2012A&A...541A.145C


C.D.S. - SIMBAD4 rel 1.7 - 2019.11.12CET23:31:25

2012A&A...541A.145C - Astronomy and Astrophysics, volume 541A, 145-145 (2012/5-1)

On the nature of the galactic early-B hypergiants.

CLARK J.S., NAJARRO F., NEGUERUELA I., RITCHIE B.W., URBANEJA M.A. and HOWARTH I.D.

Abstract (from CDS):

Despite their importance to a number of astrophysical fields, the lifecycles of very massive stars are still poorly defined. In order to address this shortcoming, we present a detailed quantitative study of the physical properties of four early-B hypergiants (BHGs) of spectral type B1-4 Ia+; Cyg OB2 #12, ζ1 Sco, HD 190603 and BP Cru. These are combined with an analysis of their long-term spectroscopic and photometric behaviour in order to determine their evolutionary status. Quantitative analysis of UV-radio photometric and spectroscopic datasets was undertaken with a non-LTE model atmosphere code in order to derive physical parameters for comparison with apparently closely related objects, such as B supergiants (BSGs) and luminous blue variables (LBVs), and theoretical evolutionary predictions. The long-term photospheric and spectroscopic datasets compiled for the early-B HGs revealed that they are remarkably stable over long periods (≥40yrs), with the possible exception of ζ1 Sco prior to the 20th century; in contrast to the typical excursions that characterise LBVs. Quantitative analysis of ζ1 Sco, HD 190603 and BP Cru yielded physical properties intermediate between BSGs and LBVs; we therefore suggest that BHGs are the immediate descendants and progenitors (respectively) of such stars, for initial masses in the range ∼30-60M. Comparison of the properties of ζ1 Sco with the stellar population of its host cluster/association NGC 6231/Sco OB1 provides further support for such an evolutionary scenario. In contrast, while the wind properties of Cyg OB2 #12 are consistent with this hypothesis, the combination of extreme luminosity and spectroscopic mass (∼110M) and comparatively low temperature means it cannot be accommodated in such a scheme. Likewise, despite its co-location with several LBVs above the Humphreys-Davidson (HD) limit, the lack of long term variability and its unevolved chemistry apparently excludes such an identification. Since such massive stars are not expected to evolve to such cool temperatures, instead traversing an O4-6Ia->O4-6Ia+->WN7-9ha pathway, the properties of Cyg OB2 #12 are therefore difficult to understand under current evolutionary paradigms. Finally, we note that as with AG Car in its cool phase, despite exceeding the HD limit, the properties of Cyg OB2 #12 imply that it lies below the Eddington limit - thus we conclude that the HD limit does not define a region of the HR diagram inherently inimical to the presence of massive stars.

Abstract Copyright:

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

Simbad objects: 58

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Number of rows : 58

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 M 31 G 00 42 44.330 +41 16 07.50 4.86 4.36 3.44     ~ 10577 1
2 [HS80] 110A s*b 01 33 41.220 +30 22 37.15 15.181 16.236 16.285 16.279 16.321 B1Ia 22 0
3 M 33 GiG 01 33 50.904 +30 39 35.79 6.17 6.27 5.72     ~ 5025 1
4 [HS80] B324 s*y 01 33 55.93 +30 45 30.4 14.941 15.287 14.859 14.545 14.398 A8-F0Ia 30 1
5 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 14340 1
6 * J Pup * 07 53 18.1579197 -48 06 10.563676 3.11 4.10 4.24 4.26 4.38 B0.5Ib 216 0
7 NAME HD 80077 Group OpC 09 15 53.0 -50 01 00           ~ 21 1
8 HD 80077 s*b 09 15 54.7869106351 -49 58 24.573847509 10.50 10.29 9.00 7.89   B2Ia+e 122 0
9 HD 92207 sg* 10 37 27.0681943657 -58 44 00.015326487 5.71 5.95 5.45     A0Ia 145 0
10 V* AG Car WR* 10 56 11.5779283438 -60 27 12.809532379 7.00 7.57 6.96 7.73   WN11h 580 0
11 V* BP Cru HXB 12 26 37.5607088371 -62 46 13.259605389   12.70 10.66     B1.5Iaeq 596 0
12 * ksi Sco SB* 16 04 22.134576 -11 22 23.17404     4.36     F7V 122 0
13 HD 152048 * 16 46 54.1483743071 +63 23 09.636467828   9.20 7.61     K5 7 0
14 WR 77f WR* 16 47 02.96 -45 50 19.7   21.552 17.792 15.035 12.508 WN10-11h 22 0
15 Cl* Westerlund 1 W 42 * 16 47 03.25 -45 50 52.2         10.764 B9Ia+ 15 0
16 Hen 3-1250 Em* 16 47 03.6265799796 -45 50 14.357624931   20.0 15.972     B5Ia+ 21 0
17 Cl Westerlund 1 OpC 16 47 04.00 -45 51 04.9           ~ 442 0
18 Cl* Westerlund 1 W 33 * 16 47 04.1266525740 -45 50 48.475675980   20.090 15.61 12.803   B5Ia+ 19 0
19 Cl* Westerlund 1 W 13 EB* 16 47 06.4536718776 -45 50 26.067083031   21.1 17.19 14.63 12.06 BIa+ 25 0
20 Cl* Westerlund 1 W 243 s*b 16 47 07.5028508821 -45 52 29.152464693   19.873 15.730     LBV 48 0
21 HD 151515 SB* 16 49 48.2513677482 -42 00 06.175258125 6.77 7.48 7.30 7.11 6.88 O7II(f) 113 0
22 HD 151804 s*b 16 51 33.7215112148 -41 13 49.928887100 4.45 5.29 5.22     O8Iaf 348 0
23 NAME Sco OB 1 As* 16 53.5 -41 57           ~ 187 0
24 HD 152219 Al* 16 53 55.6076307131 -41 52 51.497348038 6.950 7.705 7.552   7.267 O9.5III(n) 87 0
25 * zet01 Sco s*b 16 53 59.7270104119 -42 21 43.313745214 4.80 5.31 4.79 4.32 3.86 B1Ia-0ek 344 0
26 HD 152234 s*b 16 54 01.8374467 -41 48 23.007764 4.92 5.64 5.45     B0.5Ia 176 0
27 HD 152233 SB* 16 54 03.5915443398 -41 47 29.834880322 5.93 6.72 6.59     O6II(f) 172 0
28 NGC 6231 OpC 16 54 08.51 -41 49 36.0   2.83 2.6     ~ 474 0
29 HD 152134 * 16 54 08.6613066848 -50 39 14.445944882   10.25 10.01     A2V 3 0
30 HD 152248 bL* 16 54 10.0614779606 -41 49 30.143138696 5.56 6.15 6.05     O7Iabf+O7Ib(f) 224 0
31 HD 152247 SB* 16 54 11.5170221125 -41 38 30.969538639 6.62 7.35 7.16 8.09   O9.2III 111 0
32 HD 152249 s*b 16 54 11.6391931444 -41 50 57.294733186 5.91 6.65 6.45     OC9Iab 211 0
33 HD 152270 WR* 16 54 19.6991728950 -41 49 11.535393651 6.26 6.80 6.59 6.72 6.39 WC7+O5-8 280 0
34 HD 326331 ** 16 54 25.9691443777 -41 49 55.770189619 6.886 7.678 7.497   7.143 O8IVn((f)) 63 0
35 HD 152408 s*b 16 54 58.50567 -41 09 03.0964 5.17 5.92 5.77 7.00   O8Iape 344 0
36 HD 152723 * 16 56 54.6718019380 -40 30 44.457237721 6.43 7.24 7.10 8.11 8.47 O6.5III(f) 139 0
37 HD 160529 sg* 17 41 59.0257256544 -33 30 13.702939546 8.17 7.87 6.66 5.50 4.51 A2Ia 182 1
38 NAME Gal Center reg 17 45 40.04 -29 00 28.1           ~ 11035 0
39 NAME Quintuplet Cluster OpC 17 46 13.9 -28 49 48           ~ 425 0
40 [WDL2006] 216 s*b 17 46 15.15 -28 49 32.4           O6-8Ife 16 0
41 LHO 100 * 17 46 15.15 -28 49 31.4           O6-8Ife 4 0
42 [FMM95] 3 Em* 17 46 15.240 -28 50 03.58           ~ 134 1
43 GMM 14 Em* 17 46 15.48 -28 49 20.1           ~ 8 0
44 [GMC99] D6 * 17 46 17.982 -28 49 03.46           ~ 52 0
45 HD 316285 s*b 17 48 14.0369781568 -28 00 53.124817157 11.88 11.27 9.60 9.28   B0Ieq 177 2
46 * del Sgr * 18 20 59.6435424 -29 49 41.165919   4.069 2.668     K2.5IIIaCN0.5 160 0
47 HD 168607 s*b 18 21 14.8855350307 -16 22 31.760520819 10.23 9.82 8.28 8.55   B9Iaep 171 1
48 HD 168625 s*b 18 21 19.5486475779 -16 22 26.077308888 10.15 9.78 8.37 8.76   B6Iap 246 2
49 HD 169454 s*b 18 25 15.1938696996 -13 58 42.305035144 7.39 7.61 6.71 5.82 5.13 B1Ia 305 0
50 BD-13 5061 sg* 18 39 26.1023386431 -13 50 47.162584517 10.86 10.75 9.89 9.98   B9Ia 30 1
51 IRAS 18576+0341 s*b 19 00 10.89456 +03 45 47.1096           B8I 80 1
52 HD 183143 s*b 19 27 26.5636908636 +18 17 45.191198361 8.25 8.08 6.86 5.74 4.79 B6Ia 404 0
53 HD 190603 s*b 20 04 36.1744053423 +32 13 06.952102252 5.73 6.19 5.65 5.13 4.71 B1.5Ia 322 0
54 * P Cyg s*b 20 17 47.2020844 +38 01 58.552724 4.66 5.24 4.82 4.28 4.02 B1-2Ia-0ep 1126 1
55 Schulte 12 s*b 20 32 40.9574572449 +41 14 29.276333992 16.1 14.45 11.702     B3-4Ia+ 352 0
56 * alf Cyg sg* 20 41 25.91514 +45 16 49.2197 1.11 1.34 1.25 1.14 1.04 A2Ia 712 0
57 HD 199478 s*b 20 55 49.8044819063 +47 25 03.561837777 5.79 6.12 5.64 5.16 4.78 B8Ia 211 0
58 * 6 Cas sg* 23 48 50.17052 +62 12 52.2577 6.08 6.10 5.43     A3Ia+ 178 0

    Equat.    Gal    SGal    Ecl

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2019.11.12-23:31:25

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