Table 4: Derived stellar parameters (December 2004).

  star		 spectrum H$\alpha^1$ V B-V $A_{\rm V}$ T (K) B.C.2 $M_{\rm bol}$ 3  log  $L/L_{\odot}$ phase4
GR290 Oe (WN11) -120  17.18 -0.09 0.68 30 000  -3.2 -11.5  6.5  min
Var A F-G -35  18.60 +0.88 (0.7) 6 500  -0.3  -7.25 4.8 min
Var B Be -310  17.50 -0.15 0.37   -2.0 -9.7 5.8  min
Var C B[e] -49  16.40 +0.10 0.6   -1.0  -10.0  5.9  post max
1 Equivalent width of the H$\alpha $ emission line in Å.  2 Adopted bolometric correction. See A. N. Cox, Allen's Astrophysical Quantities (2000).   3 Assuming for M 33 m-M = 24.8 (Kim et al. 2002).   4 Photometric phase.   5 Value referred to the optical spectral component (Fig. 4). The star should be subject to a $\sim$3$^{\rm m}$ obscuration in the visual due to the presence of a dusty envelope that is responsible for the strong mid-infared emission found by Humphreys et al. (1987).


Source LaTeX | All tables | In the text