Estimating the Contribution of Dynamical Ejecta in the Kilonova Associated with GW170817

被引：98

作者：

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

Abbott, R. ^{[1
]}

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

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

Ackley, K. ^{[5
,6
]}

Adams, C. ^{[7
]}

Adams, T. ^{[8
]}

Addesso, P. ^{[9
,10
]}

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

Adya, V. B. ^{[11
]}

Affeldt, C. ^{[11
]}

Afrough, M. ^{[12
]}

Agarwal, B. ^{[13
]}

Agathos, M. ^{[14
]}

Agatsuma, K. ^{[15
]}

Aggarwal, N. ^{[16
]}

Aguiar, O. D. ^{[17
]}

Aiello, L. ^{[18
,19
]}

Ain, A. ^{[20
]}

Ajith, P. ^{[21
]}

Allen, B. ^{[11
,22
,23
]}

Allen, G. ^{[13
]}

Allocca, A. ^{[24
,25
]}

Altin, P. A. ^{[26
]}

Amato, A. ^{[27
]}

Ananyeva, A. ^{[1
]}

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

Anderson, W. G. ^{[22
]}

Angelova, S. V. ^{[28
]}

Antier, S. ^{[29
]}

Appert, S. ^{[1
]}

Arai, K. ^{[1
]}

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

Areeda, J. S. ^{[30
]}

Arnaud, N. ^{[29
,31
]}

Arun, K. G. ^{[32
]}

Ascenzi, S. ^{[33
,34
]}

Ashton, G. ^{[11
]}

Ast, M. ^{[35
]}

Aston, S. M. ^{[7
]}

Astone, P. ^{[36
]}

Atallah, D. V. ^{[37
]}

Aufmuth, P. ^{[23
]}

Aulbert, C. ^{[11
]}

AultONeal, K. ^{[38
]}

Austin, C. ^{[2
]}

Avila-Alvarez, A. ^{[30
]}

Babak, S. ^{[39
]}

Bacon, P. ^{[40
]}

Bader, M. K. M. ^{[15
]}

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] Complesso Univ Monte S Angelo, INFN, Sez Napoli, I-80126 Naples, Italy

[5] Univ Florida, Gainesville, FL 32611 USA

[6] Monash Univ, Sch Phys & Astron, OzGrav, Clayton, Vic 3800, Australia

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

[8] Univ Savoie Mont Blanc, Lab Annecy Le Vieux Phys Particules, CNRS, IN2P3, F-74941 Annecy Le Vieux, France

[9] Univ Sannio Benevento, I-82100 Benevento, Italy

[10] INFN, Sez Napoli, I-80100 Naples, Italy

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

[12] Univ Mississippi, University, MS 38677 USA

[13] Univ Illinois, NCSA, Urbana, IL 61801 USA

[14] Univ Cambridge, Cambridge CB2 1TN, England

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

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

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

[18] Gran Sasso Sci Inst, I-67100 Laquila, Italy

[19] INFN, Lab Nazl Gran Sasso, Assergi, Italy

[20] Inter Univ Ctr Astron & Astrophys, Pune 411007, Maharashtra, India

[21] Tata Inst Fundamental Res, Int Ctr Theoret Sci, Bengaluru 560089, India

[22] Univ Wisconsin Milwaukee, Milwaukee, WI 53201 USA

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

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

[25] INFN, Sez Pisa, I-56127 Pisa, Italy

[26] Australian Natl Univ, OzGrav, Canberra, ACT 0200, Australia

[27] CNRS, IN2P3, LMA, F-69622 Villeurbanne, France

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

[29] Univ Paris Saclay, CNRS, IN2P3, LAL,Univ Paris Sud, F-91898 Orsay, France

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

[31] EGO, I-56021 Pisa, Italy

[32] Chennai Math Inst, Chennai 603103, Tamil Nadu, India

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

[34] INFN, Sez Roma Tor Vergata, I-00133 Rome, Italy

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

[36] INFN, Sez Roma, I-00185 Rome, Italy

[37] Cardiff Univ, Cardiff CF24 3AA, S Glam, Wales

[38] Embry Riddle Aeronaut Univ, Prescott, AZ 86301 USA

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

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

[41] Korea Inst Sci & Technol Informat, Daejeon 34141, South Korea

[42] West Virginia Univ, Morgantown, WV 26506 USA

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

[44] INFN, Sez Perugia, I-06123 Perugia, Italy

[45] Univ Minnesota, Minneapolis, MN 55455 USA

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

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

[48] CALTECH, CaRT, Pasadena, CA 91125 USA

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

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

来源：

ASTROPHYSICAL JOURNAL LETTERS | 2017年 / 850卷 / 02期

基金：

美国国家科学基金会; 澳大利亚研究理事会; 瑞士国家科学基金会; 英国科学技术设施理事会; 匈牙利科学研究基金会; 俄罗斯科学基金会; 新加坡国家研究基金会; 中国国家自然科学基金; 俄罗斯基础研究基金会;

关键词：

gravitational waves; methods: data analysis; stars: neutron; R-PROCESS NUCLEOSYNTHESIS; NEUTRINO-DRIVEN WINDS; EQUATION-OF-STATE; ELECTROMAGNETIC COUNTERPART; MASS EJECTION; MERGERS; ELEMENTS; EVENT; SUPERNOVAE; MATTER;

D O I：

10.3847/2041-8213/aa9478

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The source of the gravitational-wave (GW) signal GW170817, very likely a binary neutron star merger, was also observed electromagnetically, providing the first multi-messenger observations of this type. The two-week-long electromagnetic (EM) counterpart had a signature indicative of an r-process-induced optical transient known as a kilonova. This Letter examines how the mass of the dynamical ejecta can be estimated without a direct electromagnetic observation of the kilonova, using GW measurements and a phenomenological model calibrated to numerical simulations of mergers with dynamical ejecta. Specifically, we apply the model to the binary masses inferred from the GW measurements, and use the resulting mass of the dynamical ejecta to estimate its contribution (without the effects of wind ejecta) to the corresponding kilonova light curves from various models. The distributions of dynamical ejecta mass range between M-ej = 10(-3) - 10(-2) M-circle dot for various equations of state, assuming that the neutron stars are rotating slowly. In addition, we use our estimates of the dynamical ejecta mass and the neutron star merger rates inferred from GW170817 to constrain the contribution of events like this to the r-process element abundance in the Galaxy when ejecta mass from post-merger winds is neglected. We find that if greater than or similar to 10% of the matter dynamically ejected from binary neutron star (BNS) mergers is converted to r-process elements, GW170817-like BNS mergers could fully account for the amount of r-process material observed in the Milky Way.

引用

页数：13

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