The Eddington factor as the key to understand the winds of the most massive stars - Evidence for a Γ-dependence of Wolf-Rayet type mass loss

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Volume 535 (November 2011)

A&A, 535 (2011) A56

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Table A.1

Mass–luminosity relations for chemically-homogeneous stars.

No.	Ev. ph.	Eq.	Mass range	F₁	F₂	F₃	F₄	F₅	F₆	F₇	F₈	F₉

1	H-b.	9	12–250 M_⊙	2.875	−3.966	2.496	2.652	−0.310	−0.511
2	H-b.	9	2–100 M_⊙	1.967	−2.943	3.755	1.206	−0.727	−0.026
3	H-b.	9	60–4000 M_⊙	3.862	−2.486	1.527	1.247	−0.076	−0.183
4	H-b.	B.7	2–30 M_⊙	−2.688	−7.843	2.471	2.758	−0.233	−0.747
5	H-b.	B.7	12–4000 M_⊙	−2.416	−5.118	1.869	−0.400	0.064	0.050
6	He-b.	10	8–250 M_⊙	3.017	2.446	−0.306
7	He-b.	10	0.6–100 M_⊙	2.635	2.986	−0.488
8	He-b.	10	60–1000 M_⊙	3.826	1.619	−0.099
9	He-b.	B.8	0.3–100 M_⊙	−2.204	1.831	0.149
10	He-b.	B.8	12–500 M_⊙	−1.676	1.075	0.404

11	H-b.	11, 12	12–250 M_⊙	4.026	4.277	−1.0	25.48	36.93	−2.792	−3.226	−5.317	1.648
12	H-b.	11, 12	2–100 M_⊙	2.582	0.829	−1.0	9.375	0.333	0.543	−1.376	−0.049	0.036
13	H-b.	11, 12	60–4000 M_⊙	10.05	8.204	−1.0	151.7	254.5	−11.46	−13.16	−31.68	2.408
14	H-b.	B.13, B.14	2–30 M_⊙	5.303	5.918	−1.0	16.58	−4.292	−72.89	−7.881	−13.76	3.206
15	H-b.	B.13, B.14	12–4000 M_⊙	−14.60	3.125	1.0	251.0	15.63	72.24	18.20	12.21	0.781
16	He-b.	13	8–250 M_⊙	3.997	−1.0	25.83	−3.268
17	He-b.	13	0.6–100 M_⊙	3.059	−1.0	14.76	−2.049
18	He-b.	13	60–1000 M_⊙	8.177	−1.0	105.5	−10.10
19	He-b.	B.15	0.3–100 M_⊙	−6.144	1.0	52.54	6.711
20	He-b.	B.15	12–500 M_⊙	−1.330	1.0	5.919	2.475

Notes. The table describes the mass–luminosity relations L(M,X_H), and M(L,X_H) that are derived in this work, as well as the relations Γ_e(M,X_H), and M(Γ_e,X_H) in the appendix. For each relation we give the assumed evolutionary phase, the corresponding equation numbers, the relevant mass range, and the numeric coefficients F_n.

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