Numerical Relativity Simulations of the Neutron Star Merger GW170817: Long-term Remnant Evolutions, Winds, Remnant Disks, and Nucleosynthesis

被引：122

作者：

Nedora, Vsevolod ^{[1
]}

Bernuzzi, Sebastiano ^{[1
]}

Radice, David ^{[2
,3
,4
]}

Daszuta, Boris ^{[1
]}

Endrizzi, Andrea ^{[1
]}

Perego, Albino ^{[5
,6
]}

Prakash, Aviral ^{[2
,3
]}

Safarzadeh, Mohammadtaher ^{[7
]}

Schianchi, Federico ^{[1
]}

Logoteta, Domenico ^{[8
,9
]}

机构：

[1] Friedrich Schiller Univ Jena, Theoret Phys Inst, D-07743 Jena, Germany

[2] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA

[3] Penn State Univ, Dept Phys, 104 Davey Lab, University Pk, PA 16802 USA

[4] Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA

[5] Univ Trento, Dipartimento Fis, Via Sommar 14, I-38123 Trento, Italy

[6] INFN TIFPA, Trento Inst Fundamental Phys & Applicat, Via Sommar 14, I-38123 Infn Tifpa, Italy

[7] Harvard & Smithsonian, Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA

[8] Univ Pisa, Dipartimento Fis, Largo Pontecorvo 3, I-56127 Pisa, Italy

[9] Ist Nazl Fis Nucl INFN, Largo Pontecorvo 3, I-56127 Pisa, Italy

来源：

ASTROPHYSICAL JOURNAL | 2021年 / 906卷 / 02期

基金：

欧盟地平线“2020”;

关键词：

Gravitational waves; Gravitational wave astronomy; Nucleosynthesis; R-process; STELLAR CORE COLLAPSE; HIGH-RESOLUTION CALCULATIONS; ADAPTIVE MESH REFINEMENT; BLACK-HOLE FORMATION; GAMMA-RAY BURSTS; R-PROCESS; DRIVEN WINDS; DYNAMICAL EJECTA; PHYSICAL MODELS; MASS EJECTION;

D O I：

10.3847/1538-4357/abc9be

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present a systematic numerical relativity study of the dynamical ejecta, winds, and nucleosynthesis in neutron star (NS) merger remnants. Binaries with the chirp mass compatible with GW170817, different mass ratios, and five microphysical equations of state (EOSs) are simulated with an approximate neutrino transport and a subgrid model for magnetohydrodynamic turbulence up to 100 ms postmerger. Spiral density waves propagating from the NS remnant to the disk trigger a wind with mass flux similar to 0.1-0.5 M s(-1), which persists for the entire simulation as long as the remnant does not collapse to a black hole. This wind has average electron fraction greater than or similar to 0.3 and average velocity similar to 0.1-0.17 c and thus is a site for the production of weak r-process elements (mass number A < 195). Disks around long-lived remnants have masses similar to 0.1-0.2 M, temperatures peaking at less than or similar to 10 MeV near the inner edge, and a characteristic double-peak distribution in entropy resulting from shocks propagating through the disk. The dynamical and spiral-wave ejecta computed in our targeted simulations are not compatible with those inferred from AT2017gfo using two-components kilonova models. Rather, they indicate that multicomponent kilonova models including disk winds are necessary to interpret AT2017gfo. The nucleosynthesis in the combined dynamical ejecta and spiral-wave wind in the long-lived mergers of comparable mass robustly accounts for all the r-process peaks, from mass number similar to 75 to actinides in terms of solar abundances. Total abundances are weakly dependent on the EOS, while the mass ratio affects the production of first-peak elements.

引用

页数：20

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