Table 2: Best fit model parameters for the polar (p), intermediate (i), and disk wind (d). The mass fluxes are assumed to be constant within the indicated $\theta$ -ranges and have an error on the order of 20%.
T₀ $T_{\infty }$ $\theta_{\rm min}$ $\theta_{\rm max}$ $v_\infty$ $F_{\rm m}(\theta)$

[K] [K] [ $\hbox{$^\circ$ }$ ] [ $\hbox{$^\circ$ }$ ] [km s^-1] [g s^-1 cm^-2]

p 50 000 10 000 0 45 85 $7.2\times 10^{-2}$

i 50 000 10 000 45 78 45 $1.5\times 10^{-1}$

d 10 000 6000 78 90 35 $5.5\times 10^{-1}$

**Table 2:** Best fit model parameters for the polar (p), intermediate (i), and disk wind (d). The mass fluxes are assumed to be constant within the indicated $\theta$ -ranges and have an error on the order of 20%.
	T₀	$T_{\infty }$	$\theta_{\rm min}$	$\theta_{\rm max}$	$v_\infty$	$F_{\rm m}(\theta)$
	[K]	[K]	[ $\hbox{$^\circ$ }$ ]	[ $\hbox{$^\circ$ }$ ]	[km s^-1]	[g s^-1 cm^-2]
p	50 000	10 000	0	45	85	$7.2\times 10^{-2}$
i	50 000	10 000	45	78	45	$1.5\times 10^{-1}$
d	10 000	6000	78	90	35	$5.5\times 10^{-1}$

Source LaTeX | All tables | In the text

	1 Introduction
	2 Observations and reductions
	3 The spectral atlas
	4 The nature of the circumstellar material: nebula or wind?
	5 Modeling of the non-spherical wind
	6 Discussion
	7 Conclusions
	References
	Online Material