Open inflation with scalar-tensor gravity

Lee, Jae-weon; Koh, Seoktae; Lee, Chul H.

doi:10.1103/physrevd.58.107302

Cited by 76 publications

(122 citation statements)

References 18 publications

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“…Motivated by the increased experimental prospects for ultra-high energy neutrino detection, in the present paper we reconsider flux predictions in the above scenarios with our recently combined propagation codes [42,46,50,51]. Our main emphasize is thereby on model independent flux ranges consistent with all present data on cosmic and γ−rays.…”

Section: Introductionmentioning

confidence: 99%

Ultrahigh-energy neutrino fluxes and their constraints

et al. 2002

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Applying our recently developed propagation code we review extragalactic neutrino fluxes above 10 14 eV in various scenarios and how they are constrained by current data. We specifically identify scenarios in which the cosmogenic neutrino flux above ≃ 10 18 eV, produced by pion production of ultra high energy cosmic rays outside their sources, is considerably higher than the "WaxmanBahcall bound". This is easy to achieve for sources with hard injection spectra and luminosities that were higher in the past. Such fluxes would significantly increase the chances to detect ultra-high energy neutrinos with experiments currently under construction or in the proposal stage.

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Section: Introductionmentioning

confidence: 99%

Ultrahigh-energy neutrino fluxes and their constraints

et al. 2002

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“…(3). Electromagnetic interactions of photons and leptons with the CRB can happen on time-scales much shorter than their production rates [29]. The driving processes of the electromagnetic cascade in the cosmic background photons are inverse Compton scattering (ICS) with CMB photons, e ± + γ bgr → e ± + γ, and pair production (PP) with CMB and CIB radiation, γ + γ bgr → e + + e − [19,30].…”

Section: Electromagnetic Cascades From Heavy Nucleimentioning

confidence: 99%

Cosmogenic gamma rays and the composition of cosmic rays

Ahlers

Salvadó

2011

Phys. Rev. D

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We discuss the prospects of detecting the sources of ultra-high energy (UHE) cosmic ray (CR) nuclei via their emission of cosmogenic γ-rays in the GeV to TeV energy range. These γ-rays result from electromagnetic cascades initiated by high energy photons, electrons and positrons that are emitted by CRs during their propagation in the cosmic radiation background and are independent of the simultaneous emission of γ-rays in the vicinity of the source. The corresponding production power by UHE CR nuclei (with mass number A and charge Z) is dominated by pion photo-production (∝ A) and Bethe-Heitler pair production (∝ Z 2 ). We show that the cosmogenic γ-ray signal from a single steady UHE CR source is typically more robust with respect to variations of the source composition and injection spectrum than the accompanying signal of cosmogenic neutrinos. We study the diffuse emission from the sum of extragalactic CR sources as well as the point source emission of the closest sources.

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“…[10] then shows that the spectrum of electron-positron pairs (heretoafter simply referred to as electrons) generated by a proton of energy E can be approximated by a power-law energy distribution dn/dE e ∝ E −7/4 e . Kinematics implies that this power law holds for E min ≤ E e ≤ E PPP , where the minimal and maximal energies are given by [6] …”

Section: Nucleon Interactionsmentioning

confidence: 99%

“…[6]. The photons and pairs are followed until either their energy drops below 100 MeV or they reach an observer.…”

Section: Secondary Electromagnetic Cascades and Neutrinosmentioning

confidence: 99%

“…To this end, we have recently merged our Monte Carlo code for simulating three dimensional propagation of UHECRs in a structured, magnetized Universe [5] with a one-dimensional transport code that solves electromagnetic (EM) cascades and neutrino propagation [6]. We discuss the limitations due to the one-dimensional approximation and implement a procedure to test the resulting uncertainty on the EM cascade on the observable fluxes.…”

Section: Introductionmentioning

confidence: 99%

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CRPropa: A numerical tool for the propagation of UHE cosmic rays, γ-rays and neutrinos

Armengaud

Sigl

Beau

et al. 2007

Astroparticle Physics

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To understand the origin of ultra-high energy cosmic rays (UHECRs, defined to be above 10 18 eV), it is required to model in a realistic way their propagation in the Universe. UHECRs can interact with low energy radio, microwave, infrared and optical photons to produce electron/positron pairs or pions. The latter decay and give rise to neutrinos and electromagnetic cascades extending down to MeV energies. In addition, deflections in cosmic magnetic fields can influence the spectrum and sky distribution of primary cosmic rays and, due to the increased propagation path length, the secondary neutrino and γ−ray fluxes. Neutrino, γ−ray, cosmic ray physics and extra-galactic magnetic fields are, therefore, strongly linked subjects and should be considered together in order to extract maximal information from existing and future data, like the one expected from the Auger Observatory. For that purpose, we have developed CRPropa, a publicly-available numerical package which takes into account interactions and deflections of primary UHECRs as well as propagation of secondary electromagnetic cascades and neutrinos. CRPropa allows to compute the observable properties of UHECRs and their secondaries in a variety of models for the sources and propagation of these particles. Here we present physical processes taken into account as well as benchmark examples; a detailed documentation of the code can be found on our web site.

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Open inflation with scalar-tensor gravity

Cited by 76 publications

References 18 publications

Ultrahigh-energy neutrino fluxes and their constraints

Ultrahigh-energy neutrino fluxes and their constraints

Cosmogenic gamma rays and the composition of cosmic rays

CRPropa: A numerical tool for the propagation of UHE cosmic rays, γ-rays and neutrinos

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