We survey the theory and experimental tests for the propagation of cosmic rays in the Galaxy up to energies of 10 15 eV. A guide to the previous reviews and essential literature is given, followed by an exposition of basic principles. The basic ideas of cosmic-ray propagation are described, and the physical origin of its processes is explained. The various techniques for computing the observational consequences of the theory are described and contrasted. These include analytical and numerical techniques. We present the comparison of models with data, including direct and indirect—especially γ-ray—observations, and indicate what we can learn about cosmic-ray propagation. Some important topics, including electron and antiparticle propagation, are chosen for discussion.

/pdf/cosmic-ray-propagation-and-interactions-in-the-galaxy-52wrtrud7h.pdf

Cosmic-Ray Propagation and Interactions in the Galaxy

Aims. This paper gives a description of a new online database and associated online tools (data selection, data export, plots, etc.) for charged cosmic-ray measurements. The experimental setups (type, flight dates, techniques) from which the data originate are included in the database, along with the references to all relevant publications. Methods. The database relies on the MySQL5 engine. The web pages and queries are based on PHP, AJAX and the jquery, jquery.cluetip, jquery-ui, and table-sorter third-party libraries. Results. In this first release, we restrict ourselves to Galactic cosmic rays with Z 30 and a kinetic energy per nucleon up to a few tens of TeV/n. This corresponds to more than 200 di erent sub-experiments (i.e., di erent experiments, or data from the same experiment flying at di erent times) in as many publications. Conclusions. We set up a cosmic-ray database (CRDB) and provide tools to sort and visualise the data. New data can be submitted, providing the community with a collaborative tool to archive past and future cosmic-ray measurements.

/pdf/a-database-of-charged-cosmic-rays-xyngbfdprw.pdf

A database of charged cosmic rays

A measurement of the energy spectra of cosmic-ray positrons and electrons was made with a balloon-borne magnet- spectrometer, which was flown at a mean geomagnetic cut-o of 4.5 GV/c. The observed positron flux in the energy range 7-16 GeV is approximately an order of magnitude lower than that of electrons, as measured in other experiments at various energies. The power law spectral index of the observed dierential energy spectrum of electrons is 2:89 0:10 in the energy interval 7.5-47 GeV. For positrons the overall fit of the available data above 7 GeV has been considered. The spectral index is found to be 3:37 0:26 and the fraction of positrons, e + /(e + + e ), has a mean value of 0:064 0:003. The world data on e + /(e + + e ) from 0.1 to 30 GeV indicate that a plerion type electron spectrum is preferred over the other types. The trend of the presently existing high energy data also suggests a possible contribution of positrons produced at the pulsar polar cap. High resolution experiments capable of identifying positrons at least up to 100 GeV with high statistics are required to pinpoint the origin of both electrons and positrons in the cosmic radiation.

/pdf/measurements-of-the-absolute-energy-spectra-of-cosmic-ray-4n7pm1b974.pdf

Measurements of the absolute energy spectra of cosmic-ray positrons and electrons above 7 GeV

A dramatic increase in the accuracy and statistics of space-borne cosmic ray (CR) measurements has yielded several breakthroughs over the last several years. The most puzzling is the rise in the positron fraction above ∼10 GeV over the predictions of the propagation models assuming pure secondary production. The accuracy of the antiproton production cross section is critical for a strophysical applications and searches for new physics since antiprotons in CRs seem to hold the keys to many puzzles including the origin of those excess positrons. However, model calculations of antiproton production in CR interactions with interstellar gas are often employing parameterizations that are out of date or are using outdated physical concepts. That may lead to an incorrect interpretation of antiproton data which could have broad consequences for other areas of astrophysics. In this work, we calculate antiproton production in pp-, pA-, and AA-interactions using EPOS-LHC and QGSJET-II04, two of the most advanced Monte Carlo (MC) generators tuned to numerous accelerator data including those from the Large Hadron Collider (LHC). We show that the antiproton yields obtained with these MC generators differ by up to an order of magnitude from yields of parameterizations commonly used in astrophysics.

http://iopscience.iop.org/article/10.1088/0004-637X/803/2/54/pdf

New calculation of antiproton production by cosmic ray protons and nuclei

This paper gives a description of a new on-line database this http URL and associated on-line tools (data selection, data export, plots, etc.) for charged cosmic-ray measurements. The experimental setups (type, flight dates, techniques) from which the data originate are included in the database, along with the references to all relevant publications. The database relies on the MySQL5 engine. The web pages and queries are based on PHP, AJAX and the jquery, jquery.cluetip, jquery-ui, and table-sorter third-party libraries. In this first release, we restrict ourselves to Galactic cosmic rays with Z<=30 and a kinetic energy per nucleon up to a few tens of TeV/n. This corresponds to more than 200 different sub-experiments (i.e., different experiments, or data from the same experiment flying at different times) in as many publications. We set up a cosmic-ray database and provide tools to sort and visualise the data. New data can be submitted, providing the community with a collaborative tool to archive past and future cosmic-ray measurements. Any help/ideas to further expand and/or complement the database is welcome (please contact crdatabase@lpsc.in2p3.fr).

Momentum spectra of pions, muons, electrons and secondary positrons have been measured at an atmospheric depth of 5: 8gc m 2 with the same instrument. Data was collected by the Matter Antimatter Space Spectrometer of the New Mexico State University in a balloon flight in September 1991 at the rigidity cut-off of 4 : 5G V c 1 in Fort Sumner, New Mexico. The first measurement of the positive muon spectrum in the range 0:15 GeV c 1 to 2 GeVc 1 is reported in this paper. The spectral index above 3 GeV c 1 of the negative muon momentum spectrum of this measurement is 2:39 0:05 in agreement with analytical cascade calculations which assume a primary proton kinetic energy spectrum with a slope of 2:740:02 in the corresponding kinetic energy range. In the momentum interval 300-700 MeV c 1 , both negative and positive muon fluxes turn out to be larger than calculated fluxes by a factor of about 1.4. The measurement of the secondary electron and positron energy spectra allows a reliable subtraction of the atmospheric background from the primary electron and positron fluxes which are affected by large uncertainties in most of the experiments. The energy spectra of the secondary particles reported here have the same systematic errors implying a higher relative accuracy with respect to those measurements made in different flights.

http://people.roma2.infn.it/~morselli/A40JofPhyGMass91pion_mu.pdf

Momentum spectra of atmospheric pions, muons, electrons and positrons at balloon altitudes

The antiproton-to-proton ratio,p ¯/p, in cosmic rays has been measured in the energy range 3.7‐19 GeV. This measurement was carried out using a balloon-borne superconducting magnetic spectrometer along with a gas Cerenkov counter, an imaging calorimeter, and a time-of-flight scintillator system. The measuredp ¯/p ratio was

/pdf/measurement-of-cosmic-ray-antiprotons-from-3-7-to-19-gev-4r2otc9r6r.pdf

Measurement of Cosmic-Ray Antiprotons from 3.7 to 19 GeV

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Momentum spectra of atmospheric pions, muons, electrons and positrons at balloon altitudes

Measurement of Cosmic-Ray Antiprotons from 3.7 to 19 GeV