Effect of gravity darkening and oblate factor in rapidly rotating massive stars

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Table 2

Properties of fast and Ω-slow solutions for B-type stellar models (GD effect).

Model	Ω range	Solution	Co-existence interval	Ṁ(Ω_i)	υ_∞(Ω_i)	r_crit(Ω_i)	Ṁ(Ω_f)	υ_∞(Ω_f)	r_crit(Ω_f)
		type	Ω_i – Ω_f	(M_⊙ yr⁻¹)	(km s⁻¹)	(R_⊙)	(M_⊙ yr⁻¹)	(km s⁻¹)	(R_⊙)
B2.5 V	0.68–0.942	Fast	0.936–0.942	4.35 × 10⁻⁹	433.4	21.82	4.65 × 10⁻⁹	943.7	1.027
	0.946–0.995	Ω-slow
B0 IV	0.68–0.936	Fast	0.932–0.936	4.716 × 10⁻⁷	383.5	15.64	4.908 × 10⁻⁷	746.5	1.058
	0.932–0.995	Ω-slow
B3 I	0.69–0.886	Fast	0.870–0.886	2.552 × 10⁻⁶	280.9	12.51	2.872 × 10⁻⁶	519.1	1.049
	0.87–0.995	Ω-slow

Notes. The wind parameters are evaluated at the angular velocity values, Ω, corresponding to the beginning (i) and end (ƒ) of the co-existence region. Columns 5–7 correspond to the Ω-slow solution, while the last three columns refer to the fast solution.

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