47 research outputs found
Stochastic cosmic ray sources and the TeV break in the all-electron spectrum
Despite significant progress over more than 100 years, no accelerator has
been unambiguously identified as the source of the locally measured flux of
cosmic rays. High-energy electrons and positrons are of particular importance
in the search for nearby sources as radiative energy losses constrain their
propagation to distances of about 1 kpc around 1 TeV. At the highest energies,
the spectrum is therefore dominated and shaped by only a few sources whose
properties can be inferred from the fine structure of the spectrum at energies
currently accessed by experiments like AMS-02, CALET, DAMPE, Fermi-LAT,
H.E.S.S. and ISS-CREAM. We present a stochastic model of the Galactic
all-electron flux and evaluate its compatibility with the measurement recently
presented by the H.E.S.S. collaboration. To this end, we have MC generated a
large sample of the all-electron flux from an ensemble of random distributions
of sources. We confirm the non-Gaussian nature of the probability density of
fluxes at individual energies previously reported in analytical computations.
For the first time, we also consider the correlations between the fluxes at
different energies, treating the binned spectrum as a random vector and
parametrising its joint distribution with the help of a pair-copula
construction. We show that the spectral break observed in the all-electron
spectrum by H.E.S.S. and DAMPE is statistically compatible with a distribution
of astrophysical sources like supernova remnants or pulsars, but requires a
rate smaller than the canonical supernova rate. This important result provides
an astrophysical interpretation of the spectrum at TeV energies and allows
differentiating astrophysical source models from exotic explanations, like dark
matter annihilation. We also critically assess the reliability of using
catalogues of known sources to model the electron-positron flux.Comment: 30 pages, 12 figures; extended discussion; accepted for publication
in JCA
A new analytic solution for 2nd-order Fermi acceleration
A new analytic solution for 2nd-order Fermi acceleration is presented. In
particular, we consider time-dependent rates for stochastic acceleration,
diffusive and convective escape as well as adiabatic losses. The power law
index q of the turbulence spectrum is unconstrained and can therefore account
for Kolmogorov (q = 5/3) and Kraichnan (q = 3/2) turbulence, Bohm diffusion (q
= 1) as well as the hard-sphere approximation (q = 2). This considerably
improves beyond solutions known to date and will prove a useful tool for more
realistic modelling of 2nd-order Fermi acceleration in a variety of
astrophysical environments.Comment: 14 pages, 4 figures; comments and references added; to appear in JCA
The 'PAMELA anomaly' indicates a nearby cosmic ray accelerator
We discuss the recently observed `excesses' in cosmic ray electron and
positron fluxes which have been widely interpreted as signals of dark matter.
By considering the production and acceleration of secondary electrons and
positrons in nearby supernova remnants, we predict an additional, harder
component that becomes dominant at high energies. The unknown spatial
distribution of the supernova remnants introduces a stochastic uncertainty
which we estimate analytically. Fitting the prediction for different source
distributions to the total electron + positron flux measured by Fermi--LAT
fixes all free parameters and allows us to `postdict' the rise in the positron
fraction seen by PAMELA. A similar rise in the B/C ratio is predicted at high
energies.Comment: 9 pages, 6 figures; accepted for the publication in the proceedings
of the ICATPP Conference on Cosmic Rays for Particle and Astroparticle
Physics, Villa Olmo (Como), Oct. 201
Origin of Small-Scale Anisotropies in Galactic Cosmic Rays
The arrival directions of Galactic cosmic rays (CRs) are highly isotropic.
This is expected from the presence of turbulent magnetic fields in our Galactic
environment that repeatedly scatter charged CRs during propagation. However,
various CR observatories have identified weak anisotropies of various angular
sizes and with relative intensities of up to a level of 1 part in 1,000.
Whereas large-scale anisotropies are generally predicted by standard diffusion
models, the appearance of small-scale anisotropies down to an angular size of
10 degrees is surprising. In this review, we summarise the current experimental
situation for both the large-scale and small-scale anisotropies. We address
some of the issues in comparing different experimental results and remaining
questions in interpreting the observed large-scale anisotropies. We then review
the standard diffusive picture and its difficulty in producing the small-scale
anisotropies. Having set the stage, we review the various ideas and models put
forward for explaining the small-scale anisotropies.Comment: 60 pages, 16 figures; invited review for Progress in Particle and
Nuclear Physics (PPNP
Testing astrophysical models for the PAMELA positron excess with cosmic ray nuclei
The excess in the positron fraction reported by the PAMELA collaboration has
been interpreted as due to annihilation or decay of dark matter in the Galaxy.
More prosaically, it has been ascribed to direct production of positrons by
nearby pulsars, or due to pion production during stochastic acceleration of
hadronic cosmic rays in nearby sources. We point out that measurements of
secondary nuclei produced by cosmic ray spallation can discriminate between
these possibilities. New data on the titanium-to-iron ratio from the ATIC-2
experiment support the hadronic source model above and enable a prediction to
be made for the boron-to-carbon ratio at energies above 100 GeV. Presently, all
cosmic ray data are consistent with the positron excess being astrophysical in
origin.Comment: 4 pages, 2 figures (RevTex4); revised to include additional data in
figures and references; accepted for publication in PR
Cosmic ray electron and positron spectra at TeV energies
Observations of cosmic ray electrons have made great strides in the last
decade and direct observations of the all-electron flux as well as separate
electron and positron spectra are now available up to ~ 1 TeV. In this invited
contribution to the 2022 edition of the Rencontres de Moriond on Very High
Energy Phenomena in the Universe, we review the data on cosmic ray electron and
positron spectra at TeV energies and offer general comments on their
interpretation. Subsequently, we focus on the study of the stochastic
fluctuations and a secondary model for the positron excess.Comment: Contribution to the 2022 Very High Energy Phenomena in the Universe
(VHEPU) session of the 56th Rencontres de Moriond. 8 pages, 7 figure
On cosmic ray acceleration in supernova remnants and the FERMI/PAMELA data
We discuss recent observations of high energy cosmic ray positrons and
electrons in the context of hadronic interactions in supernova remnants, the
suspected accelerators of galactic cosmic rays. Diffusive shock acceleration
can harden the energy spectrum of secondary positrons relative to that of the
primary protons (and electrons) and thus explain the rise in the positron
fraction observed by PAMELA above 10 GeV. We normalize the hadronic interaction
rate by holding pion decay to be responsible for the gamma-rays detected by
HESS from some SNRs. By simulating the spatial and temporal distribution of
SNRs in the Galaxy according to their known statistics, we are able to then fit
the electron (plus positron) energy spectrum measured by Fermi. It appears that
IceCube has good prospects for detecting the hadronic neutrino fluxes expected
from nearby SNRs.Comment: 13 pages, 8 figures (ReVTeX 4); Clarifying comments added; Revised
prediction for B/C added (new Fig.8); References added; To appear in Phys.
Rev.
Fingerprints of Galactic Loop I on the Cosmic Microwave Background
We investigate possible imprints of galactic foreground structures such as
the "radio loops" in the derived maps of the cosmic microwave background.
Surprisingly there is evidence for these not only at radio frequencies through
their synchrotron radiation, but also at microwave frequencies where emission
by dust dominates. This suggests the mechanism is magnetic dipole radiation
from dust grains enriched by metallic iron or ferrimagnetic materials. This new
foreground we have identified is present at high galactic latitudes, and
potentially dominates over the expected -mode polarization signal due to
primordial gravitational waves from inflation.Comment: 5 pages, 4 figures; matches published versio