Parameterization of Gamma, e^+/- and Neutrino SpectraProduced by p-p Interaction in Astronomical Environment

Kamae, T.; Karlsson, Niklas; Mizuno, T.; Abe, T.; Koi, T.

doi:10.2172/882833

Cited by 37 publications

(60 citation statements)

References 34 publications

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“…where dσ dR (i + j → e ± + X) represents the differential inclusive cross section for the production of electrons and positrons in ij reactions: for the pp case we take the parametrization proposed in [29,30], while for the processes involving He, as a projectile or as a target, we adopt the rescaling of the pp cross section obtained by following the prescriptions given in [31]. The quantity n j represents the density of the target species j, which is taken from the model discussed in [32], while Φ i (R, x) is the flux of the primary CR species i.…”

Section: Methodsmentioning

confidence: 99%

Breaks in interstellar spectra of positrons and electrons derived from time-dependent AMS data

et al. 2019

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Until fairly recently, it was widely accepted that local cosmic ray spectra were largely featureless power laws, containing limited information on their acceleration and transport. This viewpoint is currently being revised in the light of evidence for a variety of spectral breaks in the fluxes of cosmic ray nuclei. Here, we focus on cosmic ray electrons and positrons which at the highest energies must be of local origin due to strong radiative losses. We consider a pure diffusion model for their Galactic transport and determine its free parameters by fitting data in a wide energy range: measurements of the interstellar spectrum by Voyager at MeV energies, radio synchrotron data (sensitive to GeV electrons and positrons) and local observations by AMS up to ∼ 1 TeV. For the first time, we also model the time-dependent fluxes of cosmic ray electrons and positrons at GeV energies recently presented by AMS, treating solar modulation in a simple extension of the widely used force-field approximation. We are able to reproduce all the available measurements to date. Our model of the interstellar spectrum of cosmic ray electrons and positrons requires the presence of a number of spectral breaks, both in the source spectra and the diffusion coefficients. While we remain agnostic as to the origin of these spectral breaks, their presence will inform future models of the microphysics of cosmic ray acceleration and transport. arXiv:1904.05899v1 [astro-ph.HE]

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Section: Methodsmentioning

confidence: 99%

Breaks in interstellar spectra of positrons and electrons derived from time-dependent AMS data

et al. 2019

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“…For c e + , there are several reasons which could ascribe its relative large values: (i) the cross section comes from Kamae et al [112,113], which needed a scale factor to correlate its values [114]; (ii) the systematics between DAMPE CREs spectrum and AMS-02 positron spectrum is also partially accounted for in the parameter c e + , which lead c e + not just a indicator of rescale factor on cross section. Moreover, we would like to point our that in this work, we focus on the extra sources which would reproduce the break at ∼ 1 TeV in DAMPE CREs data.…”

Section: Nuisance Parametersmentioning

confidence: 99%

Bayesian analysis of the break in DAMPE lepton spectra

Niu

Ding

et al. 2018

Phys. Rev. D

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Recently, DAMPE has released its first results on the high-energy cosmic-ray electrons and positrons (CREs) from about 25 GeV to 4.6 TeV, which directly detect a break at ∼ 1 TeV. This result gives us an excellent opportunity to study the source of the CREs excess. In this work, we used the data for proton and helium flux (from AMS-02 and CREAM),p/p ratio (from AMS-02), positron flux (from AMS-02) and CREs flux (from DAMPE without the peak signal point at ∼ 1.4 TeV) to do global fitting simultaneously, which can account the influence from the propagation model, the nuclei and electron primary source injection and the secondary lepton production precisely. For extra source to interpret the excess in lepton spectrum, we consider two separate scenarios (pulsar and dark matter annihilation via leptonic channels) to construct the bump ( > ∼ 100 GeV) and the break at ∼ 1 TeV. The result shows: (i) in pulsar scenario, the spectral index of the injection should be νpsr ∼ 0.65 and the cut-off should be Rc ∼ 650 GV; (ii) in dark matter scenario, the dark matter particle's mass is mχ ∼ 1208 GeV and the cross section is σv ∼ 1.48 × 10 −23 cm 3 s −1 . Moreover, in the dark matter scenario, the ττ annihilation channel is highly suppressed, and a DM model is built to satisfy the fitting results. * jsniu@itp.ac.cn † tli@itp.ac.cn arXiv:1712.00372v4 [astro-ph.HE] 26 Apr 2018[1] J. Chang, "Dark matter particle explorer: The first chinese cosmic ray and hard gamma-ray detector in space,"Chinese Journal of Space Science 34, 550 (2014).

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“…The spectra of gamma-ray and neutrino emission from CRs inside the acceleration zone have to be derived with an account for both the pion decay hadronic emission and the inverse Compton components. The corresponding radiation cross sections can be found in ( e.g., Aharonian 2004, Kelner et al 2006, Kamae et al 2006. During this relatively short stage the accelerator can be detected as a source of high energy radiation of both hadronic and leptonic origin.…”

Section: Neutrinos and Gamma-rays From Compact Clustersmentioning

confidence: 99%

Nonthermal particles and photons in starburst regions and superbubbles

Bykov

2014

Astron Astrophys Rev

118

102

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Starforming factories in galaxies produce compact clusters and loose associations of young massive stars. Fast radiation-driven winds and supernovae input their huge kinetic power into the interstellar medium in the form of highly supersonic and superalfvenic outflows. Apart from gas heating, collisionless relaxation of fast plasma outflows results in fluctuating magnetic fields and energetic particles. The energetic particles comprise a long-lived component which may contain a sizeable fraction of the kinetic energy released by the winds and supernova ejecta and thus modify the magnetohydrodynamic flows in the systems. We present a concise review of observational data and models of nonthermal emission from starburst galaxies, superbubbles, and compact clusters of massive stars. Efficient mechanisms of particle acceleration and amplification of fluctuating magnetic fields with a wide dynamical range in starburst regions are discussed. Sources of cosmic rays, neutrinos and multi-wavelength nonthermal emission associated with starburst regions including potential galactic "PeVatrons" are reviewed in the global galactic ecology context.

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Parameterization of Gamma, e^+/- and Neutrino SpectraProduced by p-p Interaction in Astronomical Environment

Cited by 37 publications

References 34 publications

Breaks in interstellar spectra of positrons and electrons derived from time-dependent AMS data

Breaks in interstellar spectra of positrons and electrons derived from time-dependent AMS data

Bayesian analysis of the break in DAMPE lepton spectra

Nonthermal particles and photons in starburst regions and superbubbles

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