High-resolution calculations of merging neutron stars - III. Gamma-ray bursts

By Stephan Rosswog, E. Ramirez-Ruiz, M. Davies. 2003

264 citations recorded by the source corpus.

Recent three-dimensional, high-resolution simulations of neutron star coalescences are analysed to assess whether short gamma-ray bursts (GRBs) could originate from such encounters. The two most popular modes of energy extraction - namely the annihilation of and magnetohydrodynamic processes - are explored in order to investigate their viability in launching GRBs. We find that annihilation can provide the necessary stresses to drive a highly relativistic expansion. However, unless the outflow is beamed into less than 1 per cent of the solid angle, this mechanism may fail to explain the apparent isotropized energies implied for short GRBs at cosmological distances. We argue that the energetic, neutrino-driven wind that accompanies the merger event will have enough pressure to provide adequate collimation to the -annihilation-driven jet, thereby comfortably satisfying constraints on event rate and apparent luminosity. We also assess magnetic mechanisms to transform the available energy into a GRB. If the central object does not collapse immediately into a black hole, it will be convective and it is expected to act as an effective large scale dynamo, amplifying the seed magnetic fields to a few times 1017 G within a small fraction of a second. The associated spindown time-scale is 0.2 s, coinciding with the typical duration of a short GRB. The efficiencies of the various assessed magnetic processes are high enough to produce isotropized luminosities in excess of 1052 erg s-1 even without beaming. (Less)

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/f7e7b17a7607751d982be8e84edbfda05b71083e

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Citations in the corpus

On the astrophysical robustness of the neutron star merger r-process (2012, methodology): “Our code is an updated version of the one that was used in earlier studies (Rosswog & Davies 2002; Rosswog & Liebendörfer 2003; Rosswog et al. 2003; Rosswog 2005).”
AFTERGLOW OBSERVATIONS OF FERMI LARGE AREA TELESCOPE GAMMA-RAY BURSTS AND THE EMERGING CLASS OF HYPER-ENERGETIC EVENTS (2010, background): “%) for the energy available to launch a relativistic jet (e.g., Rosswog et al. 2003; Birkl et al. 2007; Harikae et al. 2010).”
THE MILLISECOND MAGNETAR CENTRAL ENGINE IN SHORT GRBs (2015, background): “For NS-NS mergers, the traditional view is that a BH is formed promptly or with a short delay up to hundreds of milliseconds (e.g. Liu et al. 2012; Rosswog et al. 2003; Rezzolla et al. 2011).”
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).”
WHAT IS THE MOST PROMISING ELECTROMAGNETIC COUNTERPART OF A NEUTRON STAR BINARY MERGER? (2011, unknown): “…numerical simulations appears to vary by orders of magnitude (∼ 10−3 − 0.1 M⊙), depending on the properties of the binary and the high-density equation of state (Ruffert et al. 1997; Janka et al. 1999; Lee 2001; Rosswog et al. 2003; Shibata & Taniguchi 2008; Duez et al. 2010; Chawla et al. 2010).”
NEUTRINO SIGNATURES AND THE NEUTRINO-DRIVEN WIND IN BINARY NEUTRON STAR MERGERS (2008, background): “…& Janka 2007; Anderson et al. 2008b), 2) the production of short-hard GRBs (Ruffert et al. 1997; Ruffert & Janka 1999; Rosswog & Ramirez-Ruiz 2003; Rosswog et al. 2003; Rosswog 2005; Janka et al. 2006; Birkl et al. 2007), and 3) the pollution of the environment by r-process nuclei (Lattimer &…”
The long-term evolution of neutron star merger remnants – I. The impact of r-process nucleosynthesis (2013, background): “With neutrino luminosities of ∼ 1053 erg/s, neutron star merger remnants drive strong baryonic winds (Ruffert et al. 1997; Rosswog & RamirezRuiz 2002, 2003; Rosswog et al. 2003; Dessart et al. 2009), similar to new-born neutron stars (Duncan et al. 1986; Qian & Woosley 1996).”
THE FORMATION OF ECCENTRIC COMPACT BINARY INSPIRALS AND THE ROLE OF GRAVITATIONAL WAVE EMISSION IN BINARY–SINGLE STELLAR ENCOUNTERS (2013, background): “…cluster distribution around galaxies (Grindlay et al. 2006; Lee et al. 2010; Church et al. 2011) or the galactic potential (Bloom et al. 1999; Rosswog et al. 2003; Belczynski et al. 2006; Zheng & Ramirez-Ruiz 2007; Zemp et al. 2009; Fong et al. 2010; Kelley et al. 2010; Fong & Berger 2013).”
A DECADE OF SHORT-DURATION GAMMA-RAY BURST BROADBAND AFTERGLOWS: ENERGETICS, CIRCUMBURST DENSITIES, AND JET OPENING ANGLES (2015, background): “…of energy extraction to power the relativistic jet: the thermal energy release fromνν̄ annihilation in a baryonic outflow (Jaroszynski 1993; Mochkovitch et al. 1993) and magnetohydrodynamic (MHD) processes in the black hole’s accretion remnant (e.g. Blandford & Znajek 1977; Rosswog et al. 2003).”
Dynamical Mass Ejection from Binary Neutron Star Mergers (2016, methodology): “It follows very closely the method used in Ruffert et al. (1996), with the additional simplification that we use the local thermodynamical equilibrium chemical potential for the neutrinos while computing opacities as done in Rosswog et al. (2003).”
THE AFTERGLOWS OF SWIFT-ERA GAMMA-RAY BURSTS. II. TYPE I GRB VERSUS TYPE II GRB OPTICAL AFTERGLOWS (2008, methodology): “The viability of both neutron star-neutron star and neutron star-black hole mergers to create Type I GRBs has been shown in numerical simulations (e.g., Rosswog et al. 2003; Aloy et al. 2005; Rosswog 2005; Oechslin & Janka 2006).”