Forbush decreases recorded by the URAGAN muon hodoscope in 2006–2011

Variations in the cosmic ray muon flux on Earth’s surface during Forbush decreases (FD) recorded by the URAGAN muon hodoscope in 2006–2011 are investigated. The dependence of the rate of amplitude reduction on the primary particle energy in a range above 10 GeV at different phases of FD development is studied by analyzing the variations in the cosmic ray muon flux recorded with the hodoscope. Analytical data on the spatial and angular dynamics of the muon flux are used to estimate variations in the spatial anisotropy of the muon flux during FDs.     

Coupling functions for muon hodoscopes

The specific features of calculating the coupling functions for muon hodoscopes are considered. The results of calculating the main coupling functions for three versions of the primary spectra of cosmic rays (CR)—galactic CR, solar CR during proton events, and galactic CR variations during Forbush decreases-are presented. The calculations have been performed based on modeling CR propagation through the Earth’s atmosphere using the CORSIKA code. The mean and median CR energies, contributing to the muon detector counting rate, have been calculated for different zenith angles. It has been shown that muon detectors are sensitive to different energies of primary CRs for different directions.     

Investigating the energy, angular, and temporal characteristics of forbush effects registered by the URAGAN muon hodoscope

The results from analyzing variations in the flux of cosmic ray muons during Forbush effects (FEs) registered by the URAGAN muon hodoscope over the period 2005–2009 are presented. The dependences of the amplitudes for reductions in the intensity of the cosmic ray muon flux on the energy of primary particles in energy ranges higher than 10 GeV were obtained. Their changes upon different phases of Forbush effect development were investigated. The local anisotropy vectors were calculated on the basis of spatial-angular variations in the muon flux. Correlations between the parameters of physical properties in the near heloiosphere related to the Forbush effects and the characteristics of muon flux variations were analyzed.     

Study of the response of the cosmic ray muon flux to nonstationary processes in the Earth’s atmosphere

The results of the study of the correlation between dynamic atmospheric phenomena and cosmic ray muon flux variations are presented. The results of the long-term experiment on continuous measurements of spatioangular variations of the muon flux using the URAGAN muon hodoscope are considered. It was shown that the correlation between weather phenomena and changes in the angular distribution of the muon flux on the Earth’s surface are observed in 80% of cases, both in the general counting rate and in the zenith-azimuthal distribution of the muon flux intensity.     

Analysis of Forbush decreases observed using a muon telescope in Antarctica starting on 21 June 2015

A cosmic-ray muon telescope has been collecting data since the end of 2014, which was shortly after the telescope was built in the Zhongshan Station of Antarctica. The telescope is the first observation device to be built by Chinese scientists in Antarctica. The pressure change is very strong in Zhongshan station. The count rate of the pressure correction results shows that the large variations in the count rate are likely caused by pressure fluctuations. During the period from 18 June to 22 June 2015, four halo coronal mass ejections(CMEs) were ejected from the Sun. These CMEs initiated a series of Forbush decreases(FD) when they reached the Earth. We conducted a comprehensive study of the intensity fluctuations of galactic cosmic rays recorded during FDs. The intensity fluctuations used in this study were collected by cosmic ray detectors of multiple stations(Zhongshan, McMurdo,South Polar, and Nagoya), and the solar wind measurements were collected by ACE and WIND. The profile of the FD of 22 June demonstrated a four-step decrease. The traditional one-or two-step FD classification method does not adequately explain the FD profile results. The interaction between the faster CME that occurred on 21 June 2015 and the two slow CMEs of the earlier few days should be considered. The cosmic ray intensities of the South Pole,McMurdo, and Zhongshan stations have similar hourly variations, whereas the galactic cosmic rays recorded between polar and non-polar locations are distinct. The FD pre-increase of 22 June 2015 for the Nagoya muon telescope(non-polar location) lags those of the McMurdo and Zhongshan stations(polar locations) by 1 h. The FD onset of22 June 2015 for the Nagoya muon telescope lags those of the polar locations by 1 h.     

On the Mechanism of Temperature Variations in the Average Energy of Muons at Large Depths

Journal of Experimental and Theoretical Physics - Sources of seasonal temperature variations in the average energy of the muon flux detected in the LVD experiment have been discussed. It has been...     

Solar diurnal anisotropy measured using muons in GRAPES-3 experiment in 2006

The GRAPES-3 experiment at Ooty contains a large-area (560 m²) tracking muon detector. This detector consists of 16 modules, each 35 m² in area, that are grouped into four supermodules of 140 m² each. The threshold energy of muons is sec(θ) GeV along a direction with zenith angle θ and the angular resolution of the muon detector is 6°. Typically, it records ~4×10⁹ muons every day. The muon detector has been operating uninterruptedly since 2001, thus providing a high statistics record of the cosmic ray flux as a function of time over one decade. However, prior to using these data, the muon rate has to be corrected for two important atmospheric effects, namely, variations in atmospheric pressure and temperature. Because of the near equatorial location of Ooty (11.4°N), the seasonal variations in the atmospheric temperature are relatively small and shall be ignored here. Due to proximity to the equator, the pressure changes at Ooty display a dominant 12 h periodic behaviour in addition to other seasonal changes. Here, we discuss various aspects of a novel method for accurate pressure measurement and subsequent corrections applied to the GRAPES-3 muon data to correct these pressure-induced variations. The pressure-corrected muon data are used to measure the profile of the solar diurnal anisotropy during 2006. The data, when divided into four segments, display significant variation both in the amplitude (~45%) and phase (~42 m) of the solar diurnal anisotropy during 2006, which was a period of relatively low solar activity.     

Spectrum of long-term cosmic ray variations during the sunspot minimum in 2009

A method for determining the long-term spectrum of cosmic ray (CR) variations from observations with different ground-based (neutron monitors) and near-earth (stratosphere and satellite) detectors was presented in our previous works. In this paper, muon telescope data (Nagoya) are added, expanding the analyzed energy range and allowing us to determine the rigidity spectrum for 1974–2011. The data from the above devices for these years can be used jointly. The rigidity spectrum for the sunspot minimum of the 24th cycle was studied and compared with the CR intensity for the sunspot minima of other cycles. The reasons for abnormally high CR density during the minimum of the 24th cycle and other features of this period are discussed.     

Wide-aperture muon detector for diagnostics of the Earth’s atmosphere and magnetosphere

A wide-aperture large-area multilayered muon hodoscope is being constructed above the water Cherenkov calorimeter NEVOD (Moscow Engineering Physics Institute). This hodoscope is aimed at studying the processes in the Earth’s atmosphere and magnetosphere that lead to variations in the muon flux at the ground level. The structure of the detector and its data acquisition and triggering systems are described. Some preliminary results of the analysis of the data obtained using the first two supermodules of the system in the continuous series of measurements during 2005–2006 are discussed.     

Study on the Muon Backgroud in the Underground Laboratory of KIMS

KIMS is a group aiming at the search for WIMP. In WIMP search experiment, the muon is one important background. We measure the muon flux in Yangyang laboratory where is located at 700m underground. The structure and performance test of muon detector is described. The analysis on muon hit position and angle distribution has been performed. The simulations of muon flux have been done. The muon flux in the laboratory is found to be about (7.0±0.4)×10^-8/s/cm²/sr.     

Study of dynamics of global disturbances of the Earth’s magnetosphere using muon detectors

Amethod is developed, whichmakes it possible to predict in advance disturbances in the Earth’s magnetosphere, caused by solar flares or changes in the heliospheric magnetic field, since the cosmic particle flux reaches the Earth much earlier than coronal plasma bursts. To scan the celestial hemisphere, wide-aperture muon detectors are used. A unique system of muon hodoscopes was developed at the NEVOD Science and Education Center (MEPhI, Moscow). The data of the URAGAN muon hodoscope on two-dimensional dynamics of the muon flux during the Forbush effect of November 14, 2006 are analyzed. Changes in the muon flux intensity, measured at various directions with an interval of 30 min are shown. The results obtained demonstrate the muon flux sensitivity to solar plasma cloud motion, which offers prospects to use muon detectors to probe interplanetary space at long distances from the Earth and to predict geomagnetic disturbances.     

Studying variations of muon flux on the Earth’s surface,based on muon hodoscope data during nonstationary atmospheric processes

The first results are presented from the long-term experiment on registration of the response of the muon flux of cosmic rays to nonstationary atmospheric phenomena (storms) using the URAGAN muon hodoscope. The potential of the muon hodoscope enables us to register changes in the local anisotropy of the muon flux, the results from the analysis of which indicate the sensitivity of the penetrating component of cosmic rays to turbulent disturbances in the atmosphere during thunderstorms. Based on the analysis of 12 events in the Moscow region between May and September 2009, it is shown that the response of the muon flux is characteristic of the majority of thunderstorms, both in the general count rate and in the zenith-azimuthal distribution of intensity.     

Cosmic muon flux at shallow depths underground

The cosmic muon background has been calculated for facilities placed at shallow depths. A relatively simple formula has been proposed for the muon spectrum at sea level that ensures the calculation of the depth dependences of the vertical muon intensity and integral muon flux. Calculations show that the zenith-angle distribution of the muon flux density is almost unchanged for depths from 10 to 100 m of solid rock. The muon angular distributions are presented for all three possible cases of the arrangement of the instruments in measurements carried out on the ground and at shallow depths. It has been shown that, to eliminate the cosmic muon background, it is necessary to install an active cosmic ray shielding “umbrella” covering a zenith angle ? of no less than 80°.     

Observing high energy neutrons of solar origin using the TEMP muon hodoscope

A new method of searching for high-energy solar neutrons using the ground-based TEMP muon hodoscope with a high angular resolution of ∼1°–2° is considered. An excess in the muon flux (about four standard deviations) was observed during solar flare GLE 60 (April 15, 2001). A small excess in the permanent muon flux from the Sun (2.2σ) was also detected in the daytime over a period of 230 days upon daily 4-hour exposure.     

Detection of GLE of December 13, 2006, using the muon hodoscope

GLE of December 13, 2006, is analyzed based on the data of the muon hodoscope located at MEPhI (Moscow). The setup supermodules registered that the muon flux intensity started increasing at 0254 UTC. An increase at a maximum (0300 UTC) was 0.61 ± 0.09% (for the 10-min data), which is larger than six standard deviations. The detection of the muon flux in the hodoscope mode for the first time made it possible to obtain the two-dimensional images of an increase in the muon flux. A comparison of the muon hodoscope and neutron monitor data makes it possible to conclude that the muon event was caused by a highly collimated bunch of the solar proton fast component.     

Variations of neutrons and muons generated by cosmic rays in the atmosphere and in thunderstorm electric fields

We investigate the interrelation between cosmic rays (CRs) and the electric field of the Earth during thunderstorms established by various investigators. The data from simultaneous measurements by spectrograph of CRs and the electric field in Yakutsk are used. It is noted that in seven recorded events of prolonged (up to 9 hours) variations in the electric field by ±5 kV m⁻¹ and in one event of a one-hour increase in the field value up to +20 kV m⁻¹ the CR index rose substantially. During the thunderstorm of the latter event, the intensity of neutrons fell by a considerable 1%. At the same time, a drop of ∼0.3% was observed in the CR muon component. Such effects was not observed for higher energy muons.     

Meteorological effects in the intensity of muon groups

The data of the experimental study of cosmic ray muon groups using the DEKOR setup for the period of 2004–2007, during which significant changes in the intensity of groups at the Earth’s surface were detected, are analyzed. It was found that these variations are caused by variations of weather conditions (temperature and atmospheric pressure); barometric and temperature coefficients were determined. It turned out that magnitudes of these coefficients for muon groups are significantly higher than available values for singlemuons. Possible physicalmechanismof the effect is discussed. Since muon groups are formed at high altitudes (of the order of several kilometers), the detected effect can be used for monitoring air temperature variations in the upper troposphere.     

Muon diagnostics of the Earth’s atmosphere and magnetosphere

A method of distant monitoring of the Earth’s magnetosphere and atmosphere is described, which is based on the close correlation between the modulations in the flux of atmospheric muons detected at the Earth’s surface and the dynamic processes in the Earth’s magnetosphere and atmosphere and implies the use of large-area muon hodoscopes with high angular accuracy of muon detection. The results of the analysis of the experimental data obtained on the muon hodoscopes used at the Moscow Engineering Physics Institute show that muon detection at the Earth’s surface in the hodoscopic mode gives a qualitatively new information about the main sources of muon flux modulation.     

High-energy cosmic ray muons in the Earth’s atmosphere

We present the calculations of the atmospheric muon fluxes at energies 10–10⁷ GeV based on a numerical-analytical method for solving the hadron-nucleus cascade equations. It allows the non-power-law behavior of the primary cosmic ray (PCR) spectrum, the violation of Feynman scaling, and the growth of the total inelastic cross sections for hadron-nucleus collisions with increasing energy to be taken into account. The calculations have been performed for a wide class of hadron-nucleus interaction models using directly the PCR measurements made in the ATIC-2 and GAMMA experiments and the parameterizations of the primary spectrum based on a set of experiments. We study the dependence of atmospheric muon flux characteristics on the hadronic interaction model and the influence of uncertainties in the PCR spectrum and composition on the muon flux at sea level. Comparison of the calculated muon energy spectra at sea level with the data from a large number of experiments shows that the cross sections for hadron-nucleus interactions introduce the greatest uncertainty in the energy region that does not include the knee in the primary spectrum.     

Observation of heliospheric disturbances in the muon component of cosmic rays

The possibilities of using ground-based muon hodoscopes to study heliospheric disturbances are discussed. Mapping of the matrices of muon flux angular distributions recorded at the ground level in geocentric solar ecliptic coordinates with allowance for the asymptotic directions of primary protons of galactic cosmic rays makes it possible to observe the dynamics of heliospheric disturbances in the near-Earth space. Variations in some other characteristics of muon flux angular distributions are also analyzed.