To clump or not to clump - The impact of wind inhomogeneities on the optical and NIR spectroscopic analysis of massive OB stars

Open Access

Table 8

Stellar and wind parameters for the coarse grid models.

	V			III			I

	T_eff	log g	log Q	T_eff	log g	log β	T_eff	log g	log Q
HOT	42	4.0	−14.	42	3.8	−13.	42	3.6	−11.9
MID	36	4.0	−14.	36	3.7	−13.	36	3.4	−11.9
COOL	30	4.0	−14.	30	3.4	−13.	30	3.0	−11.9

Notes. For each luminosity class, we display T_eff (in kK), log g, and the unclumped log Q values. For all models, a helium abundance of Y_He= 0.1 and a velocity exponent β = 0.8 has been adopted.

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