The monthly rigidity spectrum of cosmic ray (CR) variations in the 19-24 cycles of solar activity was obtained by the global survey method using the data of continuous ground and near-Earth ...monitoring of CRs, exempted from atmospheric and local effects.The changes of the spectrum, first obtained for such a long period, made it possible to reveal the features of large-scale effects in CR modulation, the presence of 22-year and 11-year CR variations in the spectrum, and confirm an abnormal spectrum change in the 70s. The paper assumes a rigidity spectrum of CRs, given in a three-parameter form. Analysis of the obtained long-term CR variations for particles with rigidity 10 GV shows that the amplitude of the 22-year wave in the CR intensity increases from cycle to cycle and reaches its maximum value at the minimum of 23/24th solar activity cycle. Softening of the spectrum at the cycle minima has been revealed for the negative polarity of the solar magnetic field (qA<0). The reasons for the abnormally high CR density at the minimum of the 24th cycle and the spectrum features in the 70s are discussed. The spectrum of long-term CR variations in the 19-24 solar activity cycles, determined from the experimental data, makes it possible to verify some conclusions of the theory of heliospheric CR modulation concerning the role of the magnetic drift of particles in cycles with the different polarity of the solar magnetic field. In particular, we propose the explanation for the observed R−2 spectrum of the variations in the minima of the negative solar activity cycles, related with the scattering of particles in the vicinity of the neutral current sheet.
The inverse problem of cosmic ray transport of ultra-high energy cosmic rays is considered. The source spectrum and composition are derived based on the Auger data on energy spectrum, energy ...dependence of mean logarithm of atomic mass number and its variance. The regularization procedure for considered ill-posed problem and the statistical analysis of experimental data are employed.
The inverse problem of cosmic ray transport of ultra-high energy cosmic rays is considered. The source spectrum and composition are derived based on the recent Auger data on energy spectrum, energy ...dependence of mean logarithm of atomic mass number and its variance. The dependence of results on the extrapolation of observable spectrum beyond energies 10
20
eV is investigated.
Cosmic ray acceleration by shocks related with Slipping Interaction Regions (SIRs) in the Galactic Wind is considered. SIRs are similar to Solar Wind Corotating Interaction Regions. The spiral ...structure of our Galaxy results in a strong nonuniformity of the Galactic Wind flow and in SIR formation at distances of 50 to 100 kpc. SIRs are not corotating with the gas and magnetic field because the angular velocity of the spiral pattern differs from that of the Galactic rotation. It is shown that the collective reacceleration of the cosmic ray particles with charge $Z\rm e$ in the resulting shock ensemble can explain the observable cosmic ray spectrum beyond the “knee” up to energies of the order of $10^{17}\,Z$ eV. For the reaccelerated particles the Galactic Wind termination shock acts as a reflecting boundary.
The heliospheric modulation potential of galactic cosmic rays (CRs) is reconstructed for the era of neutron monitoring. It is based on using a modern model of the interstellar spectrum of galactic ...CRs and the spectrum of CR density variations. The spectrum of CR variations is obtained via global spectrographic processing of continuous monitoring data from the world network of detectors and is calibrated using data from direct measurements of the particle spectrum on the PAMELA magnetic spectrometer in base year 2009.
The calculations of source spectra of extragalactic cosmic rays with ultra high energies are made based on the solution of inverse problem for a system of transport equations that describes the ...propagation of protons and nuclei with energies 1018 to 1021 eV in the expanding Universe filled with the background radiation. It is assumed that protons and Iron nuclei are the most abundant species in the sources. The data from the Auger experiment is used to illustrate the method.
Using a so-called hemispherical model we derive a general transport equation for cosmic ray and thermal particles scattered in pitch angle by magnetic inhomogeneities in a moving collisionless ...plasma. The weak scattering through 90 degrees results in isotropic particle distributions in each hemisphere. The consideration is not limited by small anisotropies and by the condition that particle velocities are higher than characteristic flow velocity differences. For high velocities and small anisotropies the standard cosmic ray transport equation is recovered. We apply the equations derived for investigation of injection and acceleration of particles by collisionless shocks.
The local interstellar energy spectra of galactic cosmic rays down to a few MeV nucleon were directly measured in the experiment on the board of the Voyager 1 spacecraft. We suggest interpretation of ...these data based on our models of cosmic ray acceleration in supernova remnants and the diffusion in galactic wind where diffusion coefficient is determined by the cosmic ray streaming instability. The dependence of wind velocity on distance above the Galactic disk is determined.
We consider the diffusive shock acceleration in interstellar bubbles created by powerful stellar winds of supernova progenitors. Under the moderate stellar wind magnetization the bubbles are filled ...by the strongly magnetized low density gas. It is shown that the maximum energy of particles accelerated in this environment can exceed the ”knee” energy in the observable cosmic ray spectrum.
We present an analytical model for the hydrodynamic outflow from the disk of a starburst galaxy. The model is used to calculate the cosmic-ray propagation and the radio intensity distribution in the ...nuclear starburst region of NGC 253. We find that the cosmic-ray energy production rate of the central 600 pc of NGC 253 is about 3 x 10(41) ergs s(-1), which is about 15% of the total mechanical supernova power. For this inner region, we estimate a terminal outflow velocity of 900 km s(-1) and a mass-loss rate of (M) = 2-4 M( yr(-1).
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