Table 1: Adopted stellar parameters for the binary system WR 21a.
Variable WR OB Unit

Spectral Class. WN6^a O3 (I)f^b

log ( $L/{L}_\odot$ ) 5.2^c 6.274^d

$T_{\rm eff}$ 45 000^c 50680^d K

M_* 12^c 65^d $M_\odot$

$\mu$ 4^c 1.5^c

$v_\infty$ 2000^c 3150^c km s^-1

$\dot{M}$ expected $3.0 \times 10^{-5{c}}$ $1.4 \times 10^{-5{c}}$ $M_\odot$ yr^-1

distance d 3^c 3^c kpc

^a van der Hucht (2001); ^b Reig (1999); ^c see text.

^d Vacca et al. (1996).

**Table 1:** Adopted stellar parameters for the binary system WR 21a.
Variable	WR	OB	Unit
Spectral Class.	WN6^a	O3 (I)f^b
log ( $L/{L}_\odot$ )	5.2^c	6.274^d
$T_{\rm eff}$	45 000^c	50680^d	K
M_*	12^c	65^d	$M_\odot$
$\mu$	4^c	1.5^c
$v_\infty$	2000^c	3150^c	km s^-1
$\dot{M}$ expected	$3.0 \times 10^{-5{c}}$	$1.4 \times 10^{-5{c}}$	$M_\odot$ yr^-1
distance d	3^c	3^c	kpc

Source LaTeX | All tables | In the text

	1 Introduction
	2 WR 21a and its surroundings
	3 Observations and data reduction
	4 Results
	5 Analysis of the line features
	6 The X-ray history of WR 21a
	7 Connection with the EGRET source?
	8 Summary and conclusions
	References

^a van der Hucht (2001); ^b Reig (1999); ^c see text.
^d Vacca et al. (1996).