New empirical mass-loss recipe for UV radiation line-driven winds of hot stars across various metallicities

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Table 1

Metallicity dependence of the stellar winds of hot stars.

m	Method	Reference
OB

0.94	Modified CAK	Abbott (1982)
0.5	Modified CAK	Kudritzki et al. (1987)
0.8	Modified CAK	Puls et al. (2000)
0.85	Monte Carlo calc.	Vink et al. (2001)
0.83	Empiric $\dot{M}$ $\[\dot{M}\]$ (Hα only)	Mokiem et al. (2007)
0.5–0.8^(†)	Empiric $\dot{M}$ $\[\dot{M}\]$ (UV+opt.)	Marcolino et al. (2022)
0.66–1.64 ^(††)	Hydrodynamic stellar Atmosphere models	Björklund et al. (2023)

WN

0.86	Monte Carlo calc.	Vink & de Koter (2005)
1.2 ± 0.1	Empiric $\dot{M}$ $\[\dot{M}\]$	Hainich et al. (2017)
0.83 ± 0.09	Empiric $\dot{M}$ $\[\dot{M}\]$	Shenar et al. (2019, 2020)
1.3 ± 0.2	Empiric $\dot{M}$ $\[\dot{M}\]$	Tramper et al. (2016)

WC/WO

0.66	Monte Carlo calc.	Vink & de Koter (2005)
0.25 ± 0.08	Empiric $\dot{M}$ $\[\dot{M}\]$	Tramper et al. (2016)

OB+WR

0.86	Empiric $\dot{M}$ $\[\dot{M}\]$	This work

Notes. ^(†) The authors report that the metallicity dependence is a function of luminosity. The quoted exponents refer to stars with luminosities above log(L/L_⊙) ≳ 5.4 (i.e. valid for most of our stars). ^(††) The authors predict that the metallicity dependence is a function of temperature. We calculated the metallicity exponents for the provided validity regime of their relation.

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