Evidence for a New Production Process for<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mrow><mml:msup><mml:mrow><mml:mn>10</mml:mn></mml:mrow><mml:mrow><mml:mn>12</mml:mn></mml:mrow></mml:msup></mml:mrow></mml:math>-eV Muons

Bergeson, H. E.; Keuffel, J. W.; Larson, M. O.; Martin, E.; Mason, G. W.

doi:10.1103/physrevlett.19.1487

Cited by 86 publications

(17 citation statements)

References 10 publications

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“…Such a strong quadratic interaction-suitably modifiedcould account for the large mass of W (i.e., mw^S-4 BeV), provide the automatic cutoff for higher-order weak processes at this energy, which seems to be required to understand the KL°-KS° mass difference, and perhaps be responsible for the anomalous production of high-energy muons by short-lived particles observed recently in the cosmic radiation. [18][19][20] …”

Section: Discussionmentioning

confidence: 99%

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Second-Order Weak Processes and Weak-Interaction Cutoff

1968

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The problem of the weak-interaction cutoff A has been studied with the universal current-current theory (UFI) and the intermediate-vector-boson (IVB) model, using the Bjorken technique to treat the highenergy behavior and the "hard meson" technique of Weinberg and Schnitzer. With these methods, the most divergent contributions to the second-order weak decay K L° -> vfi and K L°-Ks° mass difference Am are essentially independent of strong interaction. From K L°-> ixjx decay, A < 35-100 BeV, and from Am, A~3-4 BeV. With this latter value of A, the predicted rate of K L° -• /*£ is reduced to a value obtained by Beg treating this process as first-order in weak and second-order in electromagnetic interaction. The Beg calculation is redone with the algebra of currents, and the soft-kaon contribution to K L° -> A*M is calculated with both the UFI and IVB models. A possible origin of the low value of A deduced from Am is discussed.

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Section: Discussionmentioning

confidence: 99%

“…We next saturate the spectral functions in (18) by the low-lying poles ^4i(1020), p(760), Z^*(1320), and i£*(890), respectively, and derive the following estimates for the branching ratio a = T(K L° -» nfi)/T(K+ -» M + *V) :…”

Section: Other Calculations Of K L° -> Y£mentioning

confidence: 99%

Second-Order Weak Processes and Weak-Interaction Cutoff

1968

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“…Learned, H. Davis, P. Kotzer, M. Shapiro (all USA), G. Zatsepin (USSR) and S. Miyake (Japan) discussed a deep-water detector to clarify puzzles in muon depth-intensity curves. The anomalies reported by the group of W. Keuffel in Utah ("Keuffel effect") [Bergeson 1967] faded away, but it was obvious that such a detector could also work for neutrinos. An informal group of people to study such a detector was assembled, led by Reines, Roberts, Miyake and Learned.…”

Section: The Early Yearsmentioning

confidence: 99%

Towards high-energy neutrino astronomy

Spiering

2012

EPJ H

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The search for the sources of cosmic rays is a three-fold assault, using charged cosmic rays, gamma rays and neutrinos. The first conceptual ideas to detect high energy neutrinos date back to the late fifties. The long evolution towards detectors with a realistic discovery potential started in the seventies and eighties, with the pioneering works in the Pacific Ocean close to Hawaii and in Lake Baikal in Siberia. But only now, half a century after the first concepts, such a detector is in operation: IceCube at the South Pole. We do not yet know whether with IceCube we will indeed detect extraterrestrial high energy neutrinos or whether this will remain the privilege of next generation telescopes. But whatever the answer will be: the path to the present detectors was a remarkable journey. This review sketches its main milestones. a

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“…The Utah experiment raised the possibility for an additional source of muons. An explanation [Bjorken et al, 1969] of the Utah experiment has been proposed that requires an anomalous absorption of muons of negative helicity and unusual shape for the sea-level muon energy spectrum. This spectrum is often inferred from stopping rate versus depth measurements near sea level.…”

Section: Introductionmentioning

confidence: 99%

“…Until the experiments of the Utah cosmic-ray group [Bergeson et al, 1967], it was universally believed that cosmic-ray muons result solely from the decay of secondary pions and kaons from cosmic-ray interactions in the atmosphere. The Utah experiment raised the possibility for an additional source of muons.…”

Section: Introductionmentioning

confidence: 99%

Stopping rate of negative cosmic-ray muons near sea level

Spannagel¹,

Fireman²

1972

J. Geophys. Res.

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A production rate of 0. 065 ± 0. 003 Ar atom/kg min of K at 2-mwe depth below sea level was measured by sweeping argon from potassium solutions. This rate is unaffected by surrounding the solution by paraffin and is attributed to negative-muon captures and the electromagnetic interaction of fast muons, and not to a nucleonic cosmic-ray component. The 37 39 Ar yield from K by the stopping of negative muons in a muon beam of the SREL synchrocyclotron was measured to be 8. 5 ± 1. 7%. The stopping rate of negative cosmic-ray muons at 2-mwe depth below sea level from these measurements and an estimated 17% electromagnetic production is 0.63 ± 0.13 |_i /kg min. Previous measurements on the muon stopping rate vary by a factor of 5. Our value is slightly higher but is consistent with two 37 previous high values. The sensitivity of the Ar radiochemical method for the detection of muons is considerably higher than that of the previous radiochemical methods and could be used to measure the negative-muon capture rates at greater depths. IntroductionUntil the experiments of the Utah cosmic-ray group [Bergeson et al., 1967], it was universally believed that cosmic-ray muons result solely from the decay of secondary pions and kaons from cosmic-ray interactions in the atmosphere. The Utah experiment raised the possibility for an additional source of muons. An explanation [Bjorken et al., 1969] of the Utah experiment has been proposed that requires an anomalous absorption of muons of negative helicity and unusual shape for the sea-level muon energy spectrum. This spectrum is often inferred from stopping rate versus depth measurements near sea level. Although the muon stopping rate has been 111-098 measured by three different methods, measurements by even the same method often disagree. Stopped muon rates have mainly been measured with nuclear emulsions and with scintillators at depths to 300 mwe (meters of water equivalent). Recent measurements by Bergamasco [1970] are a factor of 2-5 higher than previous ones. Additional measurements of the stopped negative-muon rate might be helpful in determining whether cosmic muons result solely from the decay of secondary IT and K mesons.Until now, because of restricted sensitivity, radiochemical methods for detection have yielded positive results to a depth of only 0.2 mwe. Winsberg [1956] Cl from rainwater produced by the Ar (|jt , v n) reaction. Rama and Honda [1961] extracted gold radioactivities from mercury at sea level and state that their result is 59 consistent with Winsberg's. Takagi and Tanaka [1969] observed a Fe radioactivity of 0. 35 ± 0.14 atom/kg min induced by cosmic-ray muons in cobalt at sea level. This is a lower limit for the stopping of negative muons because the yield of the reaction was not determined. A more sensitive radiochemical method with a measured yield is needed. -37The K ([i , v 2n)Ar reaction offers the possibility for extremely high sensitivity because it is possible to extract argon with almost 100% efficiency from large 37 volumes of potassium ...

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Evidence for a New Production Process for1012-eV Muons

Cited by 86 publications

References 10 publications

Second-Order Weak Processes and Weak-Interaction Cutoff

Second-Order Weak Processes and Weak-Interaction Cutoff

Towards high-energy neutrino astronomy

Stopping rate of negative cosmic-ray muons near sea level

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