High Energy Cosmic-Rays and Neutrinos from Cosmological Gamma-Ray Burst Fireballs

Waxman, Eli

doi:10.1238/physica.topical.085a00117

Cited by 21 publications

(15 citation statements)

References 63 publications

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“…When there are many sources the above constraint disappears, as the central limit theorem would guarantee that a featureless spectrum would be produced; this is no-tably one of the peculiarities of the γ−ray burst model of UHECR origin [27].…”

Section: For Which D(e)mentioning

confidence: 99%

Centaurus A as the source of ultrahigh-energy cosmic rays?

Isola

Lemoine²,

Sigl³

2001

Phys. Rev. D

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We present numerical simulations for energy spectra and angular distributions of nucleons above 10 19 eV injected by the radio-galaxy Centaurus A at a distance 3.4 Mpc and propagating in extragalactic magnetic fields in the sub-micro Gauss range. We show that field strengths B 0.3µG, as proposed by Farrar & Piran, cannot provide sufficient angular deflection to explain the observational data. A magnetic field of intensity B 1µG could reproduce the observed large-scale isotropy and could marginally explain the observed energy spectrum. However, it would not readily account for the E = 320 ± 93 EeV Fly's Eye event that was detected at an angle 136 o away from Cen-A. Such a strong magnetic field also saturates observational upper limits from Faraday rotation observations and X-ray bremsstrahlung emission from the ambient gas (assuming equipartition of energy). This scenario may already be tested by improving magnetic field limits with existing instruments. We also show that high energy cosmic ray experiments now under construction will be able to detect the level of anisotropy predicted by this scenario. We conclude that for magnetic fields B 0.1−0.5 µG, considered as more reasonable for the local Supercluster environment, in all likelihood at least a few sources within 10 Mpc from the Earth should contribute to the observed ultra high energy cosmic ray flux.

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Section: For Which D(e)mentioning

confidence: 99%

Centaurus A as the source of ultrahigh-energy cosmic rays?

Isola

Lemoine²,

Sigl³

2001

Phys. Rev. D

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“…It is assumed that particles undergo Fermi acceleration [58,59,86] at the forward shock. The synchrotron radiation coming from shock accelerated electrons is broadly considered to be the origin of the observed afterglow light curve [77].…”

Section: Photon Energy Distribution During the Afterglowmentioning

confidence: 99%

Multi-messenger detection prospects of gamma-ray burst afterglows with optical jumps

Guarini,

Tamborra,

Bégué

et al. 2021

Preprint

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Afterglow light curves of gamma-ray bursts (GRBs) exhibit very complex temporal and spectral features, such as a sudden intensity jump about one hour after the prompt emission in the optical band. We model this feature through the late collision of two relativistic shells and investigate the corresponding high-energy neutrino emission within a multi-messenger framework, while contrasting our findings with the ones from the classic fireball model. For a constant density circumburst medium, the total number of emitted neutrinos can increase by about an order of magnitude within a dynamical time when an optical jump occurs with respect to the self-similar afterglow scenario. By exploring the detection prospects with the IceCube Neutrino Observatory and future radio arrays such as IceCube-Gen2 radio, RNO-G and GRAND200k, as well as the POEMMA spacecraft, we conclude that the detection of neutrinos with IceCube-Gen2 radio could enable us to constrain the fraction of GRB afterglows with a jump as well as the properties of the circumburst medium. We also investigate the neutrino signal expected for the afterglows of GRB 100621A and a GRB 130427A-like burst with an optical jump. The detection of neutrinos from GRB afterglows could be crucial to explore the yet-to-be unveiled mechanism powering the optical jumps.

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“…The gamma-ray and afterglow radiation are likely to be emitted from relativistic electrons accelerated in shock waves; the same shocks should also accelerate protons. The protons then collide with gamma-ray photons to produce charged pions that decay into neutrinos (10 5 -10 10 GeV) [146,142,145]. This scenario was first investigated for the internal shock model [146,102], and it has been pointed out that a km-scale neutrino detector would observe at least several tens of events per year [145] correlated with GRBs.…”

Section: High-energy Neutrinosmentioning

confidence: 99%

Multimessenger astronomy with the Einstein Telescope

et al. 2010

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Gravitational waves (GWs) are expected to play a crucial rôle in the development of multimessenger astrophysics. The combination of GW observations with other astrophysical triggers, such as from gamma-ray and X-ray satellites, optical/radio telescopes, and neutrino detectors allows us to decipher science that would otherwise be inaccessible. In this paper, we provide a broad review from the multimessenger perspective of the science reach offered by the third generation interferometric GW detectors and by the Einstein Telescope (ET) in particular. We focus on cosmic transients, and base our estimates on the results obtained by ET's predecessors GEO, LIGO, and Virgo.[] RCS ; compiled 12

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High Energy Cosmic-Rays and Neutrinos from Cosmological Gamma-Ray Burst Fireballs

Cited by 21 publications

References 63 publications

Centaurus A as the source of ultrahigh-energy cosmic rays?

Centaurus A as the source of ultrahigh-energy cosmic rays?

Multi-messenger detection prospects of gamma-ray burst afterglows with optical jumps

Multimessenger astronomy with the Einstein Telescope

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