The Tarantula Massive Binary Monitoring II. First SB2 orbital and spectroscopic analysis for the Wolf-Rayet binary R145

被引：41

作者：

Shenar, T. ^{[1
]}

Richardson, N. D. ^{[2
]}

Sablowski, D. P. ^{[3
]}

Hainich, R. ^{[1
]}

Sana, H. ^{[4
]}

Moffat, A. F. J. ^{[5
,6
]}

Todt, H. ^{[1
]}

Hamann, W. -R. ^{[1
]}

Oskinova, L. M. ^{[1
]}

Sander, A. ^{[1
]}

Tramper, F. ^{[7
]}

Langer, N. ^{[8
]}

Bonanos, A. Z. ^{[9
]}

de Mink, S. E. ^{[10
]}

Grafener, G. ^{[11
]}

Crowther, P. A. ^{[12
]}

Vink, J. S. ^{[11
]}

Almeida, L. A. ^{[13
,14
]}

de Koter, A. ^{[4
,10
]}

Barba, R. ^{[15
]}

Herrero, A. ^{[16
]}

Ulaczyk, K. ^{[17
]}

机构：

[1] Univ Potsdam, Inst Phys & Astron, Karl Liebknecht Str 24-25, D-14476 Potsdam, Germany

[2] Univ Toledo, Dept Phys & Astron, Ritter Observ, 2801 W Bancroft St, Toledo, OH 43606 USA

[3] Leibniz Inst Astrophys Potsdam, Sternwarte 16, D-14482 Potsdam, Germany

[4] Katholieke Univ Leuven, Inst Astrophys, Celestijnenlaan 200 D, B-3001 Leuven, Belgium

[5] Univ Montreal, Dept Phys, CP 6128,Succ Ctr Ville, Montreal, PQ H3C 3J7, Canada

[6] Univ Montreal, Ctr Rech Astrophys Quebec, CP 6128,Succ Ctr Ville, Montreal, PQ H3C 3J7, Canada

[7] European Space Astron Ctr ESA ESAC, POB 78, Madrid 28691, Spain

[8] Univ Bonn, Argelander Inst Astron, Hugel 71, D-53121 Bonn, Germany

[9] Natl Observ Athens, IAASARS, Penteli 15236, Greece

[10] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands

[11] Armagh Observ, Coll Hill, Armagh BT61 9DG, North Ireland

[12] Univ Sheffield, Dept Phys & Astron, Sheffield S3 7RH, S Yorkshire, England

[13] Inst Astron Geofis & Ciencias, Rua Matao 1226, Sao Paulo, SP, Brazil

[14] Johns Hopkins Univ, Dept Phys & Astron, Bloomberg Ctr Phys & Astron, 3400N Charles St, Baltimore, MD 21218 USA

[15] Univ la Serena, Dept Fis & Astron, Av Juan Cisternas 1200 Norte, La Serena, Chile

[16] Univ La Laguna, Inst Astrofis, Avda Astrofis Francisco Sanchez S-N, Tenerife 38071, Spain

[17] Univ Warsaw Observ, Al Ujazdowskie 4, PL-00478 Warsaw, Poland

来源：

ASTRONOMY & ASTROPHYSICS | 2017年 / 598卷

基金：

巴西圣保罗研究基金会; 加拿大自然科学与工程研究理事会;

关键词：

binaries: spectroscopic; stars: Wolf-Rayet; stars: massive; Magellanic Clouds; stars: individual: R 145; stars: atmospheres; LARGE-MAGELLANIC-CLOUD; BLANKETED MODEL ATMOSPHERES; X-RAY; ECLIPSING-BINARY; COLLIDING WINDS; PRESUPERNOVA EVOLUTION; OBSERVATIONAL CAMPAIGN; ACCURATE DETERMINATION; STELLAR EVOLUTION; SPECTRAL-ANALYSIS;

D O I：

10.1051/0004-6361/201629621

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present the first SB2 orbital solution and disentanglement of the massive Wolf-Rayet binary R145 (P = 159 d) located in the Large Magellanic Cloud. The primary was claimed to have a stellar mass greater than 300 M-circle dot, making it a candidate for being the most massive star known to date. While the primary is a known late-type, H-rich Wolf-Rayet star (WN6h), the secondary has so far not been unambiguously detected. Using moderate-resolution spectra, we are able to derive accurate radial velocities for both components. By performing simultaneous orbital and polarimetric analyses, we derive the complete set of orbital parameters, including the inclination. The spectra are disentangled and spectroscopically analyzed, and an analysis of the wind-wind collision zone is conducted. The disentangled spectra and our models are consistent with a WN6h type for the primary and suggest that the secondary is an O3.5 If*/WN7 type star. We derive a high eccentricity of e = 0 : 78 and minimum masses of M-1 sin(3) i approximate to M-2 sin(3) i = 13 +/- 2 M-circle dot, with q = M-2/M-1 = 1.01 +/- 0.07. An analysis of emission excess stemming from a wind-wind collision yields an inclination similar to that obtained from polarimetry (i = 39 +/- 6 degrees). Our analysis thus implies M-1 = 53(-20)(+40) and M2 = 54(-20)(+40) M-circle dot, excluding M-1 > 300 M-circle dot. A detailed comparison with evolution tracks calculated for single and binary stars together with the high eccentricity suggests that the components of the system underwent quasi-homogeneous evolution and avoided mass-transfer. This scenario would suggest current masses of approximate to 80 M-circle dot and initial masses of M-i,M-1 approximate to 10(5) and M-i,M-2 approximate to 90 M-circle dot, consistent with the upper limits of our derived orbital masses, and would imply an age of approximate to 2.2 Myr.

引用

页数：16

共 115 条

[1] Observation of Gravitational Waves from a Binary Black Hole Merger [J].

Abbott, B. P. ;

Abbott, R. ;

Abbott, T. D. ;

Abernathy, M. R. ;

Acernese, F. ;

Ackley, K. ;

Adams, C. ;

Adams, T. ;

Addesso, P. ;

Adhikari, R. X. ;

Adya, V. B. ;

Affeldt, C. ;

Agathos, M. ;

Agatsuma, K. ;

Aggarwal, N. ;

Aguiar, O. D. ;

Aiello, L. ;

Ain, A. ;

Ajith, P. ;

Allen, B. ;

Allocca, A. ;

Altin, P. A. ;

Anderson, S. B. ;

Anderson, W. G. ;

Arai, K. ;

Arain, M. A. ;

Araya, M. C. ;

Arceneaux, C. C. ;

Areeda, J. S. ;

Arnaud, N. ;

Arun, K. G. ;

Ascenzi, S. ;

Ashton, G. ;

Ast, M. ;

Aston, S. M. ;

Astone, P. ;

Aufmuth, P. ;

Aulbert, C. ;

Babak, S. ;

Bacon, P. ;

Bader, M. K. M. ;

Baker, P. T. ;

Baldaccini, F. ;

Ballardin, G. ;

Ballmer, S. W. ;

Barayoga, J. C. ;

Barclay, S. E. ;

Barish, B. C. ;

Barker, D. ;

Barone, F. .

PHYSICAL REVIEW LETTERS, 2016, 116 (06)

[2] THE MULTIPLICITY OF MASSIVE STARS: A HIGH ANGULAR RESOLUTION SURVEY WITH THE HST FINE GUIDANCE SENSOR [J].

Aldoretta, E. J. ;

Caballero-Nieves, S. M. ;

Gies, D. R. ;

Nelan, E. P. ;

Wallace, D. J. ;

Hartkopf, W. I. ;

Henry, T. J. ;

Jao, W. -C. ;

Maiz Apellaniz, J. ;

Mason, B. D. ;

Moffat, A. F. J. ;

Norris, R. P. ;

Richardson, N. D. ;

Williams, S. J. .

ASTRONOMICAL JOURNAL, 2015, 149 (01)

[3] The Tarantula Massive Binary Monitoring I. Observational campaign and OB-type spectroscopic binaries [J].

Almeida, L. A. ;

Sana, H. ;

Taylor, W. ;

Barba, R. ;

Bonanos, A. Z. ;

Crowther, P. ;

Damineli, A. ;

de Koter, A. ;

de Mink, S. E. ;

Evans, C. J. ;

Gieles, M. ;

Grin, N. J. ;

Henault-Brunet, V. ;

Langer, N. ;

Lennon, D. ;

Lockwood, S. ;

Maiz Apellaniz, J. ;

Moffat, A. F. J. ;

Neijssel, C. ;

Norman, C. ;

Ramirez-Agudelo, O. H. ;

Richardson, N. D. ;

Schootemeijer, A. ;

Shenar, T. ;

Soszynski, I. ;

Tramper, F. ;

Vink, J. S. .

ASTRONOMY & ASTROPHYSICS, 2017, 598

[4] ACCURATE MASSES AND RADII OF NORMAL STARS [J].

ANDERSEN, J .

ASTRONOMY AND ASTROPHYSICS REVIEW, 1991, 3 (02) :91-126

[5]

[Anonymous], MESSENGER

[6]

[Anonymous], IAU S

[7]

[Anonymous], A A

[8]

[Anonymous], PASP

[9]

[Anonymous], 2015, Highlights of Astronomy, DOI DOI 10.1017/S1743921314004657

[10] POLARIMETRIC ACCURACY REQUIRED FOR THE DETERMINATION OF BINARY INCLINATIONS [J].

ASPIN, C ;

SIMMONS, JFL ;

BROWN, JC .

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 1981, 194 (01) :283-291

← 1 2 3 4 5 6 7 8 9 10 →