Solar modulation of galactic cosmic rays with the ARINA and PAMELA spectrometers

Solar modulation of the proton flux in Galactic space radiation during the period from the end of the 23rd to the beginning of 24th cycle of solar activity is investigated using data from the PAMELA magnetic spectrometer and ARINA scintillation spectrometer. The time dependence of proton intensity is plotted, and shows typical features in a form of rises and falls against a main trend. In order to explain these, the correlation between variations in the Galactic proton flux and solar/interplanetary parameters is investigated.     

Secondary electron and positron fluxes in the near-Earth space observed in the ARINA and PAMELA experiments

Secondary electron and positron fluxes in the energy range from 3 MeV to 7 GeV were measured with the ARINA and PAMELA spectrometers onboard the Resurs-DK satellite launched on June 15, 2006 into an elliptical orbit with an inclination of 70.4° and an altitude of 350–600 km. It is shown that positrons dominate over electrons by a factor of up to 4–5 in the geomagnetic equator region (L < 1.2 and B > 0.25).     

Criteria for selecting electrons with energies above 50 GeV according to the PAMELA experiment data

To separate the particles such as electrons and positrons, which are insignificant in number, from the total particle flux of cosmic rays, reliable enough criteria of their selection should be found. The proposed selection technique based on such criteria as the interaction in the first calorimeter layers, difference in the energy release for protons and electrons, and the measured number of neutrons makes it possible to separate electrons from the total charged particle flux with an impurity fraction no larger than 2% of the electron flux.     

Trapped Positrons and Electrons in the Inner Radiation Belt According to Data of the PAMELA Experiment

Measurements of secondary-electron and secondary-positron fluxes below the geomagnetic cutoff in near-Earth space were performed by means of the PAMELA magnetic spectrometer installed on board the Resurs-DK1 satellite launched on June 15, 2006, in an elliptical orbit of inclination 70° and altitude 350 to 600 km. This spectrometer permits measuring the fluxes of electrons and positrons over a wide energy range, as well as determining their spatial distributions to a precision of about 2°. A calculation of particle trajectories in the geomagnetic field makes it possible to separate electrons and positrons originating from cosmic-ray interactions in the Earth’s magnetosphere. The spatial distributions of quasitrapped, trapped, and short-lived albedo positrons and electrons of energy above 70 MeV in the radiation belt were analyzed. The ratio of the electron-to-positron fluxes and the energy spectra of the electrons and positrons in question are indicative of different productionmechanisms for stably trapped and quasitrapped secondary particles.     

Features of Short-Period Oscillations of Microwave Emission from the Solar Active Region before the Flare

The radiation of microwave sources above sunspots at a frequency of 17 GHz gives information about the parameters of solar plasma in the regions where the magneti-field strength is B ~ 2000 G in the transition region between the chromosphere and corona. Short-period oscillations (with a period of several minutes) of microwave emission from solar active regions (ARs) reflect wave processes in magnetic flux tubes of sunspots. Short-period oscillations of microwave emission from AR NOAA 12242 before two flares on December 17, 2014 are analyzed. This analysis is based on solar radio images obtained by means of the Nobeyama Radio Heliograph with a 10″?15″ two-dimensional spatial resolution. The radio maps of the whole solar disk were synthesized in a nonstandard mode with a cadence of 10 s and an averaging time of 10 s. An increase in the power of about ten-minute oscillations of microwave radiation approximately 40 to 50 min before the M1.5 flare (01: 00 UT) is found. On the same day, an increase in the power of ten-minute oscillations is observed about 60 min before the M8.7 flare (04: 42 UT). This effect is similar to the effect found earlier by two groups of authors independently for three-minute oscillations—namely, they observed a sharp increase in three-minute oscillations 15 to 20 min before the radio burst accompanying the flare. The effect in question may be interpreted as an relationship ofMHD waves propagating along the magnetic flux tube of a sunspot and the onset of the solar flare.     

Cosmic-ray positron from superparticle dark matter and the PAMELA anomaly

Motivated by the anomalous positron flux recently reported by the PAMELA Collaboration, we study the cosmic-ray positron produced by the pair annihilation and the decay of superparticle dark matter. We calculate the cosmic-ray positron flux and discuss implications of the PAMELA data. We show that the positron excess observed by the PAMELA can be explained with some of the superparticle dark matter.     

Solar Modulation of <Superscript>2</Superscript>H/<Superscript>1</Superscript>H and <Superscript>3</Superscript>He/<Superscript>4</Superscript>He according to Data Obtained in the PAMELA Satellite-Borne Experiment between 2006 and 2014

Preliminary results of measurements of the solar modulation of the isotopic hydrogen and helium content in galactic cosmic rays are presented for the first time. These data were obtained between 2006 and 2014 in the PAMELA international orbital experiment via measuring the time of flight of nuclei in the Pamela scintillation telescope and via analyzing, in the multilayered calorimeter of the PAMELA magnetic spectrometer, ionization losses of nuclei whose rigidity was known from trajectory measurements and which traversed the instrument without undergoing nuclear interactions. The results of these measurements are compared with existing experimental and calculated data, which are quite scanty.     

Energy Spectrum of Ultrahigh-Energy Cosmic Rays according to Data from Ground-Based Scintillation Detectors of the Yakutsk EAS Array

Results obtained from an analysis of the energy spectrum of cosmic rays with energies in the region of E₀ ≥ 10¹⁷ eV over the period of continuous observations from 1974 to 2017 are presented. A refined expression for estimating the primary-particle energy is used for individual events. This expression is derived from calculations aimed at determining the responses of the ground-based and underground scintillation detectors of the Yakutsk array for studying extensive air showers (EAS) and performed within theQGSJET-01-d, QGSJET-II-04, SIBYLL-2.1, and EPOS-LHCmodels by employing the CORSIKA code package. The new estimate of E₀ is substantially lower than its counterpart used earlier.     

Energy Spectrum of Ultrahigh-Energy Cosmic Rays according to Data from the Ground-Based Scintillation Detectors of the Yakutsk EAS Array

Journal of Experimental and Theoretical Physics - The energy spectrum of cosmic rays with energies E0 ≥ 1017 eV over the period of continuous observations in 1974–2017 is analyzed. A...     

Terrestrial Seismic Activity and Neutrons from the Surface of the Earth Associated with Lunar and Solar Tides

drastic increase in the flux of thermal neutrons of secondary cosmic radiation coming from the Earth was observed in the Pamir Mountains during the solar eclipse of July 22, 1990. In the following years, such phenomena were observed on each new moon and each full moon, when lunar and solar tides combine to produce an exceptionally high resultant tide. Tidal forces may serve as a trigger for the release of the deepearth seismic energy in a certain region. This directed our attention to the search for a temporal correlation between earthquakes and new and full moons, which may help identify a new type of seismic activity precursor. Such a correlation was found in the circum-Pacific belt and the adjacent regions at latitudes above 40° N and 10° S. The results of daytime measurements of the thermal neutron flux from the surface of the Earth in the Western Pamirs (Moskvin Glade, 4200 m above sea level) on August 1–14, 1994, are reported in the present study. Since these days were quiet in terms of weather and heliophysical and geophysical activity, the intensity of neutrons of secondary cosmic radiation was expected to remain almost constant. However, twofold (or even larger) intraday variations of the neutron count rate were observed on August 1–14, 1994. These quiet measurement conditions rule out the possibility that these bursts were associated with certain known extraterrestrial factors. It has been demonstrated that the observed neutron-intensity peaks were produced by lunar and solar tides. These results confirm that tidal forces play a prominent part in the generation of neutron fluxes from the surface of the Earth. The Astronomical Yearbook for 1994 published by the Russian Academy of Sciences was used in the present study.     

分立波长型近红外光谱分析仪定标模型的优化

对于滤光片型或者二极管阵列型等采用非连续扫描方式工作的近红外光谱仪来说 ,如何快速、准确地进行定标波长的优选一直是很关键的问题 ,传统近红外定标波长的优选采用向前或者向后逐步多元线性回归方法 ,依据回归结果所给出的各个波长的t检验值进行定标波长的筛选 ,但是在实际应用中 ,被筛选掉的波长也可能是非常有用的定标波长 ,而增加波长的定标所给出的定标标准差往往会减小 ,但预测精度则不一定会提高。文章将组合数学中的组合生成算法和面向矩阵运算的计算机语言相结合运用于近红外最优回归定标波长的计算机选取 ,可以在较短的时间内完成最优波长组合的选取 ,由于最优波长组合的选取是在优选定标波长数一定的前提下进行比较而且以经回归定标分析确定定标标准差最小原则 ,所以由此得到的定标方程是稳健的。     

一个和X级太阳耀斑相关的甚高能GLE事件

分析怀柔宇宙线EAS阵列在1991年6月份的计数率,数据表明在6月15日的太阳X12/3B级大耀斑后的GLE事件持续期间,TeV能区的宇宙线强度在25min内比通常有将近4a的超出,增强过程持续约25min.     

Investigation of geoeffective and non-geoeffective CMEs according to data from the URAGAN muon hodoscope

Coronal mass ejections are the brightest manifestations of solar activity. Dozens of coronal mass ejections are observed daily during periods of higher solar activity. They directly affect cosmic ray fluxes that carry information on plasma clouds, including clouds moving toward the Earth. Several aspects of geoeffective and non-geoeffective coronal mass ejections, observed with the ground-based URAGAN muon hodoscope operated as part of the NEVOD experimental complex at MEPhI, are discussed. The anisotropy of cosmic ray muon fluxes recorded during coronal mass ejections in 2014 and 2015 is investigated.     

Analysis of Variations of the Muon and Hadron Components of Cosmic Rays at Different Phases of the Solar Activity During the 11-Year Solar Cycle

Physics of Atomic Nuclei - Variations of secondary cosmic rays on the Earth’s surface depend on the solar activity. To study these variations, neutron monitors and muon detectors are used....     

硅太阳能电池负载特性及Origin软件处理数据的应用研究

分别测量了多晶硅薄膜电池与卤素灯之间距离为50 cm,70 cm,90 cm时输出功率随负载电阻变化之间关系,用origin软件绘制了功率随电阻变化关系和伏安特性曲线,并找到最大功率点,计算出了电池的填充因子(FF)。结果表明距离越小,FF愈大,输出功率愈高。     

Features of the HF Signal Propagation on Oblique Sounding Paths During Solar and Magnetic Activity in September 2017

Radiophysics and Quantum Electronics - We present the results of studying the influence of solar and magnetic activity in September 2017 on the HF signal characteristics on subauroral and...