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Home All issues Volume 505 / No 2 (October II 2009) A&A, 505 2 (2009) 743-753 Full HTML
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Table 2:

Stellar parameters for the four groups of peculiar O-type stars.
Name $\log (L/\mbox{$L_{\odot}$ })$ $\mbox{$T_{\rm eff}$ }$ $\log g$ M R $\mbox{$v_{\infty}$ }$ log $\mbox{$\dot{M}$ }$ $\rho_{\rm wind}$ $v\sin i$
    (kK)   $(\mbox{$M_{\odot}$ })$ $(\mbox{$R_{\odot}$ })$ (km/s) ( $\mbox{$M_{\odot} {\rm yr}^{-1}$ }$) (10-13 $M_{\odot} {\rm yr}^{-1}$/km s-1 ${\mbox{$R_{\odot}$ }^2}$) (km/s)
Group I   OVz and weak wind dwarfs
$\Theta ^1$ Ori C 5.13 39 4.1 30 8 580 -5.7 530 24
$\Theta^2$ Ori A 4.62 30.5 3.92 17 7 25001 -7.59 1.9  
HD 42088 5.23 38 4.0 32 10 1900 -6.19 37 60
HD 54662 5.2 36.8 3.92 29 10 2456 -6.40 17 73
HD 152590 5.00 34.4 3.92 24 9 1785 -6.64 23 60
HD 93128 5.66 46.5 4.00 40 10 32101 -5.53 100 100
HD 93129B 5.86 44.0 3.92 52 13 32101 -5.25 110  
CPD-58$^{\rm o}$2611 5.3 38.2 3.92 32 10 28701 -6.23 21  
CPD-58$^{\rm o}$2620 5.2 36.8 3.92 29 24 17601 -6.43 15 110
Group II   Of?p
HD 148937 5.75 41.0 4.0 $\sim$55 15 2285 -5.45 71 76
HD 108 5.40 37.0 3.75 $\sim$35 12 1960 -5.97 37 78
HD 191612 5.4 35 3.5 $\sim$35 15 24501 -6.14 17  
Group III   Oe stars
HD 39680 5.5 40   45 11 1675 -5.69 90 218
HD 45314 4.72 31.5 3.92 18 8 24101 -7.37 3.0 285
HD 46485 5.1 35.5 3.92 27 9 1800 -6.44 25  
HD 60848 4.9 33.4 3.92 22 8.5 1765 -6.84 12 240
HD 120678 4.9 33.4 3.92 22 8.5 25801 -7.02 5.5  
Zeta Oph 4.88 32.1 3.62 20 9 1505 -6.83 12 372
HD 155806 4.9 33.4 3.92 22 8.5 2460 -7.02 5.5 91
Group IV   Onfp
HD 152248A 5.69 33.3 3.4 41 21.1 2420 -6.10 16 159
HD 210839 5.83 36.0 3.55 62 21.1 2250 -5.47 33 200
Zeta Pup 5.90 39.0 3.60 54 19.4 2250 -5.24 68 219
Cyg OB2 No. 5 5.69 33.3 3.4 41 21.1 22401 -5.64 27  
The stellar parameters are taken from the following papers: Repolust et al. (2004), Martins et al. (2005b), and Puls et al. (2006). For all stars without recent line-blanketed models, the calibrations of Martins et al. (2005a) are used. The mass-loss rates are from Monte Carlo radiation-driven wind models (Vink et al. 2000). The wind density is given as $\rho_{\rm wind}=\mbox{$\dot{M}$ }/(R^2 \mbox{$v_{\infty}$ })$. Where spectral subtypes are not provided, we interpolate. $v\sin i$ are mostly taken from Howarth et al. (1997).
1 Note that the terminal velocity is calculated by multiplication of the escape velocity by the canonical factor of 2.6 (Lamers et al. 1995).

Source LaTeX | All tables | In the text

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