2000A&A...354..193H


Query : 2000A&A...354..193H

2000A&A...354..193H - Astronomy and Astrophysics, volume 354, 193-215 (2000/2-1)

Fundamental parameters of Galactic luminous OB stars. IV. The upper HR diagram.

HERRERO A., PULS J. and VILLAMARIZ M.R.

Abstract (from CDS):

We present observations and analyses of seven Galactic O stars of type O6 and earlier. The analyses are carried out using NLTE plane-parallel, hydrostatic models as well as NLTE spherical models with mass-loss. With detailed calculations for the former and simulations for the latter, it is shown that the flux blocking due to UV metal lines is important for these objects, in agreement with previous studies, and the way the mechanism operates is explained. We find that the plane-parallel, hydrostatic unblanketed model atmospheres have increasing difficulties in fitting the early-type spectra of massive stars, and for 50000K and above a fit seems to be impossible. The gravities derived are relatively low even for the luminosity class V stars. These objects also show the mass discrepancy found in earlier studies, indicating that sphericity and mass-loss are important, even at their higher gravities. We then perform an analysis using spherical models with mass-loss. It is found that gravities should be increased by 0.1-0.25 dex, reducing, but not solving, the mass discrepancy. We show that spectroscopic masses are in better agreement with the theory of radiatively driven winds than evolutionary masses are. A helium abundance larger than solar is also obtained for most objects. Some additional effects (partly related to present approximations) that have an influence in our analyses are studied. It is found that HeIIλ4200 is less sensitive to details of the model calculations than HeIIλ4541 and thus it is preferred for temperature determinations, with the consequence of lower effective temperatures. It is shown that the fits to HeIIλ4686 are improved when the upward rates of the Heiiresonance lines are reduced (with respect to the conventional treatment adequate for lines formed in expanding atmospheres), either by setting them in detailed balance or by artificially adding extra opacity sources that simulate line blocking. The Heiiblend with Hαis also affected. Some stars of our sample have such high mass-loss rates that the derivation of gravities from the wings of Balmer lines, in particular Hγ, becomes doubtful. For the most extreme objects, the mass-loss rates needed to fit Hα are different from those needed to fit Hγ, by a maximum factor of two. From the point of view of individual stars, we have analysed some of the most massive and luminous stars in the Milky Way. According to our analysis, three of them (Cyg OB2 #7, HD 15570 and HD15558) have particularly large initial masses, close to or in excess of 100 M. Finally, the least luminous object in our sample, HD 5689, could have been erroneously assigned to Cas OB7 and might be a runaway star.

Abstract Copyright:

Journal keyword(s): stars: atmospheres - stars: early-type - stars: evolution - stars: fundamental parameters - stars: mass-loss

Simbad objects: 20

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Number of rows : 20
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 Ass Cas OB 7 As* 00 50 14 +64 04.3           ~ 61 0
2 HD 5689 * 00 59 47.5908405456 +63 36 28.250542152 8.79 9.41 9.19     O7Vn((f)) 43 0
3 Ass Per OB 1 As* 02 21 +57.6           ~ 166 1
4 HD 14947 s*b 02 26 46.9899705528 +58 52 33.118732380 7.83 8.44 7.98     O4.5If 245 0
5 HD 15558 Y*O 02 32 42.5366901168 +61 27 21.572901360 7.82 8.37 7.87 7.34 6.94 O4.5III(f) 308 0
6 HD 15570 Em* 02 32 49.4207394600 +61 22 42.089384892 8.40 8.80 8.11 7.41 6.86 O4If 295 0
7 HD 15629 Y*O 02 33 20.5873992264 +61 31 18.188762844 8.23 8.85 8.42     O4.5V((fc)) 230 0
8 Ass Cas OB 6 As* 02 43 +61.3           ~ 121 0
9 * ksi Per ** 03 58 57.9022917 +35 47 27.713205 3.190 4.080 4.060 3.88 3.89 O7.5III(n)((f)) 813 0
10 Brey 77 WR* 05 38 42.1044150840 -69 05 55.335965424     12.86   12.79 O2If* 74 0
11 RMC 136a Cl* 05 38 43.3 -69 06 08           ~ 143 2
12 * zet Pup BY* 08 03 35.04754 -40 00 11.3321 0.89 1.98 2.25 2.36 2.58 O4I(n)fp 1125 1
13 HD 93129 ** 10 43 57.462360 -59 32 51.27000 6.26 7.840 7.884 7.839   O2If*+O3.5V((f)) 195 1
14 HD 93250 * 10 44 45.0275085072 -59 33 54.680974848 6.73 8.12 7.50 8.38   O4III(fc) 302 0
15 HD 188209 s*b 19 51 59.0687638680 +47 01 38.419078944 4.61 5.55 5.63 5.54 5.64 O9.5Iab 297 0
16 HD 226868 HXB 19 58 21.6757355952 +35 12 05.784512688 9.38 9.72 8.91 8.42   O9.7Iabpvar 4092 0
17 Ass Cyg OB 2 As* 20 33.2 +41 19           ~ 871 0
18 Schulte 7 * 20 33 14.1095938872 +41 20 21.904113804 12.24 12.00 10.55     O3If* 137 0
19 Ass Cep OB 2 As* 21 51 +60.0           ~ 282 0
20 * 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

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2022.05.29-07:21:05

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