Coupling hydrodynamics with comoving frame radiative transfer - III. The Wind Regime of Early-Type B Hypergiants

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Volume 697 (May 2025)

A&A, 697 (2025) A41

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Table 1

Stellar properties of ζ¹ Sco deduced from our final PoWRHD model.

Property	This work	Cr06	Cl12
$T_{*}^{τ \max} (kK)$	21.550	–	19.8100
$T_{eff}^{τ = 2 / 3} (kK)$	17.7	18.0	17.2
log L/L⊙	5.96	6.10	5.93
log gτ max (cgs)	2.3550	–	2.20100
log gτ=2/3 (cgs)	2.02	2.20	1.97
v sin i (km s–1)	45	74	45
vmac (km s–1)	50	–	50
M (M⊙)	39	72	36
$R_{*}^{τ max} (R_{⊙})$	6950	–	77100
Rτ=2/3 (R⊙)	100	112	103
Γe	0.51	0.35	0.47
vturb (km s–1)	14	15	15
ξmax (km s–1)	180	50	90
XH	0.60	0.55	0.55
X He	0.38	0.43	0.43
XC × 103	2.1	0.1	1.0
XN × 103	6.0	1.7	6.0
XO × 103	4.9	1.8	3.0
v∞ (km s–1)	300	390	390
$\log \overset{\cdot}{M} (M_{⊙} {yr}^{- 1}]$	–5.27	–5.22	–5.79

Notes. For comparison, we also show the results from Crowther et al. (2006, Cr06) and Clark et al. (2012, Cl12). The subscripts on $T_{*}^{τ}^{m a x}$ $T{_*^\tau ^{max}}$ , log g^{τ max} and $R_{*}^{τ}^{m a x}$ $R{_*^\tau ^{max}}$ refer to the maximum Rosseland mean optical depth τ_max of each study.

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