67 research outputs found
Cosmic-Ray proton spectrum below 100 TeV in the local region
The propagation of cosmic-ray protons in the Galaxy is discussed under the
framework of a three dimensional convection-diffusion model. Starting with the
assumption of a uniform and continuous distribution of cosmic-ray sources
injecting CRs continuously in the Galaxy and by invoking a supernova explosion
at various distances from the Earth, it is found that only those sources
located within a distance of ~ 1.5 kpc can produce appreciable temporal
fluctuations in the CR proton flux observed at the Earth. So, the construction
of the local CR proton spectrum is discussed by seperating the contributions of
the distant sources from that of the nearby sources. The contribution from the
distant sources is treated in the framework of a continuous source distribution
model both in space as well as time, but that of the nearby sources in a
discrete space-time source model. The study predicts the presence of at least
one old nearby source with a characteristic age of ~ 10^5 yrs located at a
distance of ~ 0.1 kpc to explain the observed proton flux below ~ 100 GeV.Comment: 8 pages, 6 figures, 1 table, uses mn2e.cls, minor text corrections,
accepted for publication in MNRA
Effect of nearby supernova remnants on local Cosmic-Rays
We study in detail the effect of different particle release times from
sources on the cosmic-ray (CR) spectrum below in the Galaxy. We
discuss different possible forms of particle injection such as burst-like
injection, continuous injection for a finite time, injection from a stationary
source and energy dependent injection. When applied to the nearby known
supernova remnants, we find that the observed CR anisotropy data favour the
burst-like particle injection model for the CR diffusion coefficient
with in the local region. In the study we have
also found that the contribution of the sources G114.3+0.3 and Monogem dominate
if the observed anisotropy is a result of the effect of the nearby sources.
Further study shows that we should not neglect the contribution of the
undetected old sources to the local CR anisotropy.Comment: 7 pages, 3 figures, MNRAS accepted, minor text correction
GeV-TeV cosmic-ray spectral anomaly as due to re-acceleration by weak shocks in the Galaxy
Recent cosmic-ray measurements have found an anomaly in the cosmic-ray energy
spectrum at GeV-TeV energies. Although the origin of the anomaly is not clearly
understood, suggested explanations include effect of cosmic-ray source
spectrum, propagation effects, and the effect of nearby sources. In this paper,
we propose that the spectral anomaly might be an effect of re-acceleration of
cosmic rays by weak shocks in the Galaxy. After acceleration by strong
supernova remnant shock waves, cosmic rays undergo diffusive propagation
through the Galaxy. During the propagation, cosmic rays may again encounter
expanding supernova remnant shock waves, and get re-accelerated. As the
probability of encountering old supernova remnants is expected to be larger
than the younger ones due to their bigger sizes, re-acceleration is expected to
be mainly due to weaker shocks. Since weaker shocks generate a softer particle
spectrum, the resulting re-accelerated component will have a spectrum steeper
than the initial cosmic-ray source spectrum produced by strong shocks. For a
reasonable set of model parameters, it is shown that such re-accelerated
component can dominate the GeV energy region while the non-reaccelerated
component dominates at higher energies, explaining the observed GeV-TeV
spectral anomaly.Comment: 12 pages, A&A accepte
Nearby supernova remnants and the cosmic-ray spectral hardening at high energies
Recent measurements of cosmic-ray spectra of several individual nuclear
species by the CREAM, TRACER, and ATIC experiments indicate a change in the
spectral index of the power laws at TeV energies. Possible explanations among
others include non linear diffusive shock acceleration of cosmic-rays,
different cosmic-ray propagation properties at higher and lower energies in the
Galaxy and the presence of nearby sources. In this paper, we show that if
supernova remnants are the main sources of cosmic rays in our Galaxy, the
effect of the nearby remnants can be responsible for the observed spectral
changes. Using a rigidity dependent escape of cosmic-rays from the supernova
remnants, we explain the apparent observed property that the hardening of the
helium spectrum occurs at relatively lower energies as compared to the protons
and also that the spectral hardening does not persist beyond TeV
energies.Comment: 6 pages, MNRAS accepted, minor text correction
On the contribution of nearby sources to the observed cosmic-ray nuclei
The presence of nearby discrete cosmic-ray (CR) sources can lead to many
interesting effects on the observed properties of CRs. In this paper, we study
about the possible effects on the CR primary and secondary spectra and also the
subsequent effects on the CR secondary-to-primary ratios. For the study, we
assume that CRs undergo diffusive propagation in the Galaxy and we neglect the
effect of convection, energy losses and reacceleration. In our model, we assume
that there exists a uniform and continuous distribution of CR sources in the
Galaxy generating a stationary CR background at the Earth. In addition, we also
consider the existence of some nearby sources which inject CRs in a discrete
space-time model. Assuming a constant CR source power throughout the Galaxy,
our study has found that the presence of nearby supernova remnants (SNRs)
produces noticeable variations in the primary fluxes mainly above ~ 100 GeV/n,
if CRs are assumed to be released instantaneously after the supernova
explosion. The variation reaches a value of ~ 45% at around 10^5 GeV/n. Respect
to earlier studies, the variation in the case of the secondaries is found to be
almost negligible. We also discuss about the possible effects of the different
particle release times from the SNRs. For the particle release time of ~ 10^5
yr, predicted by the diffusive shock acceleration theories in SNRs, we have
found that the presence of the nearby SNRs hardly produces any significant
effects on the CRs at the Earth.Comment: 12 pages, 8 figures, 2 tables, accepted for publication in MNRA
High energy diffuse gamma-ray emission of the galactic disk and Galactic Cosmic-Ray spectra
Observations of diffuse Galactic gamma-ray spectrum by the EGRET instrument
reveal an excess above ~ 1 GeV over the expected gamma-ray spectrum calculated
under the assumption that the locally observed cosmic-ray (CR) spectra
represent the galactic CR spectra. Assuming that Galactic CRs of energy below ~
100 TeV are accelerated by supernova remnant (SNR) shock waves and that the
shock compression ratio is SNR age dependent, the average source injection
spectra from an ensemble of SNRs is calculated both in the inner (330<l<30) and
outer (30<l<330) regions of the galaxy. The calculation considers the SNR age
distribution in the galaxy. Injecting these spectra in the galaxy and using a
3-D convection-diffusion equation, the CR electrons and protons spectra in the
two galactic regions are obtained and their spectra in the galactic disk are
found to be flatter than the observed CR spectra. The diffuse gamma-ray
spectrum produced by the interaction of these galactic CRs with the ISM and
ISRFs is compared with the experimental data in both the galactic regions.
Furthermore, the steepening of the observed local CR spectra from the galactic
disk CR spectra are discussed by propagating local CRs having a source spectrum
derived using local SNR age distribution (SNRs located within 1.5 kpc from the
Sun), for a diffusion coefficient D_0 ~ 0.3\times 10^{27} cm^2 s^{-1} in the
local region which is much less than the typical value in the galaxy D_0 ~
(1-10)\times 10^{28} cm^2 s^{-1}. The results obtained in this paper support
the SNR origin of galactic CRs.Comment: 30 pages, 12 figures, uses elsart.cls, some misprints are corrected,
accepted in Astroparticle Physic
The influence of the atmospheric refractive index on radio Xmax measurements of air showers
The refractive index of the atmosphere, which is n ≈ 1:0003 at sea level, varies with altitude and with local temperature, pressure and humidity. When performing radio measurements of air showers, natural variations in n will change the radio lateral intensity distribution, by changing the Cherenkov angle. Using CoREAS simulations, we have evaluated the systematic error on measurements of the shower maximum Xmax due to variations in n. It was found that a 10% increase in refractivity (n - 1) leads to an underestimation of Xmax between 8 and 22 g/cm2 for proton-induced showers at zenith angles from 15 to 45 degrees, respectively
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