Measurements of Meson Masses and Related Quantities

Smith, Frances M.; Birnbaum, W.; Barkas, Walter H.

doi:10.1103/physrev.91.765

Cited by 91 publications

(21 citation statements)

References 2 publications

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“…Calculations by Jackson and McCarthy [27] confirmed that negative particles lose energy at a slower rate, with the difference dropping from tens of percent at MeV energies to about 0.3% in the GeV range. These calculations were subsequently verified experimentally both at MeV energies [28,29,30] and in the GeV range [31]. The approximations used in [27], however, break down when going to even higher energies and so more exact numerical methods are needed.…”

Section: Discussionmentioning

confidence: 89%

Measurement of the atmospheric muon charge ratio at TeV energies with the MINOS detector

Adamson¹,

Andreopoulos²,

Arms³

et al. 2007

Phys. Rev. D

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The 5.4 kton MINOS far detector has been taking charge-separated cosmic ray muon data since the beginning of August, 2003 at a depth of 2070 meters-water-equivalent in the Soudan Underground Laboratory, Minnesota, USA. The data with both forward and reversed magnetic field running configurations were combined to minimize systematic errors in the determination of the underground muon charge ratio. When averaged, two independent analyses find the charge ratio underground to be N µ + /N µ − = 1.374 ± 0.004 (stat.) +0.012−0.010 (sys.). Using the map of the Soudan rock overburden, the muon momenta as measured underground were projected to the corresponding values at the surface in the energy range 1-7 TeV. Within this range of energies at the surface, the MINOS data are consistent with the charge ratio being energy independent at the two standard deviation level. When the MINOS results are compared with measurements at lower energies, a clear rise in the charge ratio in the energy range 0.3 -1.0 TeV is apparent. A qualitative model shows that the rise is consistent with an increasing contribution of kaon decays to the muon charge ratio.

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Section: Discussionmentioning

confidence: 89%

Measurement of the atmospheric muon charge ratio at TeV energies with the MINOS detector

Adamson¹,

Andreopoulos²,

Arms³

et al. 2007

Phys. Rev. D

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“…Above the cavern hall lies 72.1 m of Dolomite/Shale bedrock with a density of 2.41 g/cm 3 , followed by 22.2 m of Glacial till with a density of 2.29 g/cm 3 . It has been suggested in [7] that at the MINOS Near Detector depth the slightly higher rate of energy loss of µ + over µ − [25][26][27][28][29][30] could lead to a surface charge ratio that is slightly higher than that observed underground. However, as the magnitude of this effect is negligible when compared to the systematic uncertainties of this measurement we have assumed the same energy loss function for both charges.…”

Section: The Atmospheric Muon Charge Ratio At the Surfacementioning

confidence: 99%

Measurement of the underground atmospheric muon charge ratio using the MINOS Near Detector

Adamson¹,

Andreopoulos²,

Auty³

et al. 2011

Phys. Rev. D

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The magnetized MINOS Near Detector, at a depth of 225 meters of water equivalent (mwe), is used to measure the atmospheric muon charge ratio. The ratio of observed positive to negative 2 atmospheric muon rates, using 301 days of data, is measured to be 1.266 ± 0.001(stat.) +0.015 −0.014 (syst.). This measurement is consistent with previous results from other shallow underground detectors, and is 0.108 ± 0.019(stat. + syst.) lower than the measurement at the functionally identical MINOS Far Detector at a depth of 2070 mwe. This increase in charge ratio as a function of depth is consistent with an increase in the fraction of muons arising from kaon decay for increasing muon surface energies.PACS numbers: 13.85. Tp. 95.55.Vj, 95.85.Ry

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“…When possible, these charge-sign-dependent effects provide a key test of our understanding. The first indications of such a dependence came from the work of Barkas and coworkers [6], who observed different ranges for positive and negative pions in matter. Initially this observation was attributed to a difference in the pion masses, but latter it was demonstrated that it is due to higher-order contributions to the energy loss rate or stopping power [7,8].…”

Section: Introductionmentioning

confidence: 99%

Exploring the Barkas effect with keV-electron scattering

Grande

Vos

2013

Phys. Rev. A

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The energy loss of fast ions at close collision is mainly due to electron-ion collisions. The electrons are approximately stationary and they collide with a fast-moving ion. Here we study the same collision experimentally, in a reference system where the ions (or atoms) are stationary and interacting with keV electrons. Scattering cross sections under these conditions deviate from Rutherford, and we link these deviations, at higher energies, to the Z 3 contributions to the electronic stopping and the related Barkas effect and, at lower energies, also to quantum interference. The present measurements are well described by partial-wave calculations of the elastic cross section of electrons scattering from atoms. Encouraged by this agreement we use these calculations to estimate the Barkas factor for all elements and many energies. A universal curve for the Barkas factor due to close collisions is obtained for neutral projectiles and similar curves with smaller magnitude are found for ions.

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Measurements of Meson Masses and Related Quantities

Cited by 91 publications

References 2 publications

Measurement of the atmospheric muon charge ratio at TeV energies with the MINOS detector

Measurement of the atmospheric muon charge ratio at TeV energies with the MINOS detector

Measurement of the underground atmospheric muon charge ratio using the MINOS Near Detector

Exploring the Barkas effect with keV-electron scattering

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