Relation between the neutrino flux from Centaurus A and the associated diffuse neutrino flux

Koers, Hylke; Tinyakov, P.

doi:10.1103/physrevd.78.083009

Cited by 26 publications

(54 citation statements)

References 34 publications

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“…In this study we consider the model proposed by Koers & Tinyakov (2008) and the model proposed by Becker & Biermann (2009). In both models, pγ interaction is the dominant source process, and follows the standard picture of flavour distribution at observation as outlined above.…”

Section: High-energy Neutrino Production Modelsmentioning

confidence: 99%

“…However, these breaks are close in energy, and the model therefore assumes a single break energy. This energy is determined through the γ-ray break energy, E γ,br " 200 MeV for Cen A (see Koers & Tinyakov 2008, and references therein), such that E CR,br " 3ˆ10 8 E γ,br . The all-flavour neutrino flux from Cen A, Φ CenA ν all , using the UHECR proton flux Φ CenA p as a normalization, can then be expressed by…”

Section: The Koers and Tinyakov (Kt) Modelmentioning

confidence: 99%

“…Whereas neutrinos escape unhindered, the neutrons will decay to CR protons, which would be observable. Koers & Tinyakov (2008) use data from the PAO to estimate the ultra high energy cosmic ray (UHECR) flux from Cen A, and diffuse UHECR flux, above the threshold energy of PAO, E CR,th " 5.7ˆ10 19 eV. Due to the common production path of CR protons and neutrinos, and that the emission from Cen A is assumed representative for all sources, the UHECR flux is used to scale the neutrino flux.…”

Section: The Koers and Tinyakov (Kt) Modelmentioning

confidence: 99%

“…The model by Koers & Tinyakov (2008) studies the relation between diffuse and point-source neutrino emission, and uses the RG nearest to us, Cen A, as a typical source for neutrino production ( Fig. 2).…”

Section: The Koers and Tinyakov (Kt) Modelmentioning

confidence: 99%

“…Various scenarios for high-energy neutrino production in AGN jets have been proposed (see e.g. Mannheim 1995;Mücke et al 1999;Atoyan & Dermer 2003;Koers & Tinyakov 2008;Becker & Biermann 2009). The basic mechanism can be understood as follows.…”

Section: Introductionmentioning

confidence: 99%

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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: High-energy Neutrino Production Modelsmentioning

confidence: 99%

Section: The Koers and Tinyakov (Kt) Modelmentioning

confidence: 99%

Section: The Koers and Tinyakov (Kt) Modelmentioning

confidence: 99%

Section: The Koers and Tinyakov (Kt) Modelmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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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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Energy-independent new physics in the flavour ratios of high-energy astrophysical neutrinos

Bustamante

Gago

Peña-Garay

2010

J. High Energ. Phys.

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We have studied the consequences of breaking the CPT symmetry in the neutrino sector, using the expected high-energy neutrino flux from distant cosmological sources such as active galaxies. For this purpose we have assumed three different hypotheses for the neutrino production model, characterised by the flavour fluxes at production φ 0 e : φ 0 µ : φ 0 τ = 1 : 2 : 0, 0 : 1 : 0, and 1 : 0 : 0, and studied the theoretical and experimental expectations for the muon-neutrino flux at Earth, φ µ , and for the flavour ratios at Earth, R = φ µ /φ e and S = φ τ /φ µ . CPT violation (CPTV) has been implemented by adding an energy-independent term to the standard neutrino oscillation Hamiltonian. This introduces three new mixing angles, two new eigenvalues and three new phases, all of which have currently unknown values. We have varied the new mixing angles and eigenvalues within certain bounds, together with the parameters associated to pure standard oscillations. Our results indicate that, for the models 1 : 2 : 0 and 0 : 1 : 0, it might possible to find large deviations for φ µ , R, and S between the cases without and with CPTV, provided the CPTV eigenvalues lie within 10 −29 − 10 −27 GeV, or above. Moreover, if CPTV exists, there are certain values of R and S that can be accounted for by up to three production models. If no CPTV were observed, we could set limits on the CPTV eigenvalues of the same order. Detection prospects calculated using IceCube suggest that for the models 1 : 2 : 0 and 0 : 1 : 0, the modifications due to CPTV are larger and more clearly separable from the standard-oscillations predictions. We conclude that IceCube is potentially able to detect CPTV but that, depending on the values of the CPTV parameters, there could be a mis-determination of the neutrino production model.

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Neutrinos from active black holes, sources of ultra high energy cosmic rays

Becker

Biermann

2009

Astroparticle Physics

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a b s t r a c tA correlation between the highest energy cosmic rays (above $60 EeV) and the distribution of active galactic nuclei (AGN) gives rise to a prediction of neutrino production in the same sources. In this paper, we present a detailed AGN model, predicting neutrino production near the foot of the jet, where the photon fields from the disk and synchrotron radiation from the jet itself create high optical depths for proton-photon interactions. The protons escape from later shocks where the emission region is optically thin for proton-photon interactions. Consequently, cosmic rays are predicted to come from FR-I galaxies, independent of the orientation of the source. Neutrinos, on the other hand, are only observable from sources directing their jet towards Earth, i.e. flat spectrum radio sources and in particular BL Lac type objects, due to the strongly boosted neutrino emission.

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Relation between the neutrino flux from Centaurus A and the associated diffuse neutrino flux

Cited by 26 publications

References 34 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

Energy-independent new physics in the flavour ratios of high-energy astrophysical neutrinos

Neutrinos from active black holes, sources of ultra high energy cosmic rays

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