2019A&A...627A.151S


C.D.S. - SIMBAD4 rel 1.7 - 2020.10.29CET21:58:34

2019A&A...627A.151S - Astronomy and Astrophysics, volume 627A, 151-151 (2019/7-2)

The Wolf-Rayet binaries of the nitrogen sequence in the Large Magellanic Cloud. Spectroscopy, orbital analysis, formation, and evolution.

SHENAR T., SABLOWSKI D.P., HAINICH R., TODT H., MOFFAT A.F.J., OSKINOVA L.M., RAMACHANDRAN V., SANA H., SANDER A.A.C., SCHNURR O., ST-LOUIS N., VANBEVEREN D., GOTBERG Y. and HAMANN W.-R.

Abstract (from CDS):

Context. Massive Wolf-Rayet (WR) stars dominate the radiative and mechanical energy budget of galaxies and probe a critical phase in the evolution of massive stars prior to core collapse. It is not known whether core He-burning WR stars (classical WR; cWR) form predominantly through wind stripping (w-WR) or binary stripping (b-WR). Whereas spectroscopy of WR binaries has so-far largely been avoided because of its complexity, our study focuses on the 44 WR binaries and binary candidates of the Large Magellanic Cloud (LMC; metallicity Z~=0.5Z), which were identified on the basis of radial velocity variations, composite spectra, or high X-ray luminosities. Aims. Relying on a diverse spectroscopic database, we aim to derive the physical and orbital parameters of our targets, confronting evolution models of evolved massive stars at subsolar metallicity and constraining the impact of binary interaction in forming these stars. Methods. Spectroscopy was performed using the Potsdam Wolf-Rayet (PoWR) code and cross-correlation techniques. Disentanglement was performed using the code Spectangular or the shift-and-add algorithm. Evolutionary status was interpreted using the Binary Population and Spectral Synthesis (BPASS) code, exploring binary interaction and chemically homogeneous evolution. Results. Among our sample, 28/44 objects show composite spectra and are analyzed as such. An additional five targets show periodically moving WR primaries but no detected companions (SB1); two (BAT99 99 and 112) are potential WR + compact-object candidates owing to their high X-ray luminosities. We cannot confirm the binary nature of the remaining 11 candidates. About two-thirds of the WN components in binaries are identified as cWR, and one-third as hydrogen-burning WR stars. We establish metallicity-dependent mass-loss recipes, which broadly agree with those recently derived for single WN stars, and in which so-called WN3/O3 stars are clear outliers. We estimate that 45±30% of the cWR stars in our sample have interacted with a companion via mass transfer. However, only ~=12±7% of the cWR stars in our sample naively appear to have formed purely owing to stripping via a companion (12% b-WR). Assuming that apparently single WR stars truly formed as single stars, this comprises ~=4% of the whole LMC WN population, which is about ten times less than expected. No obvious differences in the properties of single and binary WN stars, whose luminosities extend down to log L~=5.2[L], are apparent. With the exception of a few systems (BAT99 19, 49, and 103), the equatorial rotational velocities of the OB-type companions are moderate (veq≤250km/s) and challenge standard formalisms of angular-momentum accretion. For most objects, chemically homogeneous evolution can be rejected for the secondary, but not for the WR progenitor. Conclusions. No obvious dichotomy in the locations of apparently single and binary WN stars on the Hertzsprung-Russell diagram is apparent. According to commonly used stellar evolution models (BPASS, Geneva), most apparently single WN stars could not have formed as single stars, implying that they were stripped by an undetected companion. Otherwise, it must follow that pre-WR mass-loss/mixing (e.g., during the red supergiant phase) are strongly underestimated in standard stellar evolution models.

Abstract Copyright: © ESO 2019

Journal keyword(s): stars: massive - stars: Wolf-Rayet - Magellanic Clouds - binaries: close - binaries: spectroscopic - stars: evolution

Errata: erratum vol. 641, art. C2 (2020)

Simbad objects: 77

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Number of rows : 77

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     ~ 11057 1
2 NAME SMC G 00 52 38.0 -72 48 01   2.79 2.2     ~ 9564 1
3 HD 5980 WR* 00 59 26.5847969465 -72 09 53.927725716   11.13 11.31   11.029 WN4+O7I: 363 1
4 HD 9974 WR* 01 38 55.6271504593 +58 09 22.671823428 9.85 10.71 10.69     WN3h-w 158 0
5 NAME Magellanic Clouds GrG 03 00 -71.0           ~ 5766 1
6 Brey 3 WR* 04 52 57.3973799275 -66 41 13.495098750 13.793 14.531 14.640   14.527 WN4b 35 0
7 SK -67 18 WR* 04 55 14.9238992344 -67 11 23.749108611 10.990 11.803 11.95   12.072 O6-7n-nn+WN5-6-A 55 0
8 HD 32109 WR* 04 55 31.3419672483 -67 30 02.683822100 12.893 13.46 13.81 13.95 13.512 WN4b 70 0
9 Brey 10a WR* 04 57 27.4549113851 -67 39 02.868479987 12.213 13.314 13.496   13.564 O2If*/WN5 53 1
10 HD 268856 WR* 04 58 56.3627926026 -68 48 04.730973756   12.130 10.827 10.34 9.33 WN4o(+OB) 37 0
11 HD 268847 WR* 04 59 51.5599828055 -67 56 55.440010992 13.658 14.21 14.58 14.75 14.426 WN4b 50 0
12 HD 269015 WR* 05 04 12.3242039777 -70 03 55.403600765 13.183 14.07 14.28 14.40 14.108 WN4o 43 0
13 HD 34169 WR* 05 09 40.4192565947 -68 53 24.755119043 12.773 13.47 13.65 14.02 13.697 WN4b+O5: 60 1
14 HD 34632 WR* 05 13 43.7715301497 -67 22 29.381793393 12.144 13.002 13.07 13.41 13.271 WN4+OB 28 0
15 Brey 19a WR* 05 14 57.2839962735 -71 36 18.314627217   14.87 15.10 15.49   WN4ha 18 0
16 HD 269333 WR* 05 18 19.2101847037 -69 11 40.655834630 10.375 11.23 11.29 11.47 11.412 WN+BI 56 0
17 Brey 23 WR* 05 20 44.7284628858 -65 28 20.444855910 13.774 14.43 14.65 14.87 14.534 WN4b+OB 36 0
18 Brey 25 WR* 05 22 04.4095841528 -67 59 06.779107874 14.589 15.326 15.207   14.993 WN4b 35 0
19 HD 36063 WR* 05 22 22.5297442838 -71 35 58.151974584 11.583 12.43 12.66 12.85 12.602 WN7 65 0
20 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 14998 1
21 HD 269485 WR* 05 24 24.1937327527 -68 31 35.596373567 13.593 14.40 14.46 14.39 14.574 WN4b/WCE+OB 54 0
22 Brey 33 WR* 05 26 36.8640 -68 50 59.640   14.591 14.77     WN4(h)a 28 0
23 HD 269546 WR* 05 26 45.3199315750 -68 49 52.786974246 9.00 9.83 9.86 9.76 9.76 WN5b(h)+B3I 102 0
24 Brey 37 WR* 05 27 37.6899657541 -70 36 05.320790978 12.875 13.85 14.07 14.43 14.249 WN4o+OB 37 0
25 HD 269618 WR* 05 29 12.3652285107 -68 45 36.154397830 14.391 15.104 15.295 15.32 15.222 WN3b 28 0
26 HD 269624 WR* 05 29 31.6378583206 -68 54 28.817861004 14.008 14.491 14.781 14.81 14.703 WN4b 42 1
27 Brey 40a WR* 05 29 33.2066825323 -70 59 34.838593733 12.472 13.20 13.39 13.90 13.743 WN4:b+O8V 39 0
28 HD 269748 WR* 05 33 10.5705967402 -67 42 43.055762502 12.093 13.054 13.186   12.828 WN4b+O8: 47 0
29 Brey 49 WR* 05 33 10.8687893344 -69 29 01.006247724 13.435 14.227 14.42   14.512 WN4(h)a 21 0
30 Brey 51 WR* 05 34 37.4804697354 -66 14 37.991946375 14.196 15.041 15.312   15.273 WN3(h) 20 0
31 HD 269784 WR* 05 34 59.385 -69 44 06.33 13.347 14.081 14.073   14.321 WN4o+O9: 26 0
32 IRSF J05352853-6940090 WR* 05 35 28.5224484120 -69 40 08.931861384           WN3+O8-9III 4 0
33 Brey 56 WR* 05 35 42.1983672394 -69 12 34.588531247 12.969 13.708 13.587   13.325 WN5ha 33 1
34 Brey 60 WR* 05 35 44.279 -68 59 36.79 14.527 15.068 14.782 14.87 14.473 WN4+O8: 23 0
35 Brey 61 WR* 05 35 45.0257300827 -68 58 44.534221076 14.632 15.532 15.376   15.533 WN4h+O3: 22 0
36 BAT99 77 WR* 05 35 58.889 -69 11 47.88           WN7 67 0
37 HD 269828 EB* 05 35 58.91 -69 11 47.3     13.031   12.837 WN7+O3 72 0
38 BAT99 78 WR* 05 35 59.085 -69 11 51.12   13.07 12.94     WN6(+O8V) 21 0
39 Brey 57 WR* 05 35 59.8169082147 -69 11 22.218225371 13.143 13.784 13.486   12.060 WN7ha+OB 31 0
40 BAT99 80 WR* 05 35 59.913 -69 11 50.70     13.0     O4If+OB 19 0
41 Brey 66 WR* 05 36 33.58 -69 09 17.3 15.636 15.937 16.108   15.627 WN3b 28 0
42 IRSF J05374762-6921136 WR* 05 37 47.6086857476 -69 21 13.574145564           WN3+O7.5V 4 0
43 HD 269891 WR* 05 37 49.0345689657 -69 05 08.219994930 11.791 9.447 11.39 11.55   WN6+B1Ia 65 0
44 Brey 74a WR* 05 37 51.3383720439 -69 09 46.692195685 12.483 13.474 13.446 13.62 13.278 O3If* 30 0
45 RMC 135 WR* 05 38 33.62 -69 04 50.4   12.63 13.48     WN7h+OB 55 0
46 NAME 30 Dor Nebula SFR 05 38 36.0 -69 05 11           ~ 1050 2
47 Brey 78 WR* 05 38 40.2960 -69 05 59.640           O2.5If*/WN6 36 0
48 Brey 75 WR* 05 38 40.53 -69 05 57.2   12.84 12.75   12.34 WN6h 58 0
49 RMC 140b WR* 05 38 41.5650 -69 05 15.500   12.61 12.66   12.54 WN6 26 0
50 RMC 140a WR* 05 38 41.600 -69 05 13.39   12.18 12.12   12.40 WN4+WC5 31 0
51 RMC 140 WR* 05 38 41.62 -69 05 14.0   11.213 11.616     WN7+WC4/5pec 76 0
52 NGC 2070 Cl* 05 38 42 -69 06.0     7.25     ~ 329 1
53 Brey 77 WR* 05 38 42.13 -69 05 55.3   11.08 10.96     O2If* 72 0
54 RMC 139 WR* 05 38 42.3548071421 -69 04 58.201053806   12.04 11.94     O6.5Iafc+O6Iaf 86 0
55 RMC 136 Cl* 05 38 42.396 -69 06 03.36           ~ 1751 1
56 BAT99 108 WR* 05 38 42.43 -69 06 02.2   12.78 12.77     WN5h 60 0
57 BAT99 111 WR* 05 38 42.765 -69 06 03.36   13.51 13.66     WN9ha 37 0
58 BAT99 112 WR* 05 38 42.9162 -69 06 04.938   12.95 12.86     WN5h 48 0
59 BAT99 113 WR* 05 38 43.12 -69 05 46.8   13.56 13.47   13.44 O2If*/WN5 37 0
60 BAT99 114 WR* 05 38 43.20 -69 06 14.6   13.52 13.40   13.31 O2If*/WN5 32 0
61 Brey 84 HXB 05 38 44.2507887068 -69 06 06.008788720     13.10   12.70 WN5h:a 52 0
62 HD 38282 WR* 05 38 53.3788120199 -69 02 00.896643506   10.98 11.11 11.26   WN5/6h+WN6/7h 151 1
63 HD 269928 WR* 05 38 57.0668705166 -69 06 05.660972436   12.02 11.94 12.00 11.58 WN6/7 121 0
64 HD 269956 WR* 05 40 07.5364893415 -69 24 31.929655191 12.043 13.014 13.166 13.51 13.205 WN4b+O8: 41 0
65 Brey 97 WR* 05 41 48.5698169547 -70 35 30.786068009 13.570 14.522 14.701 14.50 14.834 MN3ha+O5V 23 1
66 HD 45166 WR* 06 26 19.1550467867 +07 58 28.071465236 9.05 9.81 9.88     WRpec+B8V 71 1
67 HD 50896 WR* 06 54 13.0440847499 -23 55 42.020318514 5.74 6.63 6.91 7.74   WN4b 743 0
68 Mrk 30 G 10 19 38.280 +57 25 06.82   17.0       ~ 18 0
69 V* V712 Car bL* 10 23 58.0120989646 -57 45 48.938103165 15.466 15.473 13.5 12.6   O3If*/WN6+O3If*/WN6 148 1
70 Mrk 34 Sy2 10 34 08.606 +60 01 52.33   15.71 14.65     ~ 215 1
71 HD 93131 WR* 10 43 52.2575981063 -60 07 04.016913264 5.52 6.43 6.48 7.46   WN6ha-w 278 0
72 NGC 3353 AGN 10 45 22.390 +55 57 37.36 12.90 13.25 12.79     ~ 324 1
73 Mrk 39 GiP 11 18 20.753 +53 45 09.77   17.0       ~ 24 0
74 Mrk 42 Sy1 11 53 41.7727871132 +46 12 42.171866526   16.24 15.45     ~ 194 0
75 HD 177230 WR* 19 03 59.0232385542 -04 19 01.911120922 11.32 11.60 11.12     WN8 162 0
76 HD 193576 WR* 20 19 32.4230196684 +38 43 53.958209968 8.15 8.53 8.00     WN5+O6II-V 686 0
77 V* V1521 Cyg HXB 20 32 25.78 +40 57 27.9           WN4/5-6/7 1778 2

    Equat.    Gal    SGal    Ecl

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2020.10.29-21:58:34

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