Neutrino signal dependence on   gamma-ray burst emission mechanism

Pitik, Tetyana; Tamborra, Irene; Πετροπούλου, Μαρία

doi:10.1088/1475-7516/2021/05/034

Cited by 32 publications

(27 citation statements)

References 162 publications

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“…However, association studies of blazars hint toward no excess from the broader population (Aartsen et al 2017). Various other source classes have been proposed as factories of the observed cosmic neutrino flux (Mészáros 2017a;Ahlers & Halzen 2018;Vitagliano et al 2020), such as gamma-ray bursts, cluster of galaxies, star-forming galaxies, and tidal disruption events (TDEs; Tamborra et al 2014;Zandanel et al 2015;Wang & Liu 2016;Mészáros 2017b;Dai & Fang 2017;Lunardini & Winter 2017;Murase 2017;Senno et al 2017;Waxman 2017;Pitik et al 2021). Nevertheless, the neutrino emission from each of these source classes cannot fully account for the observed neutrino flux.…”

Section: Introductionmentioning

confidence: 99%

Is the High-energy Neutrino Event IceCube-200530A Associated with a Hydrogen-rich Superluminous Supernova?

Pitik

Tamborra

Angus

et al. 2022

ApJ

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The Zwicky Transient Facility follow-up campaign of alerts released by the IceCube Neutrino Observatory has led to the likely identification of the transient AT2019fdr as the source of the neutrino event IC200530A. AT2019fdr was initially suggested to be a tidal disruption event in a Narrow-Line Seyfert 1 galaxy. However, the combination of its spectral properties, color evolution, and feature-rich light curve suggests that AT2019fdr may be a Type IIn superluminous supernova. In the latter scenario, IC200530A may have been produced via inelastic proton-proton collisions between the relativistic protons accelerated at the forward shock and the cold protons of the circumstellar medium. Here, we investigate this possibility and find that at most 4.6 × 10−2 muon neutrino and antineutrino events are expected to be detected by the IceCube Neutrino Observatory within 394 days of discovery in the case of excellent discrimination of the atmospheric background. After correcting for the Eddington bias, which occurs when a single cosmic neutrino event is adopted to infer the neutrino emission at the source, we conclude that IC200530A may originate from the hydrogen-rich superluminous supernova AT2019fdr.

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Section: Introductionmentioning

confidence: 99%

Is the High-energy Neutrino Event IceCube-200530A Associated with a Hydrogen-rich Superluminous Supernova?

Pitik

Tamborra

Angus

et al. 2022

ApJ

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“…In Fig. 10 we also show the predicted neutrino spectra shown in Pitik et al (2021), who computed the neutrino production for a benchmark high-luminosity GRB, among others in the internal shock model , in the internal shock model with dissipative photosphere (IS+PH, Toma et al 2011) and in the proton synchrotron marginally fast cooling model (PSYN, Florou et al 2021;Pitik et al 2021). Because these models were computed for a GRB with a different 𝛾-ray fluence than ours, we appropriately rescaled the neutrino fluence spectra of Pitik et al (2021) for a fair comparison to our results.…”

Section: The Total Neutrino Fluencementioning

confidence: 95%

Hadronic supercriticality in spherically expanding sources: application to GRB prompt emission

Florou¹,

Mastichiadis²,

Πετροπούλου³

2022

Preprint

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Relativistic hadronic plasmas can become under certain conditions supercritical, abruptly and efficiently releasing the energy stored in protons through photon outbursts. Past studies have tried to relate the features of such hadronic supercriticalities (HSC) to the phenomenology of Gamma-Ray Burst (GRB) prompt emission. In this work we investigate, for the first time, HSC in adiabatically expanding sources. We examine the conditions required to trigger HSC, study the role of expansion velocity, and discuss our results in relation to GRB prompt emission. We find multi-pulse light curves from slowly expanding regions (𝑢 exp 0.01𝑐) that are a manifestation of the natural HSC quasi-periodicity, while single-pulse light curves with a fast rise and slow decay are found for higher velocities. The formation of the photon spectrum is governed by an in-source electromagnetic cascade. The peak photon energy is ∼ 1 MeV (∼ 1 GeV) for maximum proton energies ∼ 1 − 10 PeV (1 − 10 EeV) assuming a jet Lorentz factor 100. Peak 𝛾-ray luminosities are in the range 10 49 − 10 52 erg s −1 , with the MeV-peaked spectra being ∼ 100 − 300 times more luminous than their GeV-peaked analogues. HSC bursts peaking in the MeV are also copious ∼ 10 TeV neutrino emitters, with an all-flavour fluence ∼ 10% of the 𝛾-ray one. The hypothesis that typical long-duration GRBs are powered by HSC could be tested in the near future with more sensitive neutrino telescopes like IceCube-Gen2.

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“…We comment further on the relevant cooling times in the discussion section. The model can be further constrained by the tight constraints from the IceCube (Aartsen et al 2017) and Antares (Albert et al 2017) experiments, as shown by Florou et al (2021) and Pitik et al (2021).…”

Section: Constraining Proton Synchrotron Emission Models By Bethe-hei...mentioning

confidence: 99%

Bethe-Heitler signature in proton synchrotron models for gamma-ray bursts

Bégué¹,

Samuelsson²,

Pe’er³

2021

Preprint

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We study the effect of Bethe-Heitler (BeHe) pair production on a proton synchrotron model for the prompt emission in gamma-ray bursts (GRBs). The possible parameter space of the model is constrained by consideration of the synchrotron radiation from the secondary BeHe pairs. We find two regimes of interest. 1) At high bulk Lorentz factor, large radius and low luminosity, proton synchrotron emission dominates and produces a spectrum in agreement with observations. For part of this parameter space, a subdominant (in the MeV band) power-law is created by the synchrotron emission of the BeHe pairs. This power-law extends up to few tens or hundreds of MeV. Such a signature is a natural expectation in a proton synchrotron model, and it is seen in some GRBs, including GRB 190114C recently observed by the MAGIC observatory. 2) At low bulk Lorentz factor, small radius and high luminosity, BeHe cooling dominates. The spectrum achieves the shape of a single power-law with spectral index α = −3/2 extending across the entire GBM/Swift energy window, incompatible with observations. Our theoretical results can be used to further constrain the spectral analysis of GRBs in the guise of proton synchrotron models.

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Neutrino signal dependence on gamma-ray burst emission mechanism

Cited by 32 publications

References 162 publications

Is the High-energy Neutrino Event IceCube-200530A Associated with a Hydrogen-rich Superluminous Supernova?

Is the High-energy Neutrino Event IceCube-200530A Associated with a Hydrogen-rich Superluminous Supernova?

Hadronic supercriticality in spherically expanding sources: application to GRB prompt emission

Bethe-Heitler signature in proton synchrotron models for gamma-ray bursts

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