Temperature Effect Observed for the Muon Component in the Yakutsk Cosmic-Ray Spectrograph

Berkova, M. D.; Grigoryev, Vladislav; Preobrazhensky, Maxim; Zverev, Anton; Yanke, V. G.

doi:10.1134/s1063778818050046

Cited by 8 publications

(4 citation statements)

References 8 publications

Supporting

Mentioning

Contrasting

Unclassified

Order By: Relevance

“…To remove this variability, for example, the parameter; G=(30 • N-30 • S)+(30 • N-30 • E) has been introduced, and data analysis has been carried out [5]. Berkova et al have also proposed to correct the Nagoya muon data for temperature variations in cosmic ray muon flux from meteorological data [6]. Note that the instruments themselves are in the thermostatic chamber and the temperature variation with respect to the trigger rate is negligible.…”

Section: Data Of the Nagoya Muon Telescopementioning

confidence: 99%

The 48 year data analysis of Nagoya muon telescope - Discovery of (125+-45) day periodicity

Muraki¹

2023

Proceedings of 38th International Cosmic Ray Conference — PoS(ICRC2023)

View full text Add to dashboard Cite

show abstract

Section: Data Of the Nagoya Muon Telescopementioning

confidence: 99%

The 48 year data analysis of Nagoya muon telescope - Discovery of (125+-45) day periodicity

Muraki¹

2023

Proceedings of 38th International Cosmic Ray Conference — PoS(ICRC2023)

View full text Add to dashboard Cite

show abstract

“…To remove this variability, for example, the parameter G = (30 • N-30 • S) + (30 • N-30 • E) has been introduced, and data analysis has been carried out [7]. Berkova et al (2016) have proposed to correct the Nagoya muon data for temperature variations in cosmic ray muon flux from meteorological data [8]. However, sometimes the atmospheric temperature of the lower layer differs from the variation in the upper layer (the stratosphere).…”

Section: Data Of the Nagoya Multi-directional Cosmic Ray Telescopementioning

confidence: 99%

The 48-Year Data Analysis Collected by Nagoya Muon Telescope—A Detection of Possible (125 ± 45) Day Periodicity

Muraki,

Shibata,

Takamaru

et al. 2023

Universe

View full text Add to dashboard Cite

Muons produced by cosmic rays above the atmosphere provide valuable information on the intensity of cosmic rays and variations in the upper atmosphere. Since 1970, the Nagoya University Cosmic Ray Laboratory has been observing the muon intensity using a multi-directional cosmic ray telescope with two layers of 36 plastic scintillators of 1m2 each, which measure the muon intensity in different incident directions. The energy of an incident proton that produces a muon incident from a vertical direction is over 11.5 GV. This paper analyzes vertical muon intensities obtained over 48 years from 1970 to 2018 using methods that differ from the East–West method. As a result, a new periodicity of (125±45) days and a new periodicity of (4–16) days were found. The latter appears only in winter time, so it may be caused by a synoptic-scale disturbance associated with the arrival of the Siberian cold air mass. On the other hand, the former periodicity may be related to solar dynamo activity. In 1984, the Solar Maximum Mission’s Gamma Ray Spectrometers reported a periodicity of about (154±10) days in the flux of solar gamma rays. The (125±45)-day periodicity found here is most likely related to solar dynamo activity, since the intensity of cosmic rays around 11.5 GV is affected by the magnetic field induced by the Sun. However, this (125±45)-day periodicity differs from the report measured by the GRS instrument in a point that it also appears during periods of low solar activity. Furthermore, it has not appeared often during lower solar activity since 1992. This information is important for future investigation of the origin of this periodicity.

show abstract

“…Porém, estes estão à distâncias maiores da superfície terrestre, logo, para que consigam chegar ao solo, eles precisam percorrer distancias maiores, o que implica em uma probabilidade maior de decaimento desses múons. Assim, na superfície terrestre, o número total dessas partículas detectadas vai ser menor com o aumento da temperatura, resultando em um coeficiente de temperatura negativo (15) (12). Se forem analisados apenas os múons mais energéticos, aqueles que podem ser detectados em experimentos underground, acontece o inverso: como mais múons de todas as energias foram gerados na atmosfera, mais múons com maiores energias foram produzidos.…”

Section: Dependência Com Efeitos Atmosféricosunclassified

“…Tal diferença se deve às diferentes altitudes onde os experimentos foram realizados, ao fato de que em Campinas estamos numa região de anomalia geomagnética e que as temperaturas sob as quais os dados foram coletados foram completamente distintas. Numa tentativa de correção devido à temperatura, foi utilizado um coeficiente de temperatura resultado do experimento realizado em Buckland Park (15)…”

Section: Medidas Para Comparaçõesunclassified

Medidas de intensidade de múons cósmicos com cintiladores plásticos

Nunes¹

View full text Add to dashboard Cite

The study of cosmic radiation is of utmost importance to astrophysics. Particles from different locations, from inside the solar system, and outside it, constantly arrive on Earth, carrying a lot of information about its origin. When these particles arrives to Earth's atmosphere they initiate a cascade of secondary particles resulting from the interaction of the primary cosmic ray with the atmosphere. From this rain of secondary particles, muons are the most abundant charged particles that reach the Earth's surface. Muons are highly penetrating, which can be a very big problem in some experiments, even if underground, of other particles. Because of their large number, they become extremely necessary in reconstructions of air showers to obtain information about the primary particle. Having knowledge of its characteristics, such as flux and distribution, noise in some experiments can be treated and other studies can be optimized. Muon intensity in the Earth's surface is well known to be anisotropic and has dependence on the zenith angle of I(◊)=I 0 cos n (◊). For simplicity in the calculations, this n exponent is often used with a value of 2, but studies show that this parameter has dependence on the geographical position and on the energy range of muons in question. This dissertation proposes a simple method for accurate determination of the exponent n and muon vertical intensity simultaneously, that can be determined quickly in any laboratory cosmic rays using a particle detector, which was called Muon Telescope. As a result of the application of the method on the Leptons Laboratory, in Campinas -SP -Brazil, the value for n that was obtained is about 2.30 and a value for the vertical intensity of muons around 146.40Hz/m 2 sr. This data is very satisfactory and according to similar experiments previously conducted at the Laboratory. This method was applied on Fermilab, located at the United States. On this new geographical location, the results were different from that obtained at Campinas, with n about 3.66 and the vertical intensity around 158.33 Hzm ≠2 sr ≠1 . The same experiment with the telescope will be held in other geographical locations in order to check the n exponent behavior and the muon intensity at different locations.

show abstract

Temperature Effect Observed for the Muon Component in the Yakutsk Cosmic-Ray Spectrograph

Cited by 8 publications

References 8 publications

The 48 year data analysis of Nagoya muon telescope - Discovery of (125+-45) day periodicity

The 48 year data analysis of Nagoya muon telescope - Discovery of (125+-45) day periodicity

The 48-Year Data Analysis Collected by Nagoya Muon Telescope—A Detection of Possible (125 ± 45) Day Periodicity

Medidas de intensidade de múons cósmicos com cintiladores plásticos

Contact Info

Product

Resources

About