On the Neutrino Flux from Gamma-Ray Bursts

Guetta, Dafne; Spada, M.; Waxman, Eli

doi:10.1007/10853853_72

Cited by 4 publications

(4 citation statements)

References 18 publications

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“…Since the one-zone model is not realistic in the in-ternal shock picture, R C and Γ should evolve even within one GRB. The R C -dependence of neutrino production efficiency has been discussed in the internal shock model [12,18,25,36], but its integrated effects have not been studied in detail. Hence, it is conceivable that not all collisions occur at the same radius, which has significant consequences for the neutrino and cosmic-ray production, as we show in this work.…”

Section: Arxiv:14092874v2 [Astro-phhe] 14 Oct 2015mentioning

confidence: 99%

Neutrino and cosmic-ray emission from multiple internal shocks in gamma-ray bursts

et al. 2015

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Gamma-ray bursts (GRBs) are short-lived, luminous explosions at cosmological distances, thought to originate from relativistic jets launched at the deaths of massive stars. They are among the prime candidates to produce the observed cosmic rays at the highest energies. Recent neutrino data have, however, started to constrain this possibility in the simplest models with only one emission zone. In the classical theory of GRBs, it is expected that particles are accelerated at mildly relativistic shocks generated by the collisions of material ejected from a central engine. Here we consider neutrino and cosmic-ray emission from multiple emission regions since these internal collisions must occur at very different radii, from below the photosphere all the way out to the circumburst medium, as a consequence of the efficient dissipation of kinetic energy. We demonstrate that the different messengers originate from different collision radii, which means that multi-messenger observations open windows for revealing the evolving GRB outflows.

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Section: Arxiv:14092874v2 [Astro-phhe] 14 Oct 2015mentioning

confidence: 99%

Neutrino and cosmic-ray emission from multiple internal shocks in gamma-ray bursts

et al. 2015

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“…It appears that GRBs and GRB afterglows can be adequately described by synchrotron emission of relativistic shocks (eg. Waxman 1997, Sari et al 1997, Guetta et al 2000. These phenomenological models describe the shock by a set of adjustable parameters.…”

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confidence: 99%

Gamma-Ray Burst Phenomenology, Shock Dynamo, and the First Magnetic Fields

Gruzinov

2001

The Astrophysical Journal

157

155

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A relativistic collisionless shock propagating into an unmagnetized medium leaves behind a strong large-scale magnetic field. This seems to follow from two assumptions: (i) GRB afterglows are explained by synchrotron emission of a relativistic shock, (ii) magnetic field can't exist on microscopic scales only, it would decay by phase space mixing. Assumption (i) is generally accepted because of an apparent success of the shock synchrotron phenomenological model of GRB afterglow. Assumption (ii) is confirmed in this work by a low-dimensional numerical simulation. One may hypothesize that relativistic shock velocities are not essential for the magnetic field generation, and that all collisionless shocks propagating into an unmagnetized medium generate strong largescale magnetic fields. If this hypothesis is true, the first cosmical magnetic fields could have been generated in shocks of the first virialized objects.Subject headings: magnetic fields -shock waves 1. GRB Afterglow Phenomenology

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“…In a GRB, HENs and gamma-rays are expected to be produced due to the variability of the central engine's activity, that results in fluctuations of the relativistic outflow, creating internal shocks in the ejecta (e.g. [71,72,32,73]). These internal shocks accelerate electrons and protons in the outflow through the process of Fermi acceleration.…”

Section: High-energy Neutrino Productionmentioning

confidence: 99%

Bounding the time delay between high-energy neutrinos and gravitational-wave transients from gamma-ray bursts

Baret

Bartos

Bouhou

et al. 2011

Astroparticle Physics

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We derive a conservative coincidence time window for joint searches of gravitational-wave (GW) transients and high-energy neutrinos (HENs, with energies 100GeV), emitted by gamma-ray bursts (GRBs). The last are among the most interesting astrophysical sources for coincident detections with current and near-future detectors. We take into account a broad range of emission mechanisms. We take the upper limit of GRB durations as the 95% quantile of the T 90 's of GRBs observed by BATSE, obtaining a GRB duration upper limit of ∼ 150s. Using published results on high-energy (> 100MeV) photon light curves for 8 GRBs detected by Fermi LAT, we verify that most highenergy photons are expected to be observed within the first ∼ 150s of the * Corresponding author. Email: ibartos@phys.columbia.edu GRB. Taking into account the breakout-time of the relativistic jet produced by the central engine, we allow GW and HEN emission to begin up to 100s before the onset of observable gamma photon production. Using published precursor time differences, we calculate a time upper bound for precursor activity, obtaining that 95% of precursors occur within ∼ 250s prior to the onset of the GRB. Taking the above different processes into account, we arrive at a time window of t HEN − t GW ∈ [−500s, +500s]. Considering the above processes, an upper bound can also be determined for the expected time window of GW and/or HEN signals coincident with a detected GRB, t GW − t GRB ≈ t HEN − t GRB ∈ [−350s, +150s].

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On the Neutrino Flux from Gamma-Ray Bursts

Cited by 4 publications

References 18 publications

Neutrino and cosmic-ray emission from multiple internal shocks in gamma-ray bursts

Neutrino and cosmic-ray emission from multiple internal shocks in gamma-ray bursts

Gamma-Ray Burst Phenomenology, Shock Dynamo, and the First Magnetic Fields

Bounding the time delay between high-energy neutrinos and gravitational-wave transients from gamma-ray bursts

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