Mass ejection from the merger of binary neutron stars

By K. Hotokezaka, Kentaro Kiuchi, K. Kyutoku, Hirotada Okawa, Y. Sekiguchi, M. Shibata, K. Taniguchi. 2012

338 citations recorded by the source corpus.

Numerical-relativity simulations for the merger of binary neutron stars are performed for a variety of equations of state (EOSs) and for a plausible range of the neutron-star mass, focusing primarily on the properties of the material ejected from the system. We find that a fraction of the material is ejected as a mildly relativistic and mildly anisotropic outflow with the typical and maximum velocities $\sim 0.15$ -- $0.25c$ and $\sim 0.5$ -- $0.8c$ (where $c$ is the speed of light), respectively, and that the total ejected rest mass is in a wide range $10^{-4}$ -- $10^{-2}M_{\odot}$, which depends strongly on the EOS, the total mass, and the mass ratio. The total kinetic energy ejected is also in a wide range between $10^{49}$ and $10^{51} {\rm ergs}$. The numerical results suggest that for a binary of canonical total mass $2.7M_{\odot}$, the outflow could generate an electromagnetic signal observable by the planned telescopes through the production of heavy-element unstable nuclei via the $r$-process or through the formation of blast waves during the interaction with the interstellar matter, if the EOS and mass of the binary are favorable ones.

Subfields: Astronomy and Astrophysics, Geophysics

View Paper: https://www.semanticscholar.org/paper/331b5dfa3d676ea4bc7120f6a23d75ffc9dc9350

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

In Geophysics

Citations in the corpus

Mass Ejection from the Remnant of a Binary Neutron Star Merger: Viscous-radiation Hydrodynamics Study (2017, background): “First, during the merger, the dynamical mass ejection occurs(e.g., Hotokezaka et al. 2013b; Sekiguchi et al. 2015, 2016).”
The long-term evolution of neutron star merger remnants { II. Radioactively powered transients (2013, methodology): “The observed magnitude is consistent with the models of Barnes & Kasen (2013); Tanaka & Hotokezaka (2013) and Hotokezaka et al. (2013).”
Delayed outflows from black hole accretion tori following neutron star binary coalescence (2013, background): “Although the quantity of matter expelled in dynamical ‘tidal tails’ from the merger can be large (& 10−2M⊙) in some cases (e.g. eccentric mergers; East et al. 2012), it is often found to be significantly smaller (∼ 10−4 − 10−3M⊙; Hotokezaka et al. 2013).”
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).”
Neutron-powered precursors of kilonovae (2014, background): “This fastest expanding matter originates from the shock-heated interface between the NSs, a component of the ejecta seen previously in other general relativistic (GR) simulations (e.g. Oechslin et al. 2007; Goriely et al. 2011; Hotokezaka et al. 2013).”
Red or blue? A potential kilonova imprint of the delay until black hole formation following a neutron star merger (2014, background): “For particularly nearby mergers, oscillations excited in the HMNS may be detectable in the GW strain data (Shibata 2005; Bauswein et al. 2012; Hotokezaka et al. 2013b).”
Constraining the Maximum Mass of Neutron Stars from Multi-messenger Observations of GW170817 (2017, background): “First, matter is ejected on the dynamical timescale, either by tidal forces (e.g. Ruffert et al. 1997; Rosswog et al. 1999; Radice et al. 2016) or by shock heating at the interface between the merging NSs (e.g. Oechslin et al. 2007a; Bauswein et al. 2013; Hotokezaka et al. 2013).”
The rate, luminosity function and time delay of non-Collapsar short GRBs (2014, background): “If the interpretation of this IR signal as macronova is correct it implies that 0.02–0.04 rprocess material were produced in this event (Barnes & Kasen 2013; Hotokezaka et al. 2013; Grossman et al. 2014; Piran, Korobkin & Rosswog 2014).”
r-process Nucleosynthesis from Three-dimensional Magnetorotational Core-collapse Supernovae (2017, background): “The amount of ejected r-process material has been found to be ∼ 10−3 − 10−2 M in previous studies (Winteler et al. 2012; Nishimura et al. 2015), similar to what is expected from binary neutron star mergers (e.g., (Hotokezaka et al. 2013)).”
A Magnetar Origin for the Kilonova Ejecta in GW170817 (2018, background): “2–0.3 c; e.g., Rosswog et al. 1999; Oechslin & Janka 2006; Bauswein et al. 2013; Hotokezaka et al. 2013; Sekiguchi et al. 2016; Bovard et al. 2017; Dietrich et al. 2017).”
Production of the entire range of r-process nuclides by black hole accretion disc outflows from neutron star mergers (2016, background): “Numerical simulations of these events show that a robust outcome of the merger is the ejection of ∼ 10−4– 10−1 M of highly neutron-rich matter on the dynamical time (e.g. Hotokezaka et al. 2013, Bauswein et al. 2013; see Lehner & Pretorius 2014 and Baiotti & Rezzolla 2016 for recent reviews).”
Dynamical Mass Ejection from Binary Neutron Star Mergers (2016, background): “Mass ejection may change quantitatively and possibly qualitatively with different EOS and with unequal mass binaries (Rezzolla et al. 2010; Hotokezaka et al. 2013; Bauswein et al. 2013; Sekiguchi et al. 2015; Dietrich et al. 2015; Palenzuela et al. 2015; Foucart et al. 2016), or with the inclusion…”
Optical and X-ray emission from stable millisecond magnetars formed from the merger of binary neutron stars (2013, background): “The region surrounding the site of the merger is polluted by mass ejected dynamically during the merger itself (e.g., Rosswog et al. 2012; Hotokezaka et al. 2013), and in subsequent outflows from the remnant accretion disk or the hyper-massive NS (Metzger et al. 2008; Dessart et al. 2009; Caballero…”
Constraints on the neutron star equation of state from AT2017gfo using radiative transfer simulations (2018, background): “While the velocity scale of the blue ejecta naturally matches expectations for the dynamical ejecta (e.g. Bauswein et al. 2013b; Hotokezaka et al. 2013), the relatively large quantity that we infer appears in tension with current GR merger simulations that focus on dynamical ejection mechanism.”
Binary Neutron Star Mergers: Mass Ejection, Electromagnetic Counterparts, and Nucleosynthesis (2018, methodology): “In comparison to previous studies (Oechslin et al. 2007; Hotokezaka et al. 2013b, as reported in Wu et al. 2016) we find that disk winds and viscous outflows should contribute a significantly larger fraction of the overall ejecta.”
A living theory catalogue for fast radio bursts (2018, background): “, 1973), DSR has been invoked as one of the few “microphysical” FRB models (Houde et al., 2018).”