On the presence and absence of disks around O-type stars

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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).

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