Properties of WNh stars in the Small Magellanic Cloud: evidence for homogeneous evolution

F. Martins; D. J. Hillier; J. C. Bouret; E. Depagne; C. Foellmi; S. Marchenko; A. F. Moffat

doi:10.1051/0004-6361:200811014

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Volume 495 / No 1 (February III 2009)

A&A, 495 1 (2009) 257-270

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Table 2:

Parameters of our best fit models. Uncertainties are: 3 kK (7 kK for SMC-WR1) on temperatures, 0.1 dex on luminosities (0.15 for SMC-WR1), 0.2 dex on $\dot{M}$ , 100 km s^-1 on $v_{\infty }$ , 0.05 on He/H, 30 to 50 $\%$ on abundances.
Star	ST	T_*	T_ eff $T_{{\rm eff}}$	LL_ $\log \frac{L}{L_{\odot}}$	R_*	$\log \dot{M}$	$f_{\infty }$	$\beta$	$v_{\infty }$	He/H	X	X(C)	X(N)	X(O)
		[kK]	[kK]		$R_{\odot}$	[ $M_{\odot }$ yr^-1]			[km s^-1]	#	(%)	(%)	(%)	(%)
SMC-WR1	WN3h	65.4	60.5	5.75	5.8	-5.55	0.10^a	1.0	1800	0.25	0.50	<0.004	0.12	<0.04
SMC-WR2	WN5h	44.8	42.5	5.50	9.3	-5.85	0.10^a	1.0	1000	0.15	0.62	0.005	0.35	-
SMC-WR4	WN6h	43.1	42.0	5.90	16.0	-5.00	0.15^b	1.0	1000	0.45	0.35	0.003	0.40	<0.15

^a Adopted.
^b Derived from $\chi^{2}$ fit, mass loss rate scaled from model closest to minimum ( $f_{\infty}=0.1$ ).

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