Observations of Slow Particles and Stars in Nuclear Emulsions Exposed at 17 m.w.e. Underground

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概要

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• Observations were carried out at a depth of 17 m.w.e. underground by nuclear plates made from llford G5 emulsions in gel form. The frequencies of μ-mesons and protons coming to rest in the emulsions were found to be 0.262±0.008cm^<-3>day^<-1> and 0.049±0.004cm^<-3>day^<-1>, respectively. The angular distribution of these slow protons was found to be isotropic and so they are regarded as being of secondary origin from fast μ-mesons unclerground. In addition to the stars of the types of N_p+1_p with N_p > 3, several stars of the types of 1+1_p and 2+1_p were found with a cross section for production of a few times 10^<-30>cm^2 per nucleon. Some of the stars of the type of 1+1_p may possibly be explained by photoproton production through the giant resonance absorption by emulsion nuclei of virtual photons associated with high energy μ-mesons.

• 社団法人日本物理学会の論文
• 1955-08-05

著者

• Kaneko Shin-ichi

  Institute Of Polytechnics Osaka City University

• Kubozoe Tadayoshi

  Institute Of Polytechnics Osaka City University

• Takahata Masaomi

  Institute Of Polytechnics Osaka City University

• OKAZAKI Moroe

  Institute of Polytechnics, Osaka City University

• Okazaki Moroe

  Institute Of Polytechnics Osaka City University

• Kubozoe Tadayoshi

  Institute of Polytechnics, Osaka City University

関連論文

• Intensities of Low Energy μ-Mesons and N-Component near Sea Level at 24°N
• Observations of Slow Particles and Stars in Nuclear Emulsions Exposed at 17 m.w.e. Underground
• The Non-Mesonic Photonuclear Reactions Initiated by High Energy μ-Mesons
• Frequency of Slow Cosmic-ray μ-Mesons Stopped in the Photographic Emulsions at 23 m.w.e. Underground
• Observation of the High-Energy Proton-Proton Collision in Photographic Emulsion
• The Multiplicity of Mesons Produced in the Nuclear Interaction of High Energy Nucleons and α-Particles in Cosmic Radiation
• A Calibration Measurement of Multiple Scattering of Slow μ-Mesons by the Constant Sagitta Method

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