Dynamical mass ejection from the merger of asymmetric binary neutron stars: Radiation-hydrodynamics study in general relativity

By Yuichiro Sekiguchi, Kentaro Kiuchi, K. Kyutoku, M. Shibata, K. Taniguchi. 2016

169 citations recorded by the source corpus.

EOS (DD2), with the increase of the mass asymmetry degree, the total ejecta mass signicantly increases while the average of Ye and s moderately decreases. We nd again that only for the soft EOS (SFHo), the total ejecta mass exceeds 0:01M irrespective of the mass ratio chosen in this paper. The ejecta have a variety of electron number per baryon with its average approximately between Ye 0:2 and 0:3 irrespective of the EOS employed, which is well-suited for the production of the r-process heavy elements (second and third peaks), although its averaged value decreases with the increase of the degree of mass asymmetry.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/1772c4577765006c1742543f0f59275e74bf83d1

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In Astronomy and Astrophysics

1. B. Metzger
2. E. Quataert
3. E. Berger
4. D. Kasen
5. David Radice
6. R. Fern'andez
7. Luke F. Roberts
8. Albino Perego

Citations in the corpus

• Using Gravitational-wave Observations and Quasi-universal Relations to Constrain the Maximum Mass of Neutron Stars (2017, background): “…profile (Hanauske et al. 2017), but also of microphysical ones, such as the efficiency of energy transport via neutrinos (Palenzuela et al. 2015; Sekiguchi et al. 2016; Bovard et al. 2017) and the redistribution of angular momentum via magnetic fields (Siegel et al. 2014; Palenzuela et al.…”
• Neutron-star Radius Constraints from GW170817 and Future Detections (2017, background): “…this merger outcome tends to produce larger ejecta masses as compared to a direct collapse (Bauswein et al. 2013b; Hotokezaka et al. 2013; Fernández & Metzger 2013; Metzger & Fernández 2014; Perego et al. 2014; Siegel et al. 2014; Wanajo et al. 2014; Just et al. 2015; Sekiguchi et al. 2016).”
• Impact of ejecta morphology and composition on the electromagnetic signatures of neutron star mergers (2017, background): “Dynamical ejecta have been studied extensively (Rosswog et al. 1999; Rosswog 2013; Bauswein et al. 2013; Hotokezaka et al. 2013; Sekiguchi et al. 2016; Lehner et al. 2016; Rosswog et al. 2017; Endrizzi et al. 2016), and the consensus on the value of total ejected mass is the range between 10−4 and ∼”
• The Origin of r-process Elements in the Milky Way (2017, background): “Estimates of the dynamical ejecta mass in various theoretical models vary from 10−4M to 0.1M (see e.g. Hotokezaka et al. 2013, Sekiguchi et al. 2016, Lehner et al. 2016, Bovard et al. 2017, Côté et al. 2017a, and Dietrich & Ujevic 2017 for reviews).”
• The Electromagnetic Counterpart of the Binary Neutron Star Merger LIGO/Virgo GW170817. III. Optical and UV Spectra of a Blue Kilonova from Fast Polar Ejecta (2017, background): “…consistent with the findings by Cowperthwaite et al. (2017), and is close to the escape ve- locity from neutron stars, matching theoretical predictions for the dynamical polar ejecta from the collision interface in a BNS merger (Hotokezaka et al. 2013; Bauswein et al. 2013; Sekiguchi et al. 2016).”
• Constraining the Maximum Mass of Neutron Stars from Multi-messenger Observations of GW170817 (2017, methodology): “Matter from the shocked interface expands into the polar direction and possesses a higher Ye & 0.25 (Wanajo et al. 2014; Sekiguchi et al. 2016).”
• Mass Ejection from the Remnant of a Binary Neutron Star Merger: Viscous-radiation Hydrodynamics Study (2017, background): “7 with the mass ratio between 0.85 and 1 (Sekiguchi et al. 2016).”
• Long-term GRMHD simulations of neutron star merger accretion discs: implications for electromagnetic counterparts (2018, methodology): “The ratio of internal energy to gravitational energy at the density peak is 15%, resulting in H/R ' 0.35 as generally obtained in full-physics simulations of NS-NS mergers (e.g., Sekiguchi et al. 2016).”
• RADIOACTIVITY AND THERMALIZATION IN THE EJECTA OF COMPACT OBJECT MERGERS AND THEIR IMPACT ON KILONOVA LIGHT CURVES (2016, background): “Recent hydrodynamic simulations (Bauswein et al. 2013; Hotokezaka et al. 2013; Kyutoku et al. 2015; Sekiguchi et al. 2016) suggest that mergers dynamically eject between ∼10−4 and a few ×10−2 M of material, with bulk velocities of a few tenths the speed of light.”
• GW170817: Joint Constraint on the Neutron Star Equation of State from Multimessenger Observations (2017, background): “…material can be unbound dynamically during the merger itself (Bauswein et al. 2013b; Hotokezaka et al. 2013; Lehner et al. 2016; Radice et al. 2016; Sekiguchi et al. 2016; Bovard et al. 2017; Dietrich et al. 2017b), although larger ejecta masses can be reached for small mass ratios q 0.6…”
• The Electromagnetic Counterpart of the Binary Neutron Star Merger LIGO/Virgo GW170817. II. UV, Optical, and Near-infrared Light Curves and Comparison to Kilonova Models (2017, background): “In both models, the high velocity of the blue KN ejecta suggests that it originates from the shock-heated polar region created when the neutron stars collide (e.g., Oechslin et al. 2007; Bauswein et al. 2013; Sekiguchi et al. 2016).”
• Origin of the heavy elements in binary neutron-star mergers from a gravitational-wave event (2017, background): “    + − X v X X v v X ( ) ( ) 1 (7) n”