On the consistent treatment of the quasi-hydrostatic layers in hot star atmospheres

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Table 4

Deduced stellar masses with different quasi-hydrostatic approaches.

Luminosity class	I	III	V

log g_eff [cm s^-2]^a	2.47	3.02	3.79
log g_grav(Γ_e) [cm s^-2]^b	3.00	3.25	3.82
log g_grav(Γ_rad) [cm s^-2]	3.25	3.50	4.00
M_∗(Γ_e) [M_⊙]^b	14.5	12.9	16.2
M_∗(Γ_rad) [M_⊙]	25.9	23.0	24.1

Notes.

^(a)

The effective gravity (cf. Sect. 2.4) is fixed for all models here.

^(b)

These values are derived from models that were calculated as if only the Thomson radiative pressure would enter the hydrostatic equation.

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