Cosmic-Ray Theory

Rossi, Bruno; Greisen, K.

doi:10.1103/revmodphys.13.240

Cited by 1,044 publications

(393 citation statements)

References 38 publications

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“…The well known expressions for ϕ(v) and ψ(u) can be found, for example, in [22]. In a first approximation the production of muon pairs can be obtained simply rescaling Eq.…”

Section: Leptons From Charm Decaymentioning

confidence: 99%

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Atmospheric muon and neutrino fluxes at very high energy

Illana¹,

Lipari²,

Masip³

et al. 2011

Astroparticle Physics

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The observation of astrophysical neutrinos requires a detailed understanding of the atmospheric neutrino background. Since neutrinos are produced in meson decays together with a charged lepton, important constraints on this background can be obtained from the measurement of the atmospheric muon flux. Muons, however, can also be produced as µ + µ − pairs by purely electromagnetic processes. We use the Z-moment method to study and compare the contributions to the atmospheric muon and neutrino fluxes from different sources (π/K decay, charmed and unflavored hadron decay, and photon conversion into a muon pair). We pay special attention to the contribution from unflavored mesons (η, η , ρ • , ω and φ). These mesons are abundant in air showers, their lifetimes are much shorter than those of charged pions or kaons, and they have decay branching ratios of order 10 −4 into final states containing a muon pair. We show that they may be the dominant source of muons at E µ 10 3 TeV.

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“…The well known expressions for ϕ(v) and ψ(u) can be found, for example, in [22]. In a first approximation the production of muon pairs can be obtained simply rescaling Eq.…”

Section: Leptons From Charm Decaymentioning

confidence: 99%

“…The photon spectrum is generated by the decay of neutral pions, with smaller contributions from the decay of η mesons and other hadronic resonances. The quantity σ γ and the functions A(s), B(s) and C(s) were introduced by Rossi and Greisen [22]:…”

Section: Leptons From Charm Decaymentioning

confidence: 99%

Atmospheric muon and neutrino fluxes at very high energy

Illana¹,

Lipari²,

Masip³

et al. 2011

Astroparticle Physics

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“…Therefore we can apply some simplifying hypothesis to solve the cascade equations. The analytical expressions under Approximation A obtained by Rossi & Greisen (1941) for the differential spectra are implemented here. At energies E m e c 2 Z −1/3 /α collision processes and Compton effect can be neglected and the asymptotic formulae used to describe radiation processes and pair production.…”

Section: Cascades Inside the Diskmentioning

confidence: 99%

Very high energy γ-ray emission from X-ray transients during major outbursts

Orellana

Romero

Pellizza

et al. 2007

A&A

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Context. Some high mass X-ray binaries (HMXB) have been recently confirmed as γ-ray sources by ground based Cherenkov telescopes. In this work, we discuss the γ-ray emission from X-ray transient sources formed by a Be star and a highly magnetized neutron star. This kind of systems can produce variable hadronic γ-ray emission through the mechanism proposed by Cheng and Ruderman, where a proton beam accelerated in the pulsar magnetosphere impacts the transient accretion disk. We choose as case of study the best known system of this class: A0535+26. Aims. We aim at making quantitative predictions about the very high-energy radiation generated in Be-X ray binary systems with strongly magnetized neutron stars. Methods. We study the gamma-ray emission generated during a major X-ray outburst of a HMXB adopting for the model the parameters of A0535+26. The emerging photon signal from the disk is determined by the grammage of the disk that modulates the optical depth. The electromagnetic cascades initiated by photons absorbed in the disk are explored, making use of the so-called "Approximation A" to solve the cascade equations. Very high energy photons induce Inverse Compton cascades in the photon field of the massive star. We implemented Monte Carlo simulations of these cascades, in order to estimate the characteristics of the resulting spectrum. Results. TeV emission should be detectable by Cherenkov telescopes during a major X-ray outburst of a binary formed by a Be star and a highly magnetized neutron star. The γ-ray light curve is found to evolve in anti-correlation with the X-ray signal.

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“…In these studies it has been shown that most distributions of the bulk of the secondary particles can be described by universal functions depending only on a small number of scaling parameters. Regarding distributions related to the longitudinal shower evolution, the most important parameter is the shower age s. The definition of shower age follows from the analytic treatment of electromagnetic cascades [30] and applies only to electromagnetic showers. To extend the concept to showers in general, it is common to use the phenomenological definition [12] …”

Section: Universality Of Electron and Cherenkov Photon Distributionsmentioning

confidence: 99%

Asymmetry of the angular distribution of Cherenkov photons of extensive air showers induced by the geomagnetic field

Homola

Engel

Wilczyński

2015

Astroparticle Physics

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The angular distribution of Cherenkov light in an air shower is closely linked to that of the shower electrons and positrons. As charged particles in extensive air showers are deflected by the magnetic field of the Earth, a deformation of the angular distribution of the Cherenkov light, that would be approximately symmetric about the shower axis if no magnetic field were present, is expected. In this work we study the variation of the Cherenkov light distribution as a function of the azimuth angle in the plane perpendicular to shower axis. It is found that the asymmetry induced by the geomagnetic field is most significant for early stages of shower evolution and for showers arriving almost perpendicular to the vector of the local geomagnetic field. Furthermore, it is shown that ignoring the azimuthal asymmetry of Cherenkov light might lead to a significant under-or overestimation of the Cherenkov light signal especially at sites where the local geomagnetic field is strong. Based on CORSIKA simulations, the azimuthal distribution of Cherenkov light is parametrized in dependence on the magnetic field component perpendicular to the shower axis and the local air density. This parametrization provides an efficient approximation for estimating the asymmetry of the Cherenkov light distribution for shower simulation and reconstruction in cosmic ray and gamma-ray experiments in which the Cherenkov signal of showers with energies above 10 14 eV is observed.

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Cosmic-Ray Theory

Cited by 1,044 publications

References 38 publications

Atmospheric muon and neutrino fluxes at very high energy

Atmospheric muon and neutrino fluxes at very high energy

Very high energy γ-ray emission from X-ray transients during major outbursts

Asymmetry of the angular distribution of Cherenkov photons of extensive air showers induced by the geomagnetic field

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