Study of the extreme location of the penetration boundary of solar energetic particles (protons) into the Earth’s magnetosphere during the magnetic storms in 2001–2005

The results of studying the relationship between the extreme values of the penetration boundary location of solar energetic particles (protons with energies of 1–5 and 50–90 MeV) in the Earth’s magnetosphere and the geomagnetic indices Dst and K _p are reported.     

The spectrum of cosmic-ray particles and their origin

An analysis of all the direct measurements of the spectrum for all cosmic-ray particles over the energy range 0.1–10 TeV reveals an anomaly in the spectrum in the form of a step if the spectrum is represented as E^βI₀(E). The pattern of the anomaly unequivocally implies a proton spectrum with a knee at energy close to 1 TeV. The qualitative difference between the spectra of protons and nuclei with Z≥2 (the latter have a purely power-law spectrum over a wide energy range) leads us to conclude that the acceleration conditions for protons and nuclei are different. We consider the process characteristic only of protons that may be responsible for the emergence of a knee in the proton spectrum.     

Medium energy neutrinos from solar flares

The production of neutrinos with energies higher than 0.1 GeV in the solar atmosphere during solar flares is discussed. Neutrinos and muons are generated in decays of π^+- mesons produced in nuclear interactions of accelerated solar flare protons with matter of the Sun. Muons themselves decay yielding neutrinos. These neutrinos could come to the Earth and be detected with neutrino telescopes. Estimations of fluxes of such neutrinos are given.     

Absorbed dose from galactic cosmic rays and solar protons as derived from stratospheric measurements

Regular measurements of charged-particle fluxes in the Earth’s atmosphere, performed at the Lebedev Institute of Physics, Russian Academy of Sciences since 1957 up to date, are used to determine the absorbed dose rate in the atmosphere from galactic cosmic rays in the period of minimum solar activity and from solar protons during solar proton events. The values of the absorbed dose rate estimated from the measurement data for some intense solar proton events are reported.     

Polarimetry of the polarized proton and deuteron beams at intermediate energies

Method and results of the beam polarization measurements are presented. The measurements were carried out at the proton polarized beam of Saturne-II accelerator as well as at the JINR (Dubna) synchrophasotron vector polarized deuteron beam. The analysis of the elastic (quasi-elastic) pp-scattering polarization is used as a method of the polarization measurements. The energy range of the measurement is 1.0≤T _p ≤2.8 GeV for polarized proton and 1.66≤T _d ≤7.3 GeV for polarized deuteron beams.     

Latitude effect of muons in the Earth’s atmosphere during solar activity minimum

The results of muon flux measurements (E ≥ 70 MeV) in the atmosphere during solar activity minimum are reported. The measurements were performed during Antarctic sea expedition in 1975–1976 at several geomagnetic locations (from 1 to 14 GV). The experimental data obtained made it possible to determine the latitude effect of muons in the distribution at different levels in the atmosphere. The Geant4 program was used to simulate the galactic cosmic ray transport in the Earth’s atmosphere and evaluate the angular and spectral distributions (p, e^?/e⁺, photons, muons) at different atmospheric levels. The experimental and simulated results are in satisfactory agreement.     

Energieverteilung und Wirkungsquerschnitt der Photoprotonen aus N15

The energy spectra of photo protons from highly enriched N¹⁵ were investigated with the bremsstrahlung from the Heidelberg betatron running at six different endpoint energies between 19 and 30.5 MeV. The protons were detected at 90° to theγ-beam by means of a CsJ-spectrometer with pulse shape discrimination. The energy spectra show pronounced maxima atE _p =3.2; 4.6; 9.5 and 13.3 MeV. Proton yields are given as a function of endpoint energy, the yield value atE ₀=30.5 MeV being (7.0±0.8) μb/MeV · ster. Because the first excited state in the daughter nucleus C¹⁴ lies 6.09 MeV above the groundstate, the cross section for groundstate transitions of the process N¹⁵(γ, p)C¹⁴ could be derived from the upper 6 MeV of the single proton spectra. The main contribution to the cross section comes from the region between 18 and 26 MeV excitation energy with maxima at 19.5; 20.4; 22.7 and 24.5 MeV. A “pygmy resonance” occurs at 15.2 MeV with further less pronounced structures at 13.6 and 17.0 MeV. The integrated cross section for groundstate transitions up to 30.5 MeV is (22±3) MeVmb assuming isotropic angular distribution. The ratios of protons from transitions to excited states and from the (γ, n p)-reaction to those of groundstate transitions rise from 0.45 atE ₀=24.5 MeV to 0.70 atE ₀=30.5 MeV.     

New Parameter in the Description of Solar Cosmic Ray Events—Energy of Balance between Solar and Galactic Protons

Solar proton events possess a wide variety of features that reflect the conditions of solar proton acceleration and propagation. Relevant investigations rely on statistical methods that make it possible to classify events with the aim of obtaining deeper insight into physical processes leading to the generation of solar cosmic rays. In classifying events in power, the intensity of particles with energy above 10MeV at the maximum of the event time profile or the fluence of particles throughout the event time is usually used. A new parameter, E_qm, that characterizes the proton event power and which is some kind of approximation of the maximum energy of accelerated particles is analyzed in the present study. Correlations of E_qm with properties of x-ray flares on the Sun and with the velocity of coronal mass ejections are examined.     

Relativistic SCRs during the events of solar cycle 19

Two major ground-level SCR events in solar cycle 19 are analyzed: the events of May 4 and November 12, 1960. The characteristics of relativistic solar protons (RSPs) have been obtained using the up-to-date method based on the data from the ground based network of neutron monitors. The event of May 4, 1960, occurred against a quiet background, and during the event of 12.11.1960 two shocks, caused by previous flares in the same active region, approached the Earth. The RSP dynamics, related to disturbances in the interplanetary medium, is studied. The solar proton spectra, obtained from the ground-based measurements, are compared to the direct balloon measurements performed at that time.     

Die Spektren der Neutronen aus den Reaktionen C12(γ,n)C11 und O16(γ,n)O15

The (γ, n)-reactions on carbon and oxygen were studied using the 30,5 MeV brems-strahlung beam of the Heidelberg betatron. The photoneutrons were detected via the recoil protons in a stilbene scintillator. The pulse height spectrum of scintillations produced in the stilbene crystal by the recoil protons is analyzed to yield the incident neutron energy distribution. Theγ-ray and electron background was strongly reduced through pulse shape discrimination. To test the apparatus the spectrum of the neutrons from a Po-α-Be source was measured. The energy spectrum of the photo-neutrons from O¹⁶ shows clearly two peaks at excitation energies of 22,4 and 24,4 MeV also seen in the photo-proton spectra. The energy distribution of the neutrons from C¹² (γ, n) too contains indication of structure already known from the proton spectra from C¹² (γ, p). The derived cross sections of C¹² (γ, n ₀) and O¹⁶ (γ, n ₀) coincide as well in their shape as in their absolute magnitude with the corresponding (γ, p ₀)-cross sections. In both C¹² (γ, n) and O¹⁶ (γ, n)-reaction the neutrons seem to leave the final nucleus mainly in its ground state.     

Cyclic Variations in the Solar Radiation Fluxes at the Beginning of the 21st Century

The solar activity in the current, that is, the 24th, sunspot cycle is analyzed. Cyclic variations in the sunspot number (SSN) and radiation fluxes in various spectral ranges have been estimated in comparison with the general level of the solar radiation, which is traditionally determined by the radio emission flux F_10.7 at a wavelength of 10.7 cm (2.8 GHz). The comparative analysis of the variations in the solar constant and solar indices in the UV range, which are important for modeling the state of the Earth’s atmosphere, in the weak 24th cycle and strong 22nd and 23rd cycles has shown relative differences in the amplitudes of variations from the minimum to the maximum of the cycle. The influence of the hysteresis effect between the activity indices and F_10.7 in the 24th cycle, which is taken into account here, makes it possible to refine the forecast of the UV indices and solar constant depending on the quadratic regression coefficients that associate the solar indices with F_10.7 depending on the phase of the cycle.     

Properties of proton clusters in inelastic CC interactions accompanied by the production of Λ and <Emphasis Type="Italic">K</Emphasis><Superscript>0</Superscript> particles at <Emphasis Type="Italic">p</Emphasis> = 4.2 GeV/<Emphasis Type="Italic">c</Emphasis> per nucleon

Within a new relativistically invariant approach, the properties of proton clusters that are formed together with Λ and K⁰ particles in inelastic CC interactions at p=4.2 GeV/c per nucleon are investigated in the space of relative 4-velocities. The observed proton clusters are shown to be characterized by high values of the mean kinetic energy of the protons in the cluster rest frame: 〈T _p 〉=100±2 MeV.     

Specific features of the distribution of protons at small altitudes in near-equatorial latitudes according to data of satellite experiments. I. Energy spectrum

The spectra of protons with energies from 10 keV to 1 MeV as measured in experiments conducted at satellites and the MIR orbital station are presented. These data were obtained in the area of the geomagnetic equator at L < 1.15 and at altitudes up to 1000 km. The proton spectrum was determined during periods of geomagnetic perturbations and quite periods. These spectra were approximated using a kappa-function. The proton spectra in the near-equatorial area and in the ring current are compared. The proton’s life time in the near-equatorial area is estimated, taking into account charge exchange and Coulomb scattering. It is confirmed that the ring current is a main source of protons in the near-equatorial area at low altitudes.     

Die Energieverteilung der Neutronen aus einer Po-α-Be-Quelle

The neutrons from a Po-α-Be source were detected via the recoil protons in a stilbene scintillator. The pulse height spectrum of the scintillations produced in the stilbene crystal by the recoil protons is analysed to yield the incident neutron energy distribution. Theγ-ray background was eliminated through pulse shape discrimination. Separately the spectrum of neutrons coincident withγ-rays, i.e. of neutrons from the Be⁹(α,n)C^12* reaction, has been determined. The resulting spectra are compared to previous measurements. The structure of the spectra is not compatible with an isotropic angular distribution of the neutrons relative to theα-direction. Furthermore it could be shown that the fraction of reactions leading to the 7,65 MeV state of C¹² is only about 10^?3.     

Experimental Research to Confirm the Excitation of Gamov–Teller Resonance in Compound Nucleus <Superscript>118</Superscript>Sb

At proton energies of 4–9 MeV, trial experimental investigations were performed to confirm the excitation of Gamov–Teller resonance (GTR) 1⁺ in the compound nucleus ¹¹⁸Sb discovered by B.Ya. Guzhovskiy’s research group in the ¹¹⁷Sn(p,xn) reaction at proton energies of 7.2 MeV (the first component is GTR1) and 9.9MeV (the second component is GTR2). The ¹¹⁷Sn(p,xn) reaction was used, whose neutrons and background neutrons were registered by an all-wave long counter arranged at an angle of 140° to the direction of the proton beam propagation. Simultaneously, along with the registration of neutrons, elastically and inelastically scattered protons at angles of 20° and 160° were registered. At the proton energy equal to ~7.2 MeV, in the excitation functions for ¹¹⁷Sn(p,xn), ¹¹⁷Sn(p,p₀), and ¹¹⁷Sn(p,p₄)¹¹⁷Sn* (1004.5 keV, 3/2⁺), a resonance with a width of ≈1.2 MeV having an energy structure was discovered. Its possible quantum numbers are 1⁺.     

Untersuchung der Reaktion Si28 (γ,p) AI27

A silicon semiconductor detector was irradiated with betatron bremsstrahlung of different end point energies and the energy distributions of the protons originating in the detector itself by the reaction Si²⁸(γ,p) Al²⁷ were measured with good statistical accuracy. The end point energies were varied in 1 MeV steps from 15 to 30 MeV. Using the known spectral distribution of theγ-rays the energy dependence of the total cross section of the studied reaction could be derived from the measured proton spectra. The resulting cross section shows a peak at 20, 5 MeV and a half width of 4 MeV. Approximate values for the branching ratios for transitions to excited states of the residual nucleus could also be obtained.     

On the theory of temperature distribution over the Earth’s atmosphere

The steady-state temperature distribution over the Earth’s atmosphere is described in terms of the law of degradation of energy (or the principle of entropy increase). The distribution is in satisfactory agreement with meteorological measurements. Using constructed dissipative function \(\dot Q\), a nonlinear differential equation is rigorously derived that describes the synergetics of the steady-state temperature distribution over the atmosphere, from troposphere to exosphere. A detailed analysis of solutions of this equation makes it possible to qualitatively explain nontrivial dependence T(z) over an atmospheric area inhomogeneous in chemical composition. This fact substantiates the correctness of formal introduction and necessity to consider interaction between blackbody radiation and convective stream. It is argued that hard gamma quanta far from the violet part of the spectrum are responsible for heat radiation coming from the Sun.     

Study of proton resonances in 18Ne via resonant elastic scattering of 17F+p and its astrophysical implication

The proton resonant properties in ¹⁸Ne, which determine the reaction rate of the key stellar ¹⁴O(α,p)¹⁷F reaction, have been studied by using a technique of proton resonant elastic scattering of ¹⁷F+p. A 4.22 MeV/nucleon ¹⁷F radioactive ion (RI) beam was produced via a projectile-fragmentation reaction, and separated by a Radioactive Ion Beam Line in Lanzhou (RIBLL). By bombarding a thick (C_H2) _n target, the energy spectra of the recoiled protons were measured by two ΔE-E silicon telescopes at the center-of-mass scattering angles of θ _c.m.≈175°±5°, θ _c.m.≈152°±8°, respectively. Several proton resonances in ¹⁸Ne were observed clearly. A further R-matrix analysis of the experimental data is under way to determine the resonant parameters. The present work reports the preliminary results briefly.     

Distribution function and electron state density in nonequilibrium plasma created by dye laser

Ultracold nonequilibrium plasma created by a dye laser has been studied by the molecular dynamics method. Electrons and protons in this model of nonequilibrium plasma interacted according to the Coulomb law. In the case of electron-proton interaction and a distance between particles r < a ₀ (Bohr radius), the interaction energy is constant, e ²/a ₀ (e is the charge of electron). An initial proton kinetic energy is set randomly so that the average kinetic energy is 0.01–1 K. Initial full electron energy is also set randomly, but at the same time it is positive; i.e., all the electrons according to our task are located in the continuous spectrum. Average kinetic electron energy per one particle varies from 1 to 50 K. The motion equations in periodical boundary condition for this system have been solved by molecular dynamics method. We have calculated the distribution function in the region near the ionization threshold. The distribution function is being described using electron state density in the nearest neighbor approximation with activity correction.     

Measurement of the angular distribution of the polarization of the recoil proton from the photoproduction of neutral pions on hydrogen at a photon energy of 360 MeV. II

The angular distribution of the polarization of the recoil protons from the reactionγ+p→π ⁰+p has been measured at a photon energy of 360 MeV and at pion CM angles of 58°, 75°, 96° and 105°. The polarization of the protons has been determined by the left to right ratio in scattering on a helium gas target. The trajectory of each scattered proton has been measured by a system of spark chambers.