Determination of density of temperature coefficients for the Earth’s atmosphere muons

When studying variations of cosmic ray intensity, by the use of muon telescopes located deep in the atmosphere it is necessary to take into account changes in atmospheric parameters, mainly pressure and temperature. The density distribution of temperature coefficients of the atmosphere muon intensity needs to be estimated from observations. To this purpose, the method of principal components regression and meth-ods of projection to latent structures (PLS-1 and PLS-2). We used data of continuous recording of muons, as well as Novosibirsk 2004–2010 aerological data. As shown by comparing results, PLS-2 method allows us to esti-mate the density distribution of muon intensity temperature coefficients with minimal errors.

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Distribution of temperature coefficient density for muons in the atmosphere

Solar-Terrestrial Physics ◽

10.12737/stp-34201710 ◽

2017 ◽

Vol 3 (4) ◽

pp. 93-102 ◽

Cited By ~ 2

Author(s):

Василий Кузьменко ◽

Vasiliy Kuzmenko ◽

Валерий Янчуковский ◽

Valery Yanchukovsky

Keyword(s):

Temperature Coefficient ◽

Sea Level ◽

Cosmic Ray ◽

Cosmic Ray Intensity ◽

Temperature Coefficients ◽

Specific Geometry ◽

Muon Intensity

To date, several dozens of new muon detectors have been built. When studying cosmic-ray intensity variations with these detectors, located deep in the atmosphere, it is necessary to calculate all character-istics, including the distribution of temperature coeffi-cient density for muons in the atmosphere, taking into account their specific geometry. For this purpose, we calculate the density of temperature coefficients of muon intensity in the atmosphere at various zenith angles of detection at sea level and at various depths underground for different absorption ranges of primary protons and pions in the atmosphere.

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Distribution of temperature coefficient density for muons in the atmosphere

Solnechno-Zemnaya Fizika ◽

10.12737/szf-34201710 ◽

2017 ◽

Vol 3 (4) ◽

pp. 104-116

Author(s):

Василий Кузьменко ◽

Vasiliy Kuzmenko ◽

Валерий Янчуковский ◽

Valery Yanchukovsky

Keyword(s):

Temperature Coefficient ◽

Sea Level ◽

Cosmic Ray ◽

Cosmic Ray Intensity ◽

Temperature Coefficients ◽

Specific Geometry ◽

Muon Intensity

To date, several dozens of new muon detectors have been built. When studying variations in cosmic-ray intensity with these detectors, located deep in the atmosphere, it is necessary to calculate all characteristics, including the distribution of temperature coefficient density for muons in the atmosphere, taking into account their specific geometry. For this purpose, we calculate the density of temperature coefficients of muon intensity in the atmosphere at various zenith angles of detection at sea level and at various depths underground for different absorption ranges of primary protons and pions in the atmosphere.

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Determination of Pyridostigmine Bromide in Presence of its Related Impurities by Four Modified Classical Least Square Based Models: A Comparative Study

Current Pharmaceutical Analysis ◽

10.2174/1573412915666190715094347 ◽

2020 ◽

Vol 17 (1) ◽

pp. 87-94

Author(s):

Ibrahim A. Naguib ◽

Fatma F. Abdallah ◽

Aml A. Emam ◽

Eglal A. Abdelaleem

Keyword(s):

Comparative Study ◽

Least Squares ◽

Orthogonal Projection ◽

Predictive Ability ◽

Least Square ◽

Projection To Latent Structures ◽

Preprocessing Method ◽

Spectral Residual ◽

Latent Structures

: Quantitative determination of pyridostigmine bromide in the presence of its two related substances; impurity A and impurity B was considered as a case study to construct the comparison. Introduction: Novel manipulations of the well-known classical least squares multivariate calibration model were explained in detail as a comparative analytical study in this research work. In addition to the application of plain classical least squares model, two preprocessing steps were tried, where prior to modeling with classical least squares, first derivatization and orthogonal projection to latent structures were applied to produce two novel manipulations of the classical least square-based model. Moreover, spectral residual augmented classical least squares model is included in the present comparative study. Methods: 3 factor 4 level design was implemented constructing a training set of 16 mixtures with different concentrations of the studied components. To investigate the predictive ability of the studied models; a test set consisting of 9 mixtures was constructed. Results: The key performance indicator of this comparative study was the root mean square error of prediction for the independent test set mixtures, where it was found 1.367 when classical least squares applied with no preprocessing method, 1.352 when first derivative data was implemented, 0.2100 when orthogonal projection to latent structures preprocessing method was applied and 0.2747 when spectral residual augmented classical least squares was performed. Conclusion: Coupling of classical least squares model with orthogonal projection to latent structures preprocessing method produced significant improvement of the predictive ability of it.

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Deriving the solar activity cycle modulation on cosmic ray intensity observed by Nagoya muon detector from October 1970 until December 2012

Proceedings of the International Astronomical Union ◽

10.1017/s1743921317003763 ◽

2016 ◽

Vol 12 (S328) ◽

pp. 130-133 ◽

Cited By ~ 1

Author(s):

Rafael R. S. de Mendonça ◽

Carlos. R. Braga ◽

Ezequiel Echer ◽

Alisson Dal Lago ◽

Marlos Rockenbach ◽

...

Keyword(s):

Solar Activity ◽

Cosmic Ray ◽

Activity Cycle ◽

Solar Activity Cycle ◽

Atmospheric Temperature ◽

Muon Detector ◽

Natural Phenomena ◽

Cosmic Ray Intensity ◽

Temperature Changes ◽

Muon Intensity

AbstractIt is well known that the cosmic ray intensity observed at the Earth's surface presents an 11 and 22-yr variations associated with the solar activity cycle. However, the observation and analysis of this modulation through ground muon detectors datahave been difficult due to the temperature effect. Furthermore, instrumental changes or temporary problems may difficult the analysis of these variations. In this work, we analyze the cosmic ray intensity observed since October 1970 until December 2012 by the Nagoya muon detector. We show the results obtained after analyzing all discontinuities and gaps present in this data and removing changes not related to natural phenomena. We also show the results found using the mass weighted method for eliminate the influence of atmospheric temperature changes on muon intensity observed at ground. As a preliminary result of our analyses, we show the solar cycle modulation in the muon intensity observed for more than 40 years.

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Experimental determination of the muon range–energy relation

Canadian Journal of Physics ◽

10.1139/p68-240 ◽

1968 ◽

Vol 46 (10) ◽

pp. S332-S336 ◽

Cited By ~ 2

Author(s):

W. R. Sheldon ◽

N. M. Duller

Keyword(s):

Experimental Determination ◽

Cosmic Ray ◽

Energy Relation ◽

Attenuation Length ◽

Independent Evaluation ◽

Absolute Measurements ◽

Muon Intensity ◽

Spectrometer Data ◽

Peak Value

Calculations of the zenithal distribution of cosmic-ray muons indicate the appearance of peaks at near-horizontal directions in the relative muon intensity I(θ)/I0 for Eμ > a few tens of GeV. The magnitude of the peak value of I(θ)/I0 increases monotonically with energy, representative values being 1.15 for Eμ > 50 GeV and 1.58 for Eμ > 120 GeV. Using this phenomenon, an independent evaluation can be made of the muon range–energy relation. Absolute measurements of the muon flux underground at zenith angles of 69° to 77° are compared to the calculated zenithal distribution to determine the muon range–energy relation in rock at 25–100 GeV. Suggestions are advanced for extending the energy range to a few thousand GeV and for making a purely experimental determination by utilizing magnetic spectrometer results in a context which would avoid the need to normalize the spectrometer data and would largely eliminate the problem of possible energy bias. The usefulness of these data in determining the pion attenuation length in the atmosphere is discussed.

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