Engineering properties of a Pelagic clay / by H. J. Lee.

Lee, Homa J.

doi:10.5962/bhl.title.47476

Cited by 117 publications

(169 citation statements)

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“…Of course, this conclusion might change if another type of interpolating currents is considered. The investigation of the properties of tetraquark states within the QCD sum rule approach with other interpolating diquark currents, e.g., the pseudoscalar diquark, the vector diquark, or with some mixture of qq configurations, is in progress [11].…”

Section: Resultsmentioning

confidence: 99%

A QCD sum rule study of the light scalar mesons

Lee

2006

Eur. Phys. J. A

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Section: Resultsmentioning

confidence: 99%

A QCD sum rule study of the light scalar mesons

Lee

2006

Eur. Phys. J. A

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“…The theoretical approach based on the kinetic theory of weakly turbulent collisionless plasma gives somewhat different results, see Livshits & Tsytovich (1970), Lee & Völk (1973), Kulsrud (1978), Achterberg (1981), Fedorenko et al (1990, Zirakashvili (2000). In particular, it was shown that the nonlinear interactions of Alfvén waves and thermal particles lead to the nonlinear wave damping which is described by the equation…”

Section: Maximum Energy Of Accelerated Particlesmentioning

confidence: 99%

Limits on diffusive shock acceleration in supernova remnants in the presence of cosmic-ray streaming instability and wave dissipation

Птускин

Zirakashvili

2003

A&A

186

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Abstract. The instability in the cosmic-ray precursor of a supernova shock moving in interstellar medium is studied. The level of magnetohydrodynamic turbulence in this region determines the maximum energy of particles accelerated by the diffusive shock acceleration mechanism. A high efficiency of cosmic ray acceleration is accepted, and the consideration is not limited by the case of weak turbulence. It is assumed that Kolmogorov-type nonlinear wave interactions together with the ion-neutral collisions restrict the amplitude of the random magnetic field. As a result, the maximum energy of accelerated particles strongly depends on the age of the supernova remnant. The maximum energy can be as high as ∼1017 Z eV in young supernova remnants and falls to about ∼1010 Z eV at the end of the Sedov stage. Thus the standard estimate of maximum particle energy based on the Bohm limit calculated for the interstellar magnetic field strength is not justified in this case. This finding may explain why supernova remnants with age of more than a few thousand years are not prominent sources of very high energy gamma-rays.

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“…17 The SSA of π + (π − ) displays positive (negative) asymmetries, of order 5-10% for 0.1 < x F < 0. with zero, while that for the antiproton is positive. The cross sections for π ± , K ± , proton and antiproton measured in the same kinematic ranges are in agreement with NLO QCD calculations.…”

Section: Resultsmentioning

confidence: 99%