A5023268803- Astrophysics and Cosmic Phenomena
- Dark Matter and Cosmic Phenomena
- Neutrino Physics Research
- Particle physics theoretical and experimental studies
- Radio Astronomy Observations and Technology
- Gamma-ray bursts and supernovae
- Particle Accelerators and Free-Electron Lasers
- Atmospheric Ozone and Climate
- Particle Detector Development and Performance
- Photocathodes and Microchannel Plates
- Solar and Space Plasma Dynamics
- Calibration and Measurement Techniques
- Particle accelerators and beam dynamics
- Pulsars and Gravitational Waves Research
- Atmospheric aerosols and clouds
- Radiation Detection and Scintillator Technologies
- Radiation Therapy and Dosimetry
- Atomic and Subatomic Physics Research
- Astronomical Observations and Instrumentation
- Ionosphere and magnetosphere dynamics
- Radio Wave Propagation Studies
- Electromagnetic Compatibility and Measurements
- Clay minerals and soil interactions
- Lightning and Electromagnetic Phenomena
- Nuclear materials and radiation effects
Khalifa University of Science and Technology
2022-2025
Deutsches Elektronen-Synchrotron DESY
2019-2024
Radboud University Nijmegen
2015-2023
European Southern Observatory
2023
Ruhr University Bochum
2023
Goddard Space Flight Center
2023
University of Maryland, College Park
2023
The University of Adelaide
2017-2020
Universität Hamburg
2012-2019
National Institute for Subatomic Physics
2019
We present the simulation framework CRPropa version 3 designed for efficient development of astrophysical predictions ultra-high energy particles. Users can assemble modules most relevant propagation effects in galactic and extragalactic space, include their own physics with new features, receive on output primary secondary cosmic messengers including nuclei, neutrinos photons. In extension to contained a previous version, facilitates high-performance computing comprises physical features...
We have carried out a detailed study to understand the observed energy spectrum and composition of cosmic rays with energies up ~10^18 eV. Our shows that single Galactic component subsequent cut-offs in individual spectra different elements, optimised explain below ~10^14 eV knee all-particle spectrum, cannot above ~2x10^16 discuss two approaches for second -- re-acceleration at wind termination shock, supernova explosions Wolf-Rayet stars, show latter scenario can almost all features eV,...
Cosmogenic neutrinos are produced when ultra-high-energy cosmic rays (UHECRs) interact with cosmological photon fields. Limits on the diffuse flux of these can be used to constrain fraction protons arriving at Earth energies $E_{p} \gtrsim 30$ EeV, thereby providing constraints composition UHECRs without fully relying hadronic interaction models. We show which extent current neutrino telescopes already this and discuss prospects for next-generation detectors further it. Additionally, we...
We demonstrate that a population of Active Galactic Nuclei (AGN) can describe the observed spectrum ultra-high-energy cosmic rays (UHECRs) at and above ankle, dominant contribution comes from low-luminosity BL Lacs. An additional, subdominant high-luminosity AGN is needed to improve description composition observables, leading substantial neutrino flux peaks EeV energies. also find different properties for low- populations are required; possibly similar baryonic loading already be excluded...
Abstract The landscape of high- and ultra-high-energy astrophysics has changed in the last decade, largely due to inflow data collected by large-scale cosmic-ray, gamma-ray, neutrino observatories. At dawn multimessenger era, interpretation these observations within a consistent framework is important elucidate open questions this field. CRPropa 3.2 Monte Carlo code for simulating propagation high-energy particles Universe. This version represents major leap forward, significantly expanding...
In this white paper we introduce the IMAGINE Consortium and its scientific background, goals structure. Our purpose is to coordinate facilitate efforts of a diverse group researchers in broad areas interstellar medium, Galactic magnetic fields cosmic rays, our goal develop more comprehensive insights into structures roles their interactions with rays. To achieve higher level self-consistency, depth rigour can only be achieved by coordinated experts astrophysics involved observational,...
The results of simulations the extragalactic propagation ultra-high energy cosmic rays (UHECRs) have intrinsic uncertainties due to poorly known physical quantities and approximations used in codes. We quantify simulated UHECR spectrum composition different models for background light (EBL), photodisintegration setups, concerning photopion production use simulation discuss several representative source scenarios with proton, nitrogen or iron at injection. For this purpose we SimProp CRPropa,...
Radio galaxies are intensively discussed as the sources of cosmic rays observed above about $3\,{\times}\,10^{18}\,\text{eV}$, called ultra-high energy (UHECRs). We present a first, systematic approach that takes individual characteristics these into account, well impact extragalactic magnetic-field structures up to distance 120 Mpc. use mixed simulation setup, based on 3D simulations UHECRs ejected by observed, radio taken out Mpc, and 1D over continuous source distribution contributing...
Abstract Over the last decade, observations have shown that mean mass of ultra-high-energy cosmic rays (UHECRs) increases progressively toward highest energies. However, precise composition is still unknown and several theoretical studies hint at existence a subdominant proton component up to Motivated by exciting prospect performing charged-particle astronomy with (UHE) protons we quantify level UHE-proton flux compatible present multimessenger associated fluxes neutral messengers produced...
We examine the effects of a giant magnetized halo around Galaxy on angular distribution arriving ultra-high energy cosmic rays (UHECR) observed at Earth. investigate three injection scenarios for UHECRs, and track them through isotropic turbulent magnetic fields varying strengths in Galactic halo. calculate resultant dipole quadrupole amplitudes UHECRs detected by an observer plane region. find that, regardless scenario considered, when scattering length particles is comparable to size halo,...
We discuss the possibility that PeV neutrinos recently observed by IceCube are produced interactions of extragalactic cosmic rays during their propagation through radiation backgrounds. show fluxes resulting from decays neutrons in ray protons with CMB background suppressed (Eν2dΦν/dE < 10−10 GeV/cm2 s sr), those pions UV/optical/IR backgrounds being dominant ones at energies. The anti-neutrino decay photodisintegration heavy nuclei photons also shown to be quite 10−11 while photo-pion...
High-energy astrophysical neutrino fluxes are, for many applications, modeled as simple power laws a function of energy. While this is reasonable in the case production hadronuclear $pp$ sources, it typically does not capture behavior photohadronic $p\gamma$ sources: that case, spectrum depends on properties target photons cosmic rays collide with and possible magnetic-field effects secondary pions muons. We show from known sources can be reproduced by thermal (black-body) target-photon if...
The interactions of ultra-high energy cosmic rays (UHECRs) with background photons in extragalactic space generate high-energy neutrinos and photons. Simulating UHECR propagation requires assumptions about physical quantities such as the spectrum light (EBL) photodisintegration cross sections. These assumptions, well approximations used codes, may influence computed predictions both cosmic-ray spectra composition, cosmogenic neutrino photon fluxes. Following up on our previous work where we...
The Global Cosmic-ray Observatory (GCOS) is a proposed large-scale observatory for studying ultra-high-energy cosmic particles, including rays (UHECRs), photons, and neutrinos. Its primary goal to characterise the properties of highest-energy particles in Nature with unprecedented accuracy, identify their elusive sources. With an aperture at least ten-fold larger than existing observatories, this next-generation facility should start operating after 2030, when present-day detectors will...
We interpret the correlation between local star-forming galaxy positions and ultra-high-energy cosmic ray (UHECR) directions, recently detected by Pierre Auger Observatory (PAO), in terms of physical parameters: density sources magnetic fields governing UHECR propagation. include a Galactic field model on top random extragalactic description to determine level deflections expected from an ensemble source positions. Besides fields, we also take into account energy losses with background...
The Pierre Auger Observatory (PAO) and Telescope Array (TA) collaborations report significant differences in the observed energy spectra of ultra-high-energy cosmic rays (UHECRs) above 30~EeV. In this work we present a joint fit TA PAO data using rigidity-dependent maximum model, including full marginalization over all relevant parameters. We test two possible scenarios to explain these differences. One is that they are due complex energy-dependent experimental systematics; other presence...
When ultra-high-energy cosmic rays (UHECRs) propagate through the universe they produce secondary neutrinos as well photons, electrons and positrons (initiating electromagnetic cascades) in different kinds of interactions. These cascades are detected at Earth isotropic extragalactic fluxes. The level these fluxes can be predicted used to constrain UHECR source models. public astrophysical simulation framework CRPropa 3, designed for simulating propagating extraterrestrial ultra-high energy...
Since astrophysical neutrinos are produced in the interactions of cosmic rays, identifying origin rays using directional correlations with is one most interesting possibilities field. For that purpose, especially Ultra-High Energy Cosmic Rays (UHECRs) promising, as they deflected less by extragalactic and Galactic magnetic fields than at lower energies. However, photo-hadronic UHECRs limit their horizon, while do not interact over cosmological distances. We study possibility to search for...
With the newest version of our Monte Carlo code for ultra-high-energy cosmic ray (UHECR) propagation, CRPropa 3, flux neutrinos and photons due to interactions UHECRs with extragalactic background light can be predicted. Together recently updated data isotropic diffuse gamma-ray (IGRB) by Fermi LAT, it is now possible severely constrain UHECR source models. The evolution sources especially plays an important role in determination expected secondary photon spectrum. Pure proton models are...
We consider the synchrotron emission from electrons out in Galactic halo bubble region where Fermi structures reside. Utilising a simple analytical expression for non-thermal electron distribution and toy magnetic field model, we simulate polarised maps at frequency of 30~GHz. Comparing these with observational data, obtain constraints on parameters our model. this parameter value range determine corresponding arrival directions suppression factors ultra high energy cosmic rays (UHECRs)...
Over the last decade, observations have shown that mean mass of ultra-high-energy cosmic rays (UHECRs) increases progressively toward highest energies. However, precise composition is still unknown, and several theoretical studies hint at existence a subdominant proton component up to Motivated by exciting prospect performing charged-particle astronomy with (UHE) protons we quantify level UHE-proton flux compatible present multimessenger associated fluxes neutral messengers produced in...
Solving the question of origin ultra-high energy cosmic rays (UHECRs) requires development detailed simulation tools in order to interpret experimental data and draw conclusions on UHECR universe. CRPropa is a public Monte Carlo code for galactic extragalactic propagation ray nuclei above ∼ 1017 eV, as well their photon neutrino secondaries. In this contribution new algorithms features 3, next major release, are presented. 3 introduces time-dependent scenarios include evolution presence...
To answer the fundamental questions concerning origin and nature of ultra-high energy cosmic rays (UHECRs), it is important to confront data with simulated astrophysical scenarios. These scenarios should include detailed information on particle interactions environments. achieve this goal one make use computational tools simulate propagation these particles. For reason CRPropa framework was developed. It allows UHECRs energies ≳1017 eV secondary gamma neutrinos. The newest version, 3,...