2004A&A...413..693M

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 Query : 2004A&A...413..693M

2004A&A...413..693M - Astronomy and Astrophysics, volume 413, 693-709 (2004/1-2)

Bright OB stars in the Galaxy. I. Mass-loss and wind-momentum rates of O-type stars: A pure Hα analysis accounting for line-blanketing.

MARKOVA N., PULS J., REPOLUST T. and MARKOV H.

Abstract (from CDS):

We study mass-loss and wind momentum rates of 29 Galactic O-type stars with luminosity classes I, III and V by means of a pure Hα profile analysis and investigate to what extent the results compare to those originating from a state-of-the-art, complete spectral analysis. Our investigation relies on the approximate method developed by Puls et al. (1996A&A...305..171P) which we have modified to account for the effects of line-blanketing. Effective temperatures and gravities needed to obtain quantitative results from such a simplified approach have been derived by means of calibrations based on most recent spectroscopic NLTE analyses and models of Galactic stars by Repolust, Puls and Herrero (RPH) (2003A&A accepted) and Martins et al. (2002A&A...382..999M). Comparing (I) the derived wind-densities to those determined by RPH for eleven stars in common and (II) the Wind-momentum Luminosity Relationship (WLR) for our sample stars to those derived by other investigations, we conclude that our approximate approach is actually able to provide consistent results. Additionally, we studied the consequences of fine tuning'' some of the direct and indirect parameters entering the WLR, especially by accounting for different possible values of stellar reddening and distances. Combining our data set with the corresponding data provided by Herrero et al. (2002A&A...396..949H) and RPH we finally study the WLR for the largest sample of Galactic O-type stars gathered so far, including an elaborate error treatment. The established disagreement between the theoretical predictions and the observed'' WLRs being a function of luminosity class is suggested to be a result of wind clumping. Different strategies to check this hypothesis are discussed, particularly by comparing the Hα mass-loss rates with the ones derived from radio observations.

Journal keyword(s): stars: early-type - stars: mass-loss - stars: winds, outflows - stars: distances - stars: fundamental parameters

Full paper

 Number of rows : 47
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2022
#notes
1 HD 225160 s*b 00 04 03.7944653736 +62 13 19.009200864 7.74 8.46 8.19     O8Iabf 115 0
2 NGC 869 OpC 02 18 58 +57 08.0           ~ 456 0
3 Ass Per OB 1 As* 02 21 +57.6           ~ 166 1
4 NGC 884 OpC 02 22 20 +57 08.9           ~ 467 0
5 HD 14947 s*b 02 26 46.9899705528 +58 52 33.118732380 7.83 8.44 7.98     O4.5If 245 0
6 HD 16429 SB* 02 40 44.9492589168 +61 16 55.995618720 7.91 8.29 7.67     O9.5III+F4V 159 1
7 HD 16691 Em* 02 42 52.0259349000 +56 54 16.463813796 10.187 9.07 8.70     O4If 148 0
8 Ass Cas OB 6 As* 02 43 +61.3           ~ 121 0
9 HD 17603 * 02 51 47.7980420280 +57 02 54.469902552 8.68 9.10 8.45     O7.5Ib(f) 87 0
10 BD+56 739 * 02 54 50.7852330744 +57 26 35.810085264 12.537 10.66 9.87     O9.5Ib 26 0
11 HD 18409 * 03 00 29.7126315336 +62 43 19.052057856 9.832 8.72 8.40     O9.7Ib 72 0
12 Ass Cam OB 1 As* 03 31.6 +58 38           ~ 90 0
13 Ass Per OB 2 As* 03 42.2 +33 26           ~ 322 0
14 HD 24431 ** 03 55 38.4221692944 +52 38 28.747965948 6.50 7.11 6.74 6.36 6.10 O9III+B1.5V 156 0
15 * ksi Per ** 03 58 57.9022917 +35 47 27.713205 3.190 4.080 4.060 3.88 3.89 O7.5III(n)((f)) 815 0
16 NGC 1502 OpC 04 07 49 +62 19.9   7.47 6.9     ~ 175 1
17 * alf Cam s*b 04 54 03.0103983 +66 20 33.636467 3.47 4.34 4.29 4.18 4.18 O9Ia 647 1
18 HD 34656 Em* 05 20 43.0812017952 +37 26 19.195066068 5.87 6.77 6.76     O7.5II(f) 196 0
19 Ass Aur OB 1 As* 05 22 +33.9           ~ 77 0
20 Ass Aur OB 2 As* 05 28 +34.9           ~ 44 0
21 * lam Ori A Em* 05 35 08.2760807112 +09 56 02.991326316 2.17 3.48 3.47     O8III((f)) 496 0
22 * iot Ori SB* 05 35 25.9819073 -05 54 35.643537 1.45 2.53 2.77     O9IIIvar 752 0
23 NAME Ori I As* 05 38 -02.8           ~ 585 0
24 HD 42088 * 06 09 39.5728368936 +20 29 15.450599580 6.73 7.58 7.57 8.45   O6V((f))z 237 0
25 Ass Gem OB 1 As* 06 09.8 +21 35           ~ 179 0
26 NAME Mon I MoC 06 35 +10.1           ~ 231 0
27 HD 47432 Pu* 06 38 38.1872868432 +01 36 48.675208608 5.67 6.44 6.31 6.11 6.04 O9.7Ib 175 1
28 * 15 Mon Be* 06 40 58.65963 +09 53 44.7229 3.360 4.45 4.68   4.88 O7V+B1.5/2V 777 0
29 NAME CMa OB1 As* 07 07.0 -10 28           ~ 134 0
30 HD 54662 SB* 07 09 20.2493151288 -10 20 47.635088964 5.35 6.24 6.21 7.23   O6.5Vz(n)+O7.5Vz 333 2
31 NAME GUM Nebula ISM 07 43 -42.1           ~ 406 1
32 * zet Pup BY* 08 03 35.04754 -40 00 11.3321 0.89 1.98 2.25 2.36 2.58 O4I(n)fp 1127 1
33 NAME NC 48 Em* 19 45 40.6390187808 +25 07 36.038833608 10.76 10.71 9.55     O8e 63 0
34 HD 188209 s*b 19 51 59.0687638680 +47 01 38.419078944 4.61 5.55 5.63 5.54 5.64 O9.5Iab 299 0
35 HD 190429A s*b 20 03 29.395 +36 01 30.53   7.20 7.09     O4If 83 0
36 Ass Cyg OB 3 As* 20 07 +35.9           ~ 177 0
37 HD 192639 s*b 20 14 30.4275801672 +37 21 13.816276704 6.83 7.46 7.11     O7.5Iabf 279 0
38 Ass Cyg OB 1 As* 20 17.8 +37 38           ~ 259 1
39 HD 193514 Em* 20 19 08.4971150880 +39 16 24.253036608 7.32 7.83 7.38     O7Ib(f) 182 0
40 HD 202124 s*b 21 12 28.3896178416 +44 31 54.129118980 7.33 7.94 7.76     O9Iab 92 0
41 HD 207198 * 21 44 53.2791389640 +62 27 38.048647248 5.61 6.25 5.94 5.66 5.49 O8.5II 332 0
42 Ass Cep OB 2 As* 21 51 +60.0           ~ 283 0
43 * 19 Cep * 22 05 08.7897533088 +62 16 47.332569936 4.36 5.19 5.11 4.95 4.92 O9Ib 369 0
44 * lam Cep s*b 22 11 30.5765111040 +59 24 52.154264880 4.55 5.29 5.05 4.77 4.62 O6.5I(n)fp 666 1
45 HD 210809 s*b 22 11 38.6004719208 +52 25 47.950615308 6.7 7.61 7.56     O9Iab 203 0
46 Ass Cep OB 1 As* 22 29 +56.6           ~ 83 0
47 HD 218915 s*b 23 11 06.9483955128 +53 03 29.652921252 6.32 7.22 7.20     O9.2Iab 189 1

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2022.08.09-04:00:19