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°.     

The extraterrestrial neutrino flux sensitivity of underground and undersea muon detectors

Summary The sensitivity of underground and undersea muon detectors to point sources of extraterrestrial neutrinos with power law spectra is calculated from very general considerations. It is shown that this sensitivity depends critically on the spectral slope, but is essentially independent of the muon energy threshold of the instrument out to 100 GeV. Sources with a neutrino flux comparable to the γ-ray flux from Cygnus X-3 would not be detectable underground, and are only marginally detectable by the proposed large undersea experiment, DUMAND. However, fluxes perhaps 100 times higher are possible and these would be marginally detectable underground with MACRO or in the proposed DUMAND Stage II detector, the TRIAD.

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Riassunto Si calcola la sensibilità dei rivelatori muonici sotto terra e sott'acqua a sorgenti puntiformi di neutrini extraterrestri con spettri a legge di potenza partendo da considerazioni molto generali. Si mostra che questa sensibilità dipende in modo critico dalla pendenza dello spettro ma è sostanzialmente indipendente dalla soglia d'energia muonica dello strumento fino a 100 GeV. Sorgenti con un flusso di neutrini confrontabili con il flusso di raggi γ da Cygnus X-3 non sarebbero individuabili sottoterra e sono solo marginalmente rilevabili con il grande esperimento sott'acqua DUMAND proposto. Comunque flussi forse 100 volte maggiori sono possibili e questi sarebbero marginalmente rilevabili sottoterra con MACRO o nel rivelatore proposto DUMAND del secondo stadio, il TRIAD.

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Резюме Из очень общих рассуждений вычисляется чувствительность подземных и подводных мюонных детекторов к точечным источникам внеземных нейтрино со степенными спектрами. Показываэтся, что эта чувствительность очень сильно зависит от наклода спектра, но по существу не зависит от мюонного энергетического порога прибора вне 100 ГэВ. Источники с нейтринным потоком, сравнимым с потоком ч-лучей от Лебедь X-3, не могут быть зарегистрированы подземными детекторами и не являются маргинально детектируемыми с помощью предложенного крупного подводного эксперимента ДОМАНД. Однако потоки, в 100 раз большие, оказываются возможными и могли бы быть маргинально зарегистрированы подземными детекторами, тогда как в эксперименте ДОМАНД они производят слишком большпй сигнал.

     

Role of reduced flux values in muon radiography

A numerical experiment clearly shows that the use of reduced fluxes makes it possible to eliminate the effect of the shape of the object under study on the estimate of its material density by muon radiography methods.     

Atmospheric neutrino flux supported by recent muon experiments

We present a new one-dimensional calculation of low and intermediate energy atmospheric muon and neutrino fluxes, using up-to-date data on primary cosmic rays and hadronic interactions. We study several sources of uncertainties relevant to our calculations. A comparison with the muon fluxes and charge ratios measured in several modern balloon-borne experiments suggests that the atmospheric neutrino flux is essentially lower than one used for the standard analyses of the sub-GeV and multi-GeV neutrino induced events in underground detectors.     

Specific features of studying Forbush decreases in the muon flux

The variations in the cosmic ray (CR) muon flux during the Forbush decreases (FDs), registered by the DECOR muon detector and the URAGAN muon hodoscope during the periods of their operation from 2004 to 2006, are analyzed. The unified method for determining the parameters of variations in the CR flux during FDs has been developed, and the dependences of the FD characteristics on the rigidity of primary CRs and information about the spatial-angular dynamics of the muon flux during FDs have been obtained.     

Atmospheric effects on cosmic-ray muon intensities at deep underground depths

Summary On the basis of the theoretical calculation of the atmospheric effect on the cosmic-ray muon intensity, it is demonstrated that the following two anomalous facts recently reported from muon observations at deep underground stations can be attributed to the atmospheric-temperature effect. One is the remarkable dependence of the muon intensity on the atmospheric pressure observed at Poatina (365 m w.e. in depth) and Matsushiro (250 m w.e. in depth), which is contradictory to theoretical expectations, and the other is the semi-annual variation in the muon intensity at Matsushiro, which exhibits a striking contrast to annual variations usually observed at underground stations shallower than Matsushiro. In the present paper, the barometer coefficient and the partial temperature coefficient are also provided for various combinations of parameters such as the muon threshold energy and the zenith angle to meet any requirement of observations.

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Riassunto Sulla base del calcolo teorico dell'effetto atmosferico sull'intensità dei muoni dei raggi cosmici, si dimostra che due fatti anomali riportati recentemente riguardanti osservazioni muoniche in stazioni a grande profondità si possono attribuire all'effetto della temperatura atmosferica. Uno è la notevole dipendenza dell'intensità muonica dalla pressione atmosferica osservata a Poatina (365 m w.e. di profondità) e Matsushiro (250 m w.e. di profondità), che è in contraddizione con previsioni teoriche, e l'altro è la variazione semiannuale nell'intensità muonica a Matsushiro, che mostra un contrasto stridente con le variazioni annuali osservate solitamente in stazioni sotterranee meno in profondità di Matsushiro. In questo lavoro si forniscono il coefficiente barometrico e il coefficiente parziale di temperatura per varie combinazioni di parametri come l'energia di soglia muonica e l'angolo zenitale per soddisfare ogni esigenza di osservazione.

     

Seasonal variations of the muon flux in the MUSTANG super telescope data

The temperature effect of the muon cosmic ray (CR) component is studied using the MUSTANG super telescope data (Greifswald, Germany) from 2007 throughout its period of operation. The original hourly data obtained with the telescope are adjusted for the temperature effect using a vertical atmospheric temperature profile at standard isobaric levels derived from the Global Forecast System (GFS) model. The model’s accuracy and applicability is evaluated using atmospheric sounding data collected over a number of years.     

Search for UHE cosmic sources with a large-area underground muon detector

Summary The newly discovered gamma-ray emission from Cyg-X 3 with energies up to 2·10¹⁶eV gives the first evidence that particle acceleration in galactic gamma-ray sources can reach energies of the order of 10⁴ TeV. We discuss the detectability of this type of sources by an underground muon tracking detector with area of the order of ∼1000 m² and the physical information which could be obtained in this way. Paper presented at the 2° Convegno Nazionale di Fisica Cosmica, held at L'Aquila, 29 May–2 June 1984.     

Hyperfine field calculations: Search for muon stopping sites in Fe3O4

Muon Spin Rotation (SR) results for magnetite (Fe₃O₄) are analyzed and discussed. At room temperature, a SR signal is observed due to the presence of an internal magnetic field (B_int) at the muon site. External transverse field measurements show that B_int is parallel to the magnetic spin direction, the <111> direction in zero applied field. Calculations of the hyperfine field to pinpoint muon stopping sites in magnetite show that the local field contains supertransfer (covalent) and dipolar field contributions. The implanted muons appear to stop at sites structurally similar to those reported for hematite (-Fe₃O₄), where muon-oxygen bond formation was strongly indicated.Research partially supported by US Department of Energy     

Analysis of the anisotropy of the muon flux, according to data obtained by the URAGAN muon hodoscope during heliospheric disturbances

Features of studying heliospheric disturbances caused by changes in the parameters of the interplanetary magnetic field by the anisotropy of the muon flux of cosmic rays detected on the surface of the Earth by the URAGAN muon hodoscope are considered. The anisotropy of the muon flux in the period 2007–2011 is analyzed. The forecasting potential of our approaches to studying heliospheric disturbances using the penetrating component of cosmic rays is evaluated.     

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对ITER中子通量监测器(NFM)建立了简化模型并进行了计算分析。利用MCNP程序模拟计算了具有不同慢化剂材料/类型的NFM的探测效率能量响应和时间响应,通过对结果的分析确定了不同NFM上所使用的慢化剂种类及其用量,同时给出了对ITER NFM的初步物理认识。     

Measurement of cosmic ray flux in the China JinPing underground laboratory

The China JinPing underground Laboratory (CJPL) is the deepest underground laboratory running in the world at present. In such a deep underground laboratory, the cosmic ray flux is a very important and necessary parameter for rare-event experiments. A plastic scintillator telescope system has been set up to measure the cosmic ray flux. The performance of the telescope system has been studied using the cosmic rays on the ground laboratory near the CJPL. Based on the underground experimental data taken from November 2010 to December 2011 in the CJPL, which has an effective live time of 171 days, the cosmic ray muon flux in the CJPL is measured to be (2.0±0.4)×10-10/(cm2 ·s). The ultra-low cosmic ray background guarantees an ideal environment for dark matter experiments at the CJPL.     

Derivation of muon range spectrum at different polar angles in deep underground from primary nucleon spectrum

Summary The energy spectra of sea-level muons at different zenith angles have been estimated from the latest JACEE primary spectrum using ISR results modified for p-nucleus interactions. The theoretical results have been compared with the experimental results. Using the recent modified range-energy relation after Kobayakawa along with the fluctuation correction procedure after Kiraly, Kiraly and Osborne, the muon range spectra in deep underground at different polar angles have been calculated. The derived results are well in agreement with the latest Mont Blanc data after Bergamascoet al., Battistoniet al. and Utah experiments after Bergessonet al.

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Riassunto Si stimano gli spettri d'energia muonica a livello del mare a differenti angoll zenitali dal piú recente spettro delle primarie JACEE usando risultati ISR modificati per interzioni p-nucleo. I risultati teorici sono stati confrontati con i risultati sperimentali. Usando la recente relazione modificata intervallo-energia di Kobayakawa oltre alla procedura di correzione delle fluttuazioni di Kiraly, Kiraly e Osborne sono stati calcolati gli spettri dell'intervallo muonico in profondità per differenti angolia polari. I risultati derivati sono in buon accordo con i dati piú recenti del Monte Bianco di Bergamascoet al., Battistoniet al. e gli esperimenti Utah di Bergessonet al.

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Резюме Оцениваются энергетические спектры мюонов на уровне моря длл различных зенутных углов, исходя из последнего JACEE первичного спектра с использованием ISR-результатов, модифицированных для протон-ядерных взаим действий. Теоретические результаты сравниваются с экспериментальными данным Используя недавнее модифицированное соотношение между пробегом и энергиек Кобайакавы и методику Кирали, Кирали и Осборна для флуктуационных поправок вычисляются спектры пробегов мюонов под землей для различных полярных углов. Полученные резулятаты хорошо согласуются с последними данными под Мон-Бланом и с результатами Юта-экспериментов.

     

The microscopic investigation of structures of moving flux lines by neutron and muon techniques

We have used a variety of microscopic techniques to reveal the structure and motion of flux line arrangements, when the flux lines in low T _c type II superconductors are caused to move by a transport current. Using small-angle neutron scattering by the flux line lattice (FLL), we are able to demonstrate directly the alignment by motion of the nearest-neighbor FLL direction. This tends to be parallel to the direction of flux line motion, as had been suspected from two-dimensional simulations. We also see the destruction of the ordered FLL by plastic flow and the bending of flux lines. Another technique that our collaboration has employed is the direct measurement of flux line motion, using the ultra-high-resolution spectroscopy of the neutron spin-echo technique to observe the energy change of neutrons diffracted by moving flux lines. The muon spin rotation (μSR) technique gives the distribution of values of magnetic field within the FLL. We have recently succeeded in performing μSR measurements while the FLL is moving. Such measurements give complementary information about the local speed and orientation of the FLL motion. We conclude by discussing the possible application of this technique to thin film superconductors.     

Quadrature effects on the accuracy of flux calculations in realistic atmospheres

We have investigated the accuracy of five different quadrature methods—equal steps in θ, equal steps in cos θ, Gaussian, double Gaussian and Gauss-Lobatto—on the accuracy of fluxes in realistic aerosol atmospheres, using the Gauss-Seidel method. In addition, a range of Gaussian quadrature stream numbers from two to 32 were compared. The atmospheric models considered are those recently presented by Lenoble, with the exception that we have used Henyey-Greenstein phase functions in place of Mie. Our results should be easily reproduceable by any other workers interested in similar realistic atmospheres. A table of Gauss-Lobatto weights and points is provided as an appendix.     

Sea-level muon spectrum in the energy range 1–10 TeV from the data of underground experiments

Within an adjoint approach, the properties of the muon component in various types of rock and in water are calculated with allowance for fluctuations of energy losses in all muon-interaction processes. The behavior of the muon spectrum at sea level is established on the basis of a comparison of the muonabsorption curves obtained in this way and experimental data from underground facilities. It is shown that the deficit of the calculated muon flux obtained with the aid of data from direct measurements of the spectra of primary nuclei and Reggeon models of nuclear interactions is not less than 50% in the energy range 1–10 TeV.     

Possibility of hgh Z material detection by a setup for natural cosmic-ray muon flux measurement

A design is proposed and a resolving power is calculated for a detector that monitors the unauthorized transportation of high Z materials (nuclear materials with Z > 90) using the natural cosmic-ray muon flux. The identification of nuclear materials is based on the strong dependence of the multiple scattering angle on the matter charge upon traversing the matter by cosmic muons. It is proposed that chambers assembled from drift aluminum tubes similar to chambers used in the muon system of the ATLAS detector be used as the coordinate detector for the setup. The calculations show that the proposed variant of the setup makes it possible to detect the presence of nuclear materials with a weight of about 0.5–1 kg and higher in the inspected volume in a measurement time of several minutes.     

A note on vector flux models for radiation dose calculations

This paper reviews and extends modelling of anisotropic fluxes for radiation belt protons to provide closed-form equations for vector proton fluxes and proton flux anisotropy in terms of standard omnidirectional flux models. These equations provide a flexible alternative to the data-based vector flux models currently available. At higher energies, anisotropy of trapped proton flux in the upper atmosphere depends strongly on the variation of atmospheric density with altitude. Calculations of proton flux anisotropies using present models require specification of the average atmospheric density along trapped particle trajectories and its variation with mirror point altitude. For an isothermal atmosphere, calculations show that in a dipole magnetic field, the scale height of this trajectory-averaged density closely approximates the scale height of the atmosphere at the mirror point of the trapped particle. However, for the earth's magnetic field, the altitudes of mirror points vary for protons drifting in longitude. This results in a small increase in longitude-averaged scale heights compared to the atmospheric scale heights at minimum mirror point altitudes. The trajectory-averaged scale heights are increased by about 10-20% over scale heights from standard atmosphere models for protons mirroring at altitudes less than 500 km in the South Atlantic Anomaly. Atmospheric losses of protons in the geomagnetic field minimum in the South Atlantic Anomaly control proton flux anisotropies of interest for radiation studies in low earth orbit. Standard atmosphere models provide corrections for diurnal, seasonal and solar activity-driven variations. Thus, determination of an "equilibrium" model of trapped proton fluxes of a given energy requires using a scale height that is time-averaged over the lifetime of the protons. The trajectory-averaged atmospheric densities calculated here lead to estimates for trapped proton lifetimes. These lifetimes provide appropriate time-averaging intervals for equilibrium models of trapped proton fluxes.