High energy neutrino emission and neutrino background from gamma-ray bursts in the internal shock model

By Kohta Murase, S. Nagataki. 2005

132 citations recorded by the source corpus.

High energy neutrino emission from gamma-ray bursts (GRBs) is discussed. In this paper, by using the simulation kit GEANT4, we calculate proton cooling efficiency including pion-multiplicity and proton-inelasticity in photomeson production. First, we estimate the maximum energy of accelerated protons in GRBs. Using the obtained results, neutrino flux from one burst and a diffuse neutrino background are evaluated quantitatively. We also take account of cooling processes of pion and muon, which are crucial for resulting neutrino spectra. We confirm the validity of analytic approximate treatments on GRB fiducial parameter sets, but also find that the effects of multiplicity and high-inelasticity can be important on both proton cooling and resulting spectra in some cases. Finally, assuming that the GRB rate traces the star formation rate, we obtain a diffuse neutrino background spectrum from GRBs for specific parameter sets. We introduce the nonthermal baryon-loading factor, rather than assume that GRBs are main sources of ultra-high energy cosmic rays (UHECRs). We find that the obtained neutrino background can be comparable with the prediction of Waxman and Bahcall, although our ground in estimation is different from theirs. In this paper, we study on various parameters since there are many parameters in the model. Themore » detection of high energy neutrinos from GRBs will be one of the strong evidences that protons are accelerated to very high energy in GRBs. Furthermore, the observations of a neutrino background has a possibility not only to test the internal shock model of GRBs but also to give us information about parameters in the model and whether GRBs are sources of UHECRs or not.« less

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/434be35ce1d12f07c16e2ba6200416a43e71175e

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In Astronomy and Astrophysics

1. Bing Zhang
2. Pawan Kumar
3. P. Mészáros
4. F. Ryde
5. Xuefeng Wu
6. K. Ioka
7. Kohta Murase
8. E. Berger

In Nuclear and High Energy Physics

1. Bing Zhang
2. Pawan Kumar
3. Kumiko Kotera
4. E. Orlando
5. Angela V. Olinto
6. Kohta Murase
7. F. Ryde
8. P. Mészáros

Citations in the corpus

• Detection of a Spectral Break in the Extra Hard Component of GRB 090926A (2011, background): “…that the photon field is inhomogeneous and timedependent, as will be discussed below, for which it is not so clear how the photo-hadronic interaction efficiency (as well as the neutrino production efficiency, see Murase & Nagataki (2006); Dermer et al. (2007); Razzaque (2009)) depends on Γ.”
• A Multimessenger Picture of the Flaring Blazar TXS 0506+056: Implications for High-energy Neutrino Emission and Cosmic-Ray Acceleration (2018, methodology): “For a typical synchrotron spectrum around the SED peak, the rectilinear approximation around theΔ resonance is usually valid (Murase & Nagataki 2006; Murase et al. 2014), and the characteristic proton Lorentz factor interacting with photons of the frequency hsyn synn e= is given by (Murase…”
• The physics of gamma-ray bursts & relativistic jets (2014, methodology): “the traditional internal shocks is higher than that of the high-luminosity GRBs. These GRBs give a neutrino background in the sub EeV range with a ux level comparable to that by high luminosity GRBs (Murase et al., 2006; Gupta and Zhang, 2007a). 10.2 Other neutrino emission components from GRBs GRBs”
• High-Energy Neutrinos and Cosmic Rays from Low-Luminosity Gamma-Ray Bursts? (2006, methodology): “These radii will be important for neutrino production (Murase & Nagataki 2006a).”
• Cosmogenic neutrinos: parameter space and detectabilty from PeV to ZeV (2010, background): “In optimistic source scenarios, it was calculated that the cosmogenic neutrino fluxes would be overwhelmed by the neutrinos from the acceleration site (see for example Mannheim et al., 2001 for an AGN scenario and Murase and Nagataki, 2006 for a GRB scenario).”
• Blazar Flares as an Origin of High-energy Cosmic Neutrinos? (2018, background): “…of neutrino-candidate transients is the prompt emission from γ-ray bursts (GRBs) with a typical duration of ∼ 1 − 100 s (e.g., Waxman & Bahcall 1997; Murase & Nagataki 2006; Petropoulou et al. 2014; Bustamante et al. 2015), although low-power GRBs have a longer duration of 103 − 104 s (Murase…”