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At least 595 records · Page 33
All sourcesNASA NTRSDOE OSTI
NASA NTRS1972

Yields of gamma rays emitted following capture of negative muons by Si28 and Mg24.

Measurement of the yields of specific final states excited in the capture of negative muons by Mg24 and Si28. The yields are compared with the cross sections for excitation of the analog states by 180 deg electron scattering and with the relative populations of levels produced by the decay of the giant-dipole-resonance states.

Miller, G. H.↗
NASA NTRS1972

Gamma-neutrino angular correlations in muon capture.

Using a high-resolution Ge(Li) spectrometer, it proved possible to observe several Doppler-broadened gamma-ray transitions in Al-28 excited by muon capture in Si-28. Several of these transitions are shown to be suitable for analysis in terms of angular correlations between the neutrino and a deexcitation nuclear gamma-ray. The observed transitions are interpreted in terms of gamma-neutrino correlation coefficients which are functions of the weak-interaction coupling constants.

Miller, G. H.↗
NASA NTRS1973

Muon capture rates on O-16 leading to bound states of N-16.

A low-energy spectrum of gamma-rays following muon capture in O-16 was obtained with a high-resolution 1 cu cm Ge(Li) detector. The graph of the spectrum shows the separation of contaminant peaks from the 120 keV N-16 line. It is pointed out that there is a large discrepancy between the capture rate obtained in the investigation and results reported by Deutsch et al. (1969).

Kane, F. R.↗
NASA NTRS1977

Analytic representation of the proton-proton and proton-nucleus cross-sections and its application to the sea-level spectrum and charge ratio of muons

We have calculated the sea-level differential muon momentum spectrum and their charge ratio from 1 GeV/c to 5000 GeV/c, using all of the available accelerator data. We find an excellent agreement between our calculation and the existing experimental data. We see no need, at present, to invoke any change either in the cosmic-ray chemical composition or in the nature of the hadron-nucleus interaction at hadron energies above 1500 GeV.

Badhwar, G. D.↗
NASA NTRS1978

Momentum spectra and charge ratio of muons as a function of zenith angles

A detailed calculation of both the sea-level muon momentum spectra and charge ratio at angles up to 79 deg shows excellent agreement with available experimental data in the 1-5000 GeV/c range. It shows that there is no need at present to invoke any change in the cosmic ray chemical composition, the proton and helium spectra, or the nature of the hadronic interaction from what is presently observed at proton energies up to about 1500 GeV. If scaling in the relevant energy range holds for hadrons of energies above about 1500 GeV, the present results suggest that the cosmic ray proton and helium spectrum above 100 GeV continues with the same spectral index of 2.75 up to at least about 10 TeV.

Badhwar, G. D.↗
NASA NTRS1985

The primary composition beyond 10 to the 5th power GeV as deduced from high energy hadrons and muons in air showers

Data obtained from a large set of air shower simulation calculations with use of highly refined hadronic interaction and shower simulation model are presented, in an attempt to solve the problem of primary chemical composition beyond 100,000 GeV total energy. It is rated that high energy hadrons in air showers offer a rather unique primary mass signature and show that the interpretation of high energy muon data is much more ambiguous. Predictions are compared with experimental data.

Grieder, P. K. F.↗
NASA NTRS1985

High-energy multiple muons and heavy primary cosmic-rays

Three-dimensional simulations were carried out on high-energy multiple muons. On the lateral spread, the comparison with the deep underground observations indicates that the primary cosmic rays include heavy nuclei of high content. A method to determine the average mass number of primary particles in the energy around 10 to the 15th power eV is suggested.

Mizutani, K.↗
NASA NTRS1985

Atmospheric effects on the underground muon intensity

It has previously been reported that the barometric pressure coefficient observed for muons at Poatina (vertical absorber depth 357 hg/sq cm) appears to be appreciably higher than would be expected from atmospheric absorption alone. There is a possibility that the effect is due to an upper atmospheric temperature effect arising from an inverse correlation of surface pressure with stratospheric temperature. A new proportional telescope is discussed which has been operating at Poatina since about the beginning of 83 and which has a long term stability suitable for studying variations of atmospheric origin.

Fenton, A. G.↗
NASA NTRS1985

Muon spectrum in air showers initiated by gamma rays

An analytic representation for the invariant cross-section for the production of charged pions in gamma P interactions was derived by using the available cross-sections. Using this the abundance of muons in a gamma ray initiated air shower is calculated.

Stephens, S. A.↗
NASA NTRS1985

A note on some statistical properties of rise time parameters used in muon arrival time measurements

Most investigations of the muon arrival time distribution in EAS during the past decade made use of parameters which can collectively be called rise time parameters. The rise time parameter T sub A/B is defined as the time taken for the integrated pulse from a detector to rise from A% to B% of its full amplitude. The use of these parameters are usually restricted to the determination of the radial dependence thereof. This radial dependence of the rise time parameters are usually taken as a signature of the particle interaction characteristics in the shower. As these parameters have a stochastic nature, it seems reasonable that one should also take notice of this aspect of the rise time parameters. A statistical approach to rise time parameters is presented.

Vanderwalt, D. J.↗