2013A&A...559A..16L


C.D.S. - SIMBAD4 rel 1.7 - 2019.12.10CET15:23:36

2013A&A...559A..16L - Astronomy and Astrophysics, volume 559A, 16-16 (2013/11-1)

Modelling the asymmetric wind of the luminous blue variable binary MWC 314.

LOBEL A., GROH J.H., MARTAYAN C., FREMAT Y., TORRES DOZINEL K., RASKIN G., VAN WINCKEL H., PRINS S., PESSEMIER W., WAELKENS C., HENSBERGE H., DUMORTIER L., JORISSEN A., VAN ECK S. and LEHMANN H.

Abstract (from CDS):

We present a spectroscopic analysis of MWC 314, a luminous blue variable (LBV) candidate with an extended bipolar nebula. The detailed spectroscopic variability is investigated to determine if MWC 314 is a massive binary system with a supersonically accelerating wind or a low-mass B[e] star. We compare the spectrum and spectral energy distribution to other LBVs (such as P Cyg) and find very similar physical wind properties, indicating strong kinship. We combined long-term high-resolution optical spectroscopic monitoring and V-band photometric observations to determine the orbital elements and stellar parameters and to investigate the spectral variability with the orbital phases. We developed an advanced model of the large-scale wind-velocity and wind-density structure with 3-D radiative transfer calculations that fit the orbitally modulated P Cyg profile of HeI λ5876, showing outflow velocities above 1000km/s. We find that MWC 314 is a massive semi-detached binary system of ≃1.22AU, observed at an inclination angle of i=72.8° with an orbital period of 60.8 d and e=0.23. The primary star is a low-vsini LBV candidate of m1=39.6M and R1=86.8R. The detailed radiative transfer fits show that the geometry of wind density is asymmetric around the primary star with increased wind density by a factor of 3.3, which leads the orbit of the primary. The variable orientation causes the orbital modulation that is observed in absorption portions of P Cyg wind lines. Wind accretion in the system produces a circumbinary disc. MWC 314 is in a crucial evolutionary phase of close binary systems, when the massive primary star has its H envelope being stripped and is losing mass to a circumbinary disc. MWC 314 is a key system for studying the evolutionary consequences of these effects.

Abstract Copyright:

Journal keyword(s): stars: emission-line, Be - binaries: spectroscopic - stars: massive - stars: winds, outflows - line: profiles - transfer radiative

CDS comments: Paragraph 1. V1492 Aql is a misprint for V1429 Aql.

Simbad objects: 35

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Number of rows : 35

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 HD 5980 WR* 00 59 26.5847969465 -72 09 53.927725716   11.13 11.31   11.029 WN4+O7I: 355 1
2 HD 14947 s*b 02 26 46.9895793276 +58 52 33.116841083 7.83 8.44 7.98     O4.5If 236 0
3 HD 269128 s*b 05 10 22.7894940469 -68 46 23.818379498 9.77 10.52 10.412 10.29 10.268 B2.5Ieq 92 0
4 V* S Dor sg* 05 18 14.3572490675 -69 15 01.148131817 9.08 10.39 10.25 9.74 9.14 A5Iaeq 338 0
5 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 14380 1
6 SN 1987A SN* 05 35 28.020 -69 16 11.07   4.75 4.81     SN.IIPec 4391 2
7 * zet Tau Be* 05 37 38.6854231 +21 08 33.158804 2.22 2.84 3.03 3.06 3.15 B1IVe_shell 691 0
8 HD 90177 s*b 10 22 53.8426931454 -59 37 28.361118869 9.16 9.66 8 8.15   LBV 300 0
9 * eta Car Em* 10 45 03.5455050 -59 41 03.951060 6.37 7.034 6.21 4.90 4.41 OBepec 2157 0
10 WRAY 15-682 WR* 10 53 59.5776214569 -60 26 44.358376205   11.64 10.85 10.56   WN11h 133 3
11 V* AG Car WR* 10 56 11.5779283438 -60 27 12.809532379 7.00 7.57 6.96 7.73   WN11h 581 0
12 MR 35 s*b 11 08 40.0633818066 -60 42 51.718989987   13.7       LBV 112 0
13 V* BP Cru HXB 12 26 37.5607088371 -62 46 13.259605389   12.70 10.66     B1.5Iaeq 596 0
14 Cl* Westerlund 1 W 243 s*b 16 47 07.5028508821 -45 52 29.152464693   19.873 15.730     LBV 48 0
15 * zet01 Sco s*b 16 53 59.7270104119 -42 21 43.313745214 4.80 5.31 4.79 4.32 3.86 B1Ia-0ek 345 0
16 V* V1104 Sco cC* 17 06 53.9048235955 -42 36 39.705015741 9.68 9.87 9.03 9.51   O 70 0
17 [B61] 2 s*b 17 41 35.4374195439 -30 06 38.782935913   18.0 15.00 14.23 10.30 LBV_B[e]: 43 0
18 HD 160529 sg* 17 41 59.0257256544 -33 30 13.702939546 8.17 7.87 6.66 5.50 4.51 A2Ia 182 1
19 NAME Pistol HII 17 46 15.2 -28 49 49           ~ 59 0
20 [FMM95] 3 Em* 17 46 15.240 -28 50 03.58           ~ 134 1
21 [GMC99] D6 * 17 46 17.982 -28 49 03.46           ~ 52 0
22 WR 102ka WR* 17 46 18.12 -29 01 36.6           WN10 27 0
23 HD 316285 s*b 17 48 14.0369781568 -28 00 53.124817157 11.88 11.27 9.60 9.28   B0Ieq 177 2
24 HD 168607 s*b 18 21 14.8855350307 -16 22 31.760520819 10.23 9.82 8.28 8.55   B9Iaep 171 1
25 HD 168625 s*b 18 21 19.5486475779 -16 22 26.077308888 10.15 9.78 8.37 8.76   B6Iap 246 2
26 V* V481 Sct s*b 18 33 55.2778598542 -06 58 38.634278867           LBV_B[e]: 42 0
27 IRAS 18576+0341 s*b 19 00 10.89456 +03 45 47.1096           B8I 80 1
28 BD+14 3887 Em* 19 21 33.9773483922 +14 52 56.908316938 11.86 11.3 9.89     B3Ibe 76 0
29 HBHA 1203-03 Em* 19 23 47.6416797701 +14 36 39.064626755     15.1     O4I 18 0
30 * 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 1128 1
31 IRAS 20298+4011 Em* 20 31 42.2841507943 +40 21 59.061205285     15.1     B:I[e] 83 0
32 Schulte 12 s*b 20 32 40.9574572449 +41 14 29.276333992 16.1 14.45 11.702     B3-4Ia+ 352 0
33 EM* MWC 349A Em* 20 32 45.518 +40 39 36.62           ~ 141 0
34 SN 2009ip s*b 22 23 08.26 -28 56 52.4           LBV 250 0
35 V* V509 Cas LP* 23 00 05.1007915562 +56 56 43.348681058 8.01 6.68 5.13 3.96 3.11 G4_0 308 0

    Equat.    Gal    SGal    Ecl

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2019.12.10-15:23:36

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