Photohadronic neutrinos from transients in astrophysical sources

Rachen, J. P.; Mészáros, P.

doi:10.1103/physrevd.58.123005

Cited by 340 publications

(388 citation statements)

References 66 publications

(124 reference statements)

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“…ity relation for blazars, which affects in the luminosity scaling of the resultant neutrino spectra. Extreme blazars can have Γ ą 20 (Marscher 2009), but ă 30 (Rachen & Mészáros 1998) thus future studies would do well in exploring the effects of varying Lorentz bulk factors of AGN jets on the resultant neutrino emission.…”

Section: Discussionmentioning

confidence: 99%

High-energy neutrino fluxes from AGN populations inferred from X-ray surveys

Jacobsen

et al. 2015

Mon. Not. R. Astron. Soc.

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High-energy neutrinos and photons are complementary messengers, probing violent astrophysical processes and structural evolution of the Universe. X-ray and neutrino observations jointly constrain conditions in active galactic nuclei (AGN) jets: their baryonic and leptonic contents, and particle production efficiency. Testing two standard neutrino production models for local source Cen A (Koers & Tinyakov 2008; Becker & Biermann 2009), we calculate the high-energy neutrino spectra of single AGN sources and derive the flux of high-energy neutrinos expected for the current epoch. Assuming that accretion determines both X-rays and particle creation, our parametric scaling relations predict neutrino yield in various AGN classes. We derive redshift-dependent number densities of each class, from Chandra and Swift/BAT X-ray luminosity functions (Silverman et al. 2008;Ajello et al. 2009). We integrate the neutrino spectrum expected from the cumulative history of AGN (correcting for cosmological and source effects, e.g. jet orientation and beaming). Both emission scenarios yield neutrino fluxes well above limits set by IceCube (by " 4-10 6ˆa t 1 PeV, depending on the assumed jet models for neutrino production). This implies that: (i) Cen A might not be a typical neutrino source as commonly assumed; (ii) both neutrino production models overestimate the efficiency; (iii) neutrino luminosity scales with accretion power differently among AGN classes and hence does not follow X-ray luminosity universally; (iv) some AGN are neutrino-quiet (e.g. below a power threshold for neutrino production); (v) neutrino and X-ray emission have different duty cycles (e.g. jets alternate between baryonic and leptonic flows); or (vi) some combination of the above.

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Section: Discussionmentioning

confidence: 99%

High-energy neutrino fluxes from AGN populations inferred from X-ray surveys

Jacobsen

et al. 2015

Mon. Not. R. Astron. Soc.

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“…For cosmic neutrinos with an E −2 energy spectrum an integral flux limit of E 2 φ ≤ 3.6 × 10 −8 GeV cm −2 sec −1 sr −1 has been found in the energy interval of 2 × 10 6 − 6.3 × 10 9 GeV [30]. In particular the non-detection of neutrinos from GRBs [32] has placed a tighter upper bound which is 3.7 times below the theoretical predictions [7,8,11,26] combining 40 and 59 strings. IceCube collaboration has concluded [32] that GRBs are not the only sources of cosmic rays above energy 1 EeV or the efficiency of neutrino production is much lower than the current predictions.…”

Section: Introductionmentioning

confidence: 99%

“…Shock accelerated protons may loose energy by synchrotron cooling and pγ interaction inside the source depending on the magnetic field and low energy photon density respectively. The high energy neutrino flux produced in pγ interactions have been calculated in detail in many earlier papers [6,7,8,9,10,11,12,13,14,15,16,17]. It has been noted earlier that pp interactions are only important for photospheric radii of GRB fireballs [18,19].…”

Section: Introductionmentioning

confidence: 99%

Neutrinos from decaying muons, pions, neutrons and kaons in gamma ray bursts

Moharana¹,

Gupta²

2012

Astroparticle Physics

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In the internal shock model of gamma ray bursts ultrahigh energy muons, pions, neutrons and kaons are likely to be produced in the interactions of shock accelerated relativistic protons with low energy photons (KeV-MeV). These particles subsequently decay to high energy neutrinos/antineutrinos and other secondaries. In the high internal magnetic fields of gamma ray bursts, the ultrahigh energy charged particles (µ + , π + , K + ) lose energy significantly due to synchrotron radiations before decaying into secondary high energy neutrinos and antineutrinos. The relativistic neutrons decay to high energy antineutrinos, protons and electrons. We have calculated the total neutrino flux (neutrino and antineutrino) considering the decay channels of ultrahigh energy muons, pions, neutrons and kaons. We have shown that the total neutrino flux generated in neutron decay can be higher than that produced in µ + and π + decay. The charged kaons being heavier than pions, lose energy slowly and their secondary total neutrino flux is more than that from muons and pions at very high energy. Our detailed calculations on secondary particle production in pγ interactions give the total neutrino fluxes and their flavour ratios expected on earth. Depending on the values of the parameters (luminosity, Lorentz factor, variability time, spectral indices and break energy in the photon spectrum) of a gamma ray burst the contributions to the total neutrino flux from the decay of different particles (muon, pion, neutron and kaon) may vary and they would also be reflected on the neutrino flavour ratios.

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“…Assuming that GRBs generate the observed UHECRs, the expected GRB muon and anti-muon neutrino flux may be estimated using Eq. (10) [100,101], This neutrino spectrum extends to ∼ 10 16 eV, and is suppressed at higher energy due to energy loss of pions and muons [84,100,101] (for the contribution of Kaon decay at high energy see [19]). Eq.…”

Section: Tev Fireball Neutrinosmentioning

confidence: 99%

High Energy Cosmic Ray and Neutrino Astronomy

Waxman

2011

Integrated Science &Amp; Technology Program

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Cosmic-rays with energies exceeding 10 19 eV are referred to as Ultra High Energy Cosmic Rays (UHECRs). The sources of these particles and their acceleration mechanism are unknown, and for many years have been the issue of much debate. The first part of this review describes the main constraints, that are implied by UHECR observations on the properties of candidate UHECR sources, the candidate sources, and the related main open questions. In order to address the challenges of identifying the UHECR sources and of probing the physical mechanisms driving them, a "multi-messenger" approach will most likely be required, combining electromagnetic, cosmic-ray and neutrino observations. The second part of the review is devoted to a discussion of high energy neutrino astronomy. It is shown that detectors, which are currently under construction, are expected to reach the effective mass required for the detection of high energy extra-Galactic neutrino sources, and may therefore play a key role in the near future in resolving the main open questions. The detection of high energy neutrinos from extra-Galactic sources will not only provide constraints on the identity and underlying physics of UHECR sources, but may furthermore provide information on fundamental neutrino properties.

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Photohadronic neutrinos from transients in astrophysical sources

Cited by 340 publications

References 66 publications

High-energy neutrino fluxes from AGN populations inferred from X-ray surveys

High-energy neutrino fluxes from AGN populations inferred from X-ray surveys

Neutrinos from decaying muons, pions, neutrons and kaons in gamma ray bursts

High Energy Cosmic Ray and Neutrino Astronomy

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