Gamma-ray burst jet propagation, development of angular structure, and the luminosity function

Salafia, O. S.; Barbieri, C.; Ascenzi, S.; Toffano, Mattia

doi:10.1051/0004-6361/201936335

Cited by 64 publications

(53 citation statements)

References 104 publications

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“…and the post-merger environment, including the jet launching time with respect to merger, a growing effort is devoted to model the breakout and propagation of collimated relativistic outflows following BNS mergers. Such an effort, strongly boosted by the observation of GRB 170817A, includes semi-analytical models (e.g., Salafia et al 2020;Lazzati et al 2020;Hamidani & Ioka 2021 and refs. therein) as well as two-or threedimensional (magneto)hydrodynamic simulations in the framework of special or general relativity (e.g., Nagakura et al 2014; Lazzati et al 2018;Xie et al 2018;Kathirgamaraju et al 2019;Geng et al 2019;Nathanail et al 2020;Murguia-Berthier et al 2021;Urrutia et al 2021;Nathanail et al 2021;Gottlieb et al 2021 and refs.…”

Section: Introductionmentioning

confidence: 99%

Short gamma-ray burst jet propagation in binary neutron star merger environments

Pavan

Ciolfi

Kalinani

et al. 2021

Monthly Notices of the Royal Astronomical Society

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The multimessenger event GW170817/GRB 170817A confirmed that binary neutron star (BNS) mergers can produce short gamma-ray burst (SGRB) jets. This evidence promoted new investigations on the mechanisms through which a BNS merger remnant can launch such a powerful relativistic outflow and on the propagation of the latter across the surrounding post-merger environment. In particular, great strides have been made in jet propagation models, establishing connections between the initial jet launching conditions, including the incipient jet launching time (with respect to merger) and the injection parameters, and the observable SGRB prompt and afterglow emission. However, present semi-analytical models and numerical simulations (with one notable exception) adopt simple hand-made prescriptions to account for the post-merger environment, lacking a direct association with any specific merging BNS system. Here, we present the first three-dimensional relativistic hydrodynamics simulations of incipient SGRB jets propagating through a post-merger environment that is directly imported from the outcome of a previous general relativistic BNS merger simulation. Our results show that the evolution and final properties of the jet can be largely affected by the anisotropies and the deviations from axisymmetry and homologous expansion characterizing more realistic BNS merger environments. In addition, we find that the inclusion of the gravitational pull from the central compact object, often overlooked, can have a major impact. Finally, we consider different jet launching times referred to the same BNS merger model and discuss the consequences for the ultimate jet properties.

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Section: Introductionmentioning

confidence: 99%

Short gamma-ray burst jet propagation in binary neutron star merger environments

Pavan

Ciolfi

Kalinani

et al. 2021

Monthly Notices of the Royal Astronomical Society

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“…As jets propagate out of the central engine of the sGRB, they interact with ejecta made of material launched dynamically during the compact binary merger as well as ejecta driven by the neutrinos released from the neutron star or the accretion disk formed post-merger. The sGRB jet propagation and ejecta interaction (possibly also determining their angular structure) has been studied numerically in numerous works (Aloy et al 2005;Nagakura et al 2014;Just et al 2016;Lazzati et al 2017;Xie et al 2018;Geng et al 2019;Gill et al 2019a, Kathirgamaraju et al 2019Salafia et al 2020). Such studies are inherently complex, as the relativistic nature of the outflow naturally leads to a large range of temporal and spatial scales.…”

Section: Introductionmentioning

confidence: 99%

Ready, Set, Launch: Time Interval between a Binary Neutron Star Merger and Short Gamma-Ray Burst Jet Formation

Beniamini

Duran

Πετροπούλου

et al. 2020

ApJL

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The joint detection of GW170817/GRB 170817 confirmed the long-standing theory that binary neutron star mergers produce short gamma-ray burst (sGRB) jets that can successfully break out of the surrounding ejecta. At the same time, the association with a kilonova provided unprecedented information regarding the physical properties (such as masses and velocities) of the different ejecta constituents. Combining this knowledge with the observed luminosities and durations of cosmological sGRBs detected by the Burst Alert Telescope onboard the Neil Gehrels Swift Observatory, we revisit the breakout conditions of sGRB jets. Assuming self-collimation of sGRB jets does not play a critical role, we find that the time interval between the binary merger and the launch of a typical sGRB jet is 0.1 s. We also show that for a fraction of at least~30% of sGRBs, the usually adopted assumption of static ejecta is inconsistent with observations, even if the polar ejecta mass is an order of magnitude smaller than that in GRB 170817. Our results disfavor magnetar central engines for powering cosmological sGRBs, limit the amount of energy deposited in the cocoon prior to breakout, and suggest that the observed delay of ∼1.7s in GW170817/GRB 170817 between the gravitational wave and gamma-ray signals is likely dominated by the propagation time of the jet to the gamma-ray production site.Unified Astronomy Thesaurus concepts: Gamma-ray bursts (629); Relativistic jets (1390); Neutron stars (1108); Gravitational wave sources (677); Astrophysical black holes (98)

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“…The potential dependence of LGRB progenitors properties on metallicity could very well lead not only to an evolution of the stellar efficiency to produce LGRB, η(z), but also to an evolution of the LGRB properties. For instance, cosmic evolution of the isotropic equivalent luminosity may be expected if the beaming angle evolves (Lloyd-Ronning et al 2020;Salafia et al 2020) since the beaming depends on properties of the progenitor, such as the stellar density profile, which are in turn affected by metallicity. Therefore, the reality may be an intermediary case where both the rate and the luminosity of LGRBs evolve with cosmic time.…”

Section: Cosmic Evolution Of Lgrbs: Rate or Luminosity?mentioning

confidence: 99%

Constraining the intrinsic population of long gamma-ray bursts: Implications for spectral correlations, cosmic evolution, and their use as tracers of star formation

Palmerio

Daigne

2021

A&A

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Aims. Long gamma-ray bursts (LGRBs) have been shown to be powerful probes of the Universe, in particular for studying the star formation rate up to very high redshift (z ∼ 9). Since LGRBs are produced by only a small fraction of massive stars, it is paramount to have a good understanding of their underlying intrinsic population in order to use them as cosmological probes without introducing any unwanted bias. The goal of this work is to constrain and characterise this intrinsic population. Methods. We developed a Monte Carlo model where each burst is described by its redshift and its properties at the peak of the light curve. We derived the best fit parameters by comparing our synthetic populations to carefully selected observational constraints based on the CGRO/BATSE, Fermi/GBM and Swift/BAT samples with appropriate flux thresholds. We explored different scenarios in terms of the cosmic evolution of the luminosity function and/or of the redshift distribution as well as including or not the presence of intrinsic spectral-energetics (Ep − L) correlations. Results. We find that the existence of an intrinsic Ep − L correlation is preferred but with a shallower slope than observed (αA ∼ 0.3) and a larger scatter (∼0.4 dex). We find a strong degeneracy between the cosmic evolution of the luminosity and of the LGRB rate, and show that a sample both larger and deeper than SHOALS by a factor of three is needed to lift this degeneracy. Conclusions. The observed Ep − L correlation cannot be explained only by selection effects although these do play a role in shaping the observed relation. The degeneracy between the cosmic evolution of the luminosity function and of the redshift distribution of LGRBs should be included in the uncertainties of star formation rate estimates; these amount to a factor of 10 at z = 6 and up to a factor of 50 at z = 9.

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Gamma-ray burst jet propagation, development of angular structure, and the luminosity function

Cited by 64 publications

References 104 publications

Short gamma-ray burst jet propagation in binary neutron star merger environments

Short gamma-ray burst jet propagation in binary neutron star merger environments

Ready, Set, Launch: Time Interval between a Binary Neutron Star Merger and Short Gamma-Ray Burst Jet Formation

Constraining the intrinsic population of long gamma-ray bursts: Implications for spectral correlations, cosmic evolution, and their use as tracers of star formation

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