ASTROPHYSICAL IMPLICATIONS OF THE BINARY BLACK HOLE MERGER GW150914

被引：520

作者：

Abbott, B. P. ^{[1
]}

Abbott, R. ^{[1
]}

Abbott, T. D. ^{[2
]}

Abernathy, M. R. ^{[1
]}

Acernese, F. ^{[3
,4
]}

Ackley, K. ^{[5
]}

Adams, C. ^{[6
]}

Adams, T. ^{[7
]}

Addesso, P. ^{[3
]}

Adhikari, R. X. ^{[1
]}

Adya, V. B. ^{[8
]}

Affeldt, C. ^{[8
]}

Agathos, M. ^{[9
]}

Agatsuma, K. ^{[9
]}

Aggarwal, N. ^{[10
]}

Aguiar, O. D. ^{[11
]}

Aiello, L. ^{[12
,13
]}

Ain, A. ^{[14
]}

Ajith, P. ^{[15
]}

Allen, B. ^{[16
,17
]}

Allocca, A. ^{[18
,19
]}

Altin, P. A. ^{[20
]}

Anderson, S. B. ^{[1
]}

Anderson, W. G. ^{[16
]}

Arai, K. ^{[1
]}

Araya, M. C. ^{[1
]}

Arceneaux, C. C. ^{[21
]}

Areeda, J. S. ^{[22
]}

Arnaud, N. ^{[23
]}

Arun, K. G. ^{[24
]}

Ascenzi, S. ^{[13
,25
]}

Ashton, G. ^{[26
]}

Ast, M. ^{[27
]}

Aston, S. M. ^{[6
]}

Astone, P. ^{[28
]}

Aufmuth, P. ^{[8
]}

Aulbert, C. ^{[8
]}

Babak, S. ^{[29
]}

Bacon, P. ^{[30
]}

Bader, M. K. M. ^{[9
]}

Baker, P. T. ^{[31
]}

Baldaccini, F. ^{[32
,33
]}

Ballardin, G. ^{[34
]}

Ballmer, S. W. ^{[35
]}

Barayoga, J. C. ^{[1
]}

Barclay, S. E. ^{[36
]}

Barish, B. C. ^{[1
]}

Barker, D. ^{[37
]}

Barone, F. ^{[3
,4
]}

Barr, B. ^{[36
]}

机构：

[1] CALTECH, LIGO, Pasadena, CA 91125 USA

[2] Louisiana State Univ, Baton Rouge, LA 70803 USA

[3] Univ Salerno, I-84084 Salerno, Italy

[4] Ist Nazl Fis Nucl, Sez Napoli, Complesso Univ Monte S Angelo, I-80126 Naples, Italy

[5] Univ Florida, Gainesville, FL 32611 USA

[6] LIGO Livingston Observ, Livingston, LA 70754 USA

[7] Univ Savoie Mt Blanc, CNRS, IN2P3, LAPP, F-74941 Annecy Le Vieux, France

[8] Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-30167 Hannover, Germany

[9] Nikhef, Sci Pk, NL-1098 XG Amsterdam, Netherlands

[10] MIT, LIGO, 77 Massachusetts Ave, Cambridge, MA 02139 USA

[11] Inst Nacl Pesquisas Espaciais, BR-12227010 Sao Jose Dos Campos, SP, Brazil

[12] Ist Nazl Fis Nucl, Gran Sasso Sci Inst, I-67100 Laquila, Italy

[13] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy

[14] Interuniv Ctr Astron & Astrophys, Pune 411007, Maharashtra, India

[15] Tata Inst Fundamental Res, Int Ctr Theoret Sci, Bangalore 560012, Karnataka, India

[16] Univ Wisconsin, Milwaukee, WI 53201 USA

[17] Leibniz Univ Hannover, D-30167 Hannover, Germany

[18] Univ Pisa, I-56127 Pisa, Italy

[19] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy

[20] Australian Natl Univ, GPO Box 4, Canberra, ACT 0200, Australia

[21] Univ Mississippi, Oxford, MS 38677 USA

[22] Calif State Univ Fullerton, Fullerton, CA 92831 USA

[23] Univ Paris Saclay, Univ Paris Sud, CNRS, LAL,IN2P3, Orsay, France

[24] Chennai Math Inst, Chennai, Tamil Nadu, India

[25] Univ Roma Tor Vergata, I-00133 Rome, Italy

[26] Univ Southampton, Southampton SO17 1BJ, Hants, England

[27] Univ Hamburg, D-22761 Hamburg, Germany

[28] Ist Nazl Fis Nucl, Sez Roma, I-00185 Rome, Italy

[29] Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-14476 Potsdam, Germany

[30] Univ Paris Diderot, Sorbonne Paris Cite, CNRS, APC,AstroParticule & Cosmol,IN2P3,CEA,Irfu, F-75205 Paris 13, France

[31] Montana State Univ, Bozeman, MT 59717 USA

[32] Univ Perugia, I-06123 Perugia, Italy

[33] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy

[34] EGO, I-56021 Pisa, Italy

[35] Syracuse Univ, Syracuse, NY 13244 USA

[36] Univ Glasgow, SUPA, Glasgow G12 8QQ, Lanark, Scotland

[37] LIGO Hanford Observ, Richland, WA 99352 USA

[38] RMKI, Wigner RCP, Konkoly Thege Mikos Ut 29-33, H-1121 Budapest, Hungary

[39] Columbia Univ, New York, NY 10027 USA

[40] Stanford Univ, Stanford, CA 94305 USA

[41] Univ Padua, Dipartimento Fis & Astron, I-35131 Padua, Italy

[42] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy

[43] CAMK PAN, PL-00716 Warsaw, Poland

[44] Warsaw Univ, Astron Observ, PL-00478 Warsaw, Poland

[45] Univ Birmingham, Birmingham B15 2TT, W Midlands, England

[46] Univ Genoa, I-16146 Genoa, Italy

[47] Ist Nazl Fis Nucl, Sez Genova, I-16146 Genoa, Italy

[48] RRCAT, Indore 452013, MP, India

[49] Moscow MV Lomonosov State Univ, Fac Phys, Moscow 119991, Russia

[50] Univ West Scotland, SUPA, Paisley PA1 2BE, Renfrew, Scotland

来源：

ASTROPHYSICAL JOURNAL LETTERS | 2016年 / 818卷 / 02期

基金：

美国国家科学基金会; 英国科学技术设施理事会; 新加坡国家研究基金会; 澳大利亚研究理事会;

关键词：

gravitational waves; stars: black holes; stars: massive; GRAVITATIONAL-WAVE SOURCES; YOUNG STAR-CLUSTERS; COMPACT-OBJECT BINARIES; NEUTRON-STAR; MAXIMUM MASS; DIFFERENT METALLICITIES; STELLAR EVOLUTION; PAIR-INSTABILITY; SYNTHESIS MODELS; GRAVITY-WAVES;

D O I：

10.3847/2041-8205/818/2/L22

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The discovery of the gravitational-wave (GW) source GW150914 with the Advanced LIGO detectors provides the first observational evidence for the existence of binary black hole (BH) systems that inspiral and merge within the age of the universe. Such BH mergers have been predicted in two main types of formation models, involving isolated binaries in galactic fields or dynamical interactions in young and old dense stellar environments. The measured masses robustly demonstrate that relatively "heavy" BHs (greater than or similar to 25M(circle dot)) can form in nature. This discovery implies relatively weak massive-star winds and thus the formation of GW150914 in an environment with a metallicity lower than about 1/2 of the solar value. The rate of binary-BH (BBH) mergers inferred from the observation of GW150914 is consistent with the higher end of rate predictions (greater than or similar to 1 Gpc(-3) yr(-1)) from both types of formation models. The low measured redshift (z similar or equal to 0.1) of GW150914 and the low inferred metallicity of the stellar progenitor imply either BBH formation in a low-mass galaxy in the local universe and a prompt merger, or formation at high redshift with a time delay between formation and merger of several Gyr. This discovery motivates further studies of binary-BH formation astrophysics. It also has implications for future detections and studies by Advanced LIGO and Advanced Virgo, and GW detectors in space.

引用

页数：15

共 143 条

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