1.85	2.32	3.10
0.7	1.32	0.17	1.13	1.31	1.53	1.73	2.10	2.60
0.8	1.43	0.16	1.25	1.44	1.61	1.58	1.90	2.21
0.9	1.56	0.15	1.39	1.57	1.72	1.54	1.81	2.04
1.0	1.67	0.13	1.54	1.67	1.82	1.62	1.81	2.03

Notes. The cluster is composed of ~1500 stars with known rotation periods and masses from Pleiades, M 50, M 35, and NGC 2516, all of which have ages ~150 Myr. We have evolved the cluster backwards to 100 Myr and forwards to 2 Gyr using our rotational evolution model. The distributions of rotation rates at ages of 100 Myr, 500 Myr, 1 Gyr, and 2 Gyr for this cluster are shown in Fig. 7. In this table, we give, from left to right, the average angular velocity, , the standard deviation in the angular velocity, σ_Ω, the 10th, 50th, and 90th percentiles in the angular velocity distributions, and our predicted wind mass loss rates at these percentiles. For each age, we give the values for all of the stars between 0.4 M_⊙ and 1.1 M_⊙, and for masses of 0.5 M_⊙, 0.6 M_⊙, 0.7 M_⊙, 0.8 M_⊙, 0.9 M_⊙, and 1.0 M_⊙. At each specific mass, we calculate the values of each parameter using all stars within 0.1 M_⊙ of the given mass.

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