Using population synthesis of massive stars to study the interstellar medium near OB associations

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Table 2:

Classification criteria for WR stars, and their wind velocities.
WR type	Surface abundances	Wind velocity ( `wind08`)	Wind velocity ( `wind00`)
WNL	$0.4>{\rm H}_{\rm s}>0.1$	1250	1900
WNE	H $_{\rm s}<0.1 \& {\rm C}_{\rm s}/{\rm N}_{\rm s}<10$	2000	1650
WC6-9	H $_{\rm s}<0.1 \& {\rm C}_{\rm s}/{\rm N}_{\rm s}>10 \& ({\rm C}_{\rm s}+{\rm O}_{\rm s})/{\rm He}_{\rm s}<0.5$	1760	1810
WC4-5	H $_{\rm s}<0.1 \& {\rm C}_{\rm s}/{\rm N}_{\rm s}>10 \& ({\rm C}_{\rm s}+{\rm O}_{\rm s})/{\rm He}_{\rm s}<1.0$	2650	2820
WO	H $_{\rm s}<0.1 \& {\rm C}_{\rm s}/{\rm N}_{\rm s}>10 \& ({\rm C}_{\rm s}+{\rm O}_{\rm s})/{\rm He}_{\rm s}>1.0$	3000	3000

$^{\ast}$ H $_{\rm s}, {\rm C}_{\rm s}, {\rm N}_{\rm s}$ and He $_{\rm s}$ are the fractional surface abundances (mass fraction) of hydrogen, carbon,
nitrogen and helium, respectively, and the wind velocities are in km s^-1.

Source LaTeX | All tables | In the text

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