Monte Carlo simulations of photohadronic processes in astrophysics

Mücke, A.; Engel, R.; Rachen, J. P.; Protheroe, R. J.; Stanev, T.

doi:10.1016/s0010-4655(99)00446-4

Cited by 409 publications

(449 citation statements)

References 49 publications

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“…The path of propagation is calculated step by step by integrating the Lorentz equations and computing particle interactions. Pair production is approximated as a continuous energy loss and pion production by using SOPHIA 5 , which is a Monte Carlo event generator designed to study this process (Mucke et al 2000). In the propagation of UHECRs, we assumed the computational volume to be periodic.…”

Section: Cr Propagationmentioning

confidence: 99%

Propagation of ultrahigh energy cosmic rays in extragalactic magnetic fields: a view from cosmological simulations

Hackstein¹,

Vazza²,

Brüggen³

et al. 2016

Mon. Not. R. Astron. Soc.

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We use the CRPropa code to simulate the propagation of ultra high energy cosmic rays (with energy 10 18 eV and pure proton composition) through extragalactic magnetic fields that have been simulated with the cosmological ENZO code. We test both primordial and astrophysical magnetogenesis scenarios in order to investigate the impact of different magnetic field strengths in clusters, filaments and voids on the deflection of cosmic rays propagating across cosmological distances. We also study the effect of different source distributions of cosmic rays around simulated Milky-Way like observers. Our analysis shows that the arrival spectra and anisotropy of events are rather insensitive to the distribution of extragalactic magnetic fields, while they are more affected by the clustering of sources within a ∼ 50 Mpc distance to observers. Finally, we find that in order to reproduce the observed degree of isotropy of cosmic rays at ∼ EeV energies, the average magnetic fields in cosmic voids must be ∼ 0.1 nG, providing limits on the strength of primordial seed fields.

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Section: Cr Propagationmentioning

confidence: 99%

Propagation of ultrahigh energy cosmic rays in extragalactic magnetic fields: a view from cosmological simulations

Hackstein¹,

Vazza²,

Brüggen³

et al. 2016

Mon. Not. R. Astron. Soc.

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“…We also assume that the participating nucleon is removed from the nucleus and regard this as a contribution to one-nucleon losses. The nucleon-photon interaction rates can be determined using the Monte Carle package SOPHIA [26]. We refer to the Appendices of Refs.…”

Section: Propagation Of Cosmic Ray 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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“…While our simple, analytic method allows for a more transparent look at the effects of source evolution, it does not fully encompass the particle physics involved, particularly the low and high-energy tails of the distributions of particle decays (which affect the low-and high-energy ends of the neutrino spectrum). We utilize the publicly-available simulation package CRPropa [80], which uses the SOPHIA [81] code to handle particle processes, for this purpose. We have made use of the analytical estimate described above and an extensive comparison to previous results presented in the literature (with similar parameters), to verify the results.…”

Section: Implications For Cosmogenic Neutrinosmentioning

confidence: 99%

Enhanced cosmological GRB rates and implications for cosmogenic neutrinos

Yüksel

Kistler

2007

Phys. Rev. D

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Gamma-ray bursts, which are among the most violent events in the Universe, are one of the few viable candidates to produce ultra high-energy cosmic rays. Recently, observations have revealed that GRBs generally originate from metal-poor, low-luminosity galaxies and do not directly trace cosmic star formation, as might have been assumed from their association with core-collapse supernovae. Several implications follow from these findings. The redshift distribution of observed GRBs is expected to peak at higher redshift (compared to cosmic star formation), which is supported by the mean redshift of the Swift GRB sample, hzi 3. If GRBs are, in fact, the source of the observed UHECR, then cosmic-ray production would evolve with redshift in a stronger fashion than has been previously suggested. This necessarily leads, through the GZK process, to an enhancement in the flux of cosmogenic neutrinos, providing a near-term approach for testing the gamma-ray burst-cosmic-ray connection with ongoing and proposed UHE neutrino experiments.

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Monte Carlo simulations of photohadronic processes in astrophysics

Cited by 409 publications

References 49 publications

Propagation of ultrahigh energy cosmic rays in extragalactic magnetic fields: a view from cosmological simulations

Propagation of ultrahigh energy cosmic rays in extragalactic magnetic fields: a view from cosmological simulations

Cosmogenic gamma rays and the composition of cosmic rays

Enhanced cosmological GRB rates and implications for cosmogenic neutrinos

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