High‐resolution calculations of merging neutron stars – II. Neutrino emission

By Stephan Rosswog, Mathias Liebendörfer. 2003

231 citations recorded by the source corpus.

The remnant resulting from the merger of two neutron stars produces neutrinos in copious amounts. In this paper we present the neutrino emission results obtained via Newtonian, high-resolution simulations of the coalescence event. These simulations use three-dimensional smoothed particle hydrodynamics together with a nuclear, temperature-dependent equation of state and a multiflavour neutrino leakage scheme. We present the details of our scheme, discuss the neutrino emission results from a neutron star coalescence and compare them with the core-collapse supernova case where neutrino emission has been studied for several decades. The average neutrino energies are similar to those in the supernova case, but contrary to the latter, the luminosities are dominated by electron-type antineutrinos that are produced in the hot, neutron-rich, thick disc of the merger remnant. The cooler parts of this disc contain substantial fractions of heavy nuclei, which, however, do not influence the overall neutrino emission results significantly. Our total neutrino luminosities from the merger event are considerably lower than those found in previous investigations. This imposes constraints on the ability of neutron star mergers to produce a gamma-ray burst via neutrino annihilation. The neutrinos are emitted preferentially along the initial binary rotation axis, an event seen ‘pole-on’ would appear much brighter in neutrinos than a similar event seen ‘edge-on’.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/a6b52953c720bf377909ef46498d32f8998106b8

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Citations in the corpus

Optical and X-ray emission from stable millisecond magnetars formed from the merger of binary neutron stars (2013, methodology): “⋆ E-mail: bmetzger@phys.columbia.edu Numerical simulations of the merger process (e.g., Ruffert & Janka 1999; Uryū et al. 2000; Rosswog & Liebendörfer 2003; Oechslin & Janka 2006; Chawla et al. 2010; Rezzolla et al. 2010; Hotokezaka et al. 2011) show that initially the end product is a…”
Neutrino-driven winds from neutron star merger remnants (2014, methodology): “For the central compact object, the cooling time-scale tcool, ns is governed by neutrino diffusion (see e.g. Rosswog & Liebendörfer 2003).”
Astrophysical smooth particle hydrodynamics (2009, methodology): “To model compact object mergers, neutrinos have been implemented into SPH via a hybrid, particlemesh approach (Rosswog and Liebendörfer, 2003) and by using local disk scale heights to estimate neutrino opacities (Lee et al., 2004, 2005).”
Delayed outflows from black hole accretion tori following neutron star binary coalescence (2013, background): “The BH created from a NS-NS merger, following a metastable hypermassive NS phase, is typically surrounded by a thick torus of mass ∼ 10−3 − 0.1M⊙ (Ruffert & Janka 1999; Uryū et al. 2000; Rosswog & Liebendörfer 2003; Oechslin & Janka 2006; Chawla et al. 2010; Rezzolla et al. 2010; Hotokezaka et al.”
ELECTROMAGNETIC TRANSIENTS POWERED BY NUCLEAR DECAY IN THE TIDAL TAILS OF COALESCING COMPACT BINARIES (2011, background): “…are eventually found to be accompanied by telltale optical signatures like the supernovae of long-duration GRBs (Hjorth et al. 2003), the only definitive understanding of the progenitors will come from possible associations to direct gravitational or neutrino signals (Rosswog & Liebendörfer 2003).”
Relativistic neutron star merger simulations with non-zero temperature equations of state. I. Variation of binary parameters and equation of state (2006, background): “On the other hand, Newtonian simulations with microphysical improvements have been achieved in Ruffert et al. (1996); Rosswog et al. (1999); Ruffert & Janka (2001), and Rosswog & Liebendörfer (2003).”
Three-dimensional GRMHD Simulations of Neutrino-cooled Accretion Disks from Neutron Star Mergers (2017, methodology): “Such leakage schemes are widely used in both core-collapse supernova and compact-binary merger simulations (e.g., van Riper & Lattimer 1981; Ruffert et al. 1996; Rosswog & Liebendörfer 2003; Sekiguchi et al. 2011; Ott et al. 2013; Radice et al. 2016; Perego et al. 2016).”
AN OPEN-SOURCE NEUTRINO RADIATION HYDRODYNAMICS CODE FOR CORE-COLLAPSE SUPERNOVAE (2014, background): “Various other examples of leakage schemes used in the high-energy astrophysics community include Ruffert et al. (1996); Rosswog & Liebendörfer (2003); Sekiguchi (2010) A disadvantage of neutrino leakage schemes in their purest form is that they cannot self-consistently reproduce the neutrino…”
Short-hard gamma-ray bursts (2007, unknown): “…most numerical simulations of these systems (Ruffert et al. , 1997; Ruffert & Janka, 1998, 1999; Fryer et al. , 1999; Rosswog & Ramirez-Ruiz, 2002; Rosswog & Liebendörfer, 2003; Rosswog & Ramirez-Ruiz, 2003; Rosswog, Ramirez-Ruiz & Davies, 2003; Lee & Ramirez-Ruiz, 2002; Lee, Ramirez-Ruiz &…”
Non-Radial Instabilities and Progenitor Asphericities in Core-Collapse Supernovae (2014, methodology): “…like gray transport (Fryer, Rockefeller & Warren 2006; Scheck et al. 2006) or the light bulb and leakage schemes (Ruffert, Janka & Schaefer 1996; Rosswog & Liebendörfer 2003; Murphy & Burrows 2008; O’Connor & Ott 2011) used in many recent studies of multi-dimensional instabilities in…”
The multimessenger picture of compact object encounters: binary mergers versus dynamical collisions (2012, methodology): “Our code is an updated version of the one that was used in earlier studies (Rosswog & Davies 2002; Rosswog & Liebendörfer 2003; Rosswog, Ramirez-Ruiz & Davies 2003; Rosswog 2005).”
On the astrophysical robustness of the neutron star merger r-process (2012, methodology): “12 in Rosswog & Liebendörfer (2003) and Fig.”
NEUTRINO SIGNATURES AND THE NEUTRINO-DRIVEN WIND IN BINARY NEUTRON STAR MERGERS (2008, methodology): “…after the onset of coalescence, we find that the electron antineutrino luminosity dominates 9 over the electron neutrino luminosity, but in contrast withthe work of Ruffert et al. (1996) and Rosswog & Liebendörfer (2003), our “νµ” neutrino luminosities are at least one order of magnitude higher.”
A COMPARISON OF TWO- AND THREE-DIMENSIONAL NEUTRINO-HYDRODYNAMICS SIMULATIONS OF CORE-COLLAPSE SUPERNOVAE (2013, unknown): “Concerning heavylepton neutrinos (νx = νµ, ντ , ν̄µ, ν̄τ ), we employ a leakage scheme to include the νx cooling via pair-, photo, plasma processes (e.g., Rosswog & Liebendörfer (2003); Itoh et al. (1989)).”
GENERAL-RELATIVISTIC SIMULATIONS OF THREE-DIMENSIONAL CORE-COLLAPSE SUPERNOVAE (2012, background): “…the leakage scheme by interpolating between free emission and diffusive emission rates, χleakeff,νi = χ leak loc,νi/(1 +χ leak loc,νi/χ leak diff,νi ) , (1) where χ = Q for energy loss and χ = R for number loss (see Rosswog & Liebendörfer 2003 and O’Connor & Ott 2010 for definitions and details).”