Probing intergalactic magnetic fields with simulations of electromagnetic cascades

Batista, Rafael Alves; Saveliev, Andrey; Sigl, Günter; Vachaspati, Tanmay

doi:10.1103/physrevd.94.083005

Cited by 37 publications

(46 citation statements)

References 58 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The neutrino fluences derived from numerical simulations which take into account the effect of nuclear cascade process are comparable to our analytic results. The difference at the higher energy range is due to the fact that the analytical approach does not take into account the contribution from multi-pion neutrino production as well as the energy spread of secondaries [114,118]. (The similar trend was found by Ref.…”

Section: A Neutrino Fluencessupporting

confidence: 73%

Ultrahigh-energy cosmic-ray nuclei and neutrinos from engine-driven supernovae

Zhang

Murase

2019

Phys. Rev. D

View full text Add to dashboard Cite

Transrelativistic supernovae (SNe), which are likely driven by central engines via jets or winds, have been among candidate sources of ultrahigh-energy cosmic rays (UHECRs). We investigate acceleration and survival of UHECR nuclei in the external reverse shock scenario. With composition models used in Zhang et al. (2018), we calculate spectra of escaping cosmic rays and secondary neutrinos. If their local rate is ∼ 1% of the core-collapse supernova rate, the observed UHECR spectrum and composition can be explained with the total cosmic-ray energy Ecr ∼ 10 51 erg. The maximum energy of UHECR nuclei can reach ∼ 10 20 − 10 21 eV. The diffuse flux of source neutrinos is predicted to be ∼ 10 −11 − 10 −10 GeV cm −2 s −1 sr −1 in the 0.1-1 EeV range, satisfying nucleussurvival bounds. The associated cosmogenic neutrino flux is calculated, and shown to be comparable or even higher than the source neutrino flux. These ultrahigh-energy neutrinos can be detected by ultimate detectors such as the Giant Radio Askaryan Neutrino Detector and Probe Of Extreme Multi-Messenger Astrophysics.

show abstract

Section: A Neutrino Fluencessupporting

confidence: 73%

Ultrahigh-energy cosmic-ray nuclei and neutrinos from engine-driven supernovae

Zhang

Murase

2019

Phys. Rev. D

View full text Add to dashboard Cite

show abstract

“…This is in agreement with Alves Batista et al (2019b), where equally low fluxes were predicted. 4 A small but relevant difference resides in the propagation code, since Alves Batista et al (2019b) assume a simplified redshift scaling of the CIB, whose effects in the neutrino fluxes are explained in Alves Batista et al (2019a). If we apply the same simplified scaling, the cosmogenic neutrino flux in our calculations increases by 50%.…”

Section: Cosmogenic Neutrino Fluxesmentioning

confidence: 97%

A New View on Auger Data and Cosmogenic Neutrinos in Light of Different Nuclear Disintegration and Air-shower Models

Heinze¹,

Fedynitch²,

Boncioli³

et al. 2019

ApJ

113

178

View full text Add to dashboard Cite

We study the implications of Ultra-High Energy Cosmic Ray (UHECR) data from the Pierre Auger Observatory for potential accelerator candidates and cosmogenic neutrino fluxes for different combinations of nuclear disintegration and air-shower models. We exploit the most recent spectral and mass composition data (2017) with a new, computationally efficient simulation code PriNCe. We extend a systematic framework, which has been previously applied in a combined fit by the Pierre Auger Collaboration, with the cosmological source evolution as an additional free parameter. In this framework, an ensemble of generalized UHECR accelerators is characterized by a universal spectral index (equal for all injection species), a maximal rigidity, and the normalizations for five nuclear element groups. We find that the 2017 data favor a small but constrained contribution of heavy elements (iron) at the source. We demonstrate that the results moderately depend on the nuclear disintegration (PSB, Peanut, or Talys) model, and more strongly on the air-shower (EPOS-LHC, Sibyll-2.3, or QGSjet-II-04) model. Variations of these models result in different source evolutions and spectral indices, limiting the interpretation in terms of a particular class of cosmic accelerators. Better constrained parameters include the maximal rigidity and the mass composition at the source. Hence, the cosmogenic neutrino flux can be robustly predicted. Depending on the source evolution at high redshifts the flux is likely out of reach of future neutrino observatories in most cases, and a minimal cosmogenic neutrino flux cannot be claimed from data without assuming a cosmological distribution of the sources.

show abstract

“…In general, B relates to the deflection angle of electrons via the Lorentz force, whereas L B determines the propagation regime (diffusive when the Larmor radii of electrons is much smaller than the L B , and ballistic otherwise). In addition, it has been shown that the shape of the halo is important as well as it may contain information about the magnetic helicity of IGMFs (Tashiro et al 2014;Alves Batista et al 2016a;Duplessis & Vachaspati 2017), since helical fields produce spiral-like structures in the arrival directions.…”

Section: Introductionmentioning

confidence: 99%

The Impact of Plasma Instabilities on the Spectra of TeV Blazars

Batista

Saveliev

Pino

2019

Monthly Notices of the Royal Astronomical Society

Self Cite

View full text Add to dashboard Cite

Relativistic jets from blazars are known to be sources of very-high-energy gamma rays (VHE-GRs). During their propagation in the intergalactic space, VHEGRs interact with pervasive cosmological photon fields such as the extragalactic background light (EBL) and the cosmic microwave background (CMB), producing electron-positron pairs. These pairs can upscatter CMB/EBL photons to high energies via inverse Compton (IC) scattering, thereby continuing the cascade process. This is often used to set limits on intergalactic magnetic fields (IGMFs). However, the picture may change if plasma instabilities, arising due to the interaction of the pairs with the intergalactic medium (IGM), cool down the electrons/positrons faster than inverse Compton scattering. As a consequence, the kinetic energy lost by the pairs to the IGM could cause a hardening in the observed gamma-ray spectrum at energies below ∼100 GeV. Here we study several types and models of instabilities and assess their impact for interpreting observations of distant blazars. Our results suggest that plasma instabilities can describe the spectra of some blazars and mimic the effects of IGMFs, depending on parameters such as the intrinsic spectrum of the object, the density and temperature of the IGM, and the luminosity of the beam. On the other hand, we find that for our fiducial set of parameters plasma instabilities do not have a major impact on the spectra of some of the blazars studied. Therefore, they may be used for constraining IGMFs.

show abstract

Probing intergalactic magnetic fields with simulations of electromagnetic cascades

Cited by 37 publications

References 58 publications

Ultrahigh-energy cosmic-ray nuclei and neutrinos from engine-driven supernovae

Ultrahigh-energy cosmic-ray nuclei and neutrinos from engine-driven supernovae

A New View on Auger Data and Cosmogenic Neutrinos in Light of Different Nuclear Disintegration and Air-shower Models

The Impact of Plasma Instabilities on the Spectra of TeV Blazars

Contact Info

Product

Resources

About