A Reconciliation of the Discrepancy on the Cosmic-Ray Interplanetary Diffusion Mean Free Path

1995 ◽  
Vol 449 ◽  
pp. 386 ◽  
Author(s):  
L. Dennis Zhang
Keyword(s):  
Free Path ◽  
Cosmic Ray ◽  
Mean Free Path

Measurement of the collision mean free path of penetrating shower producing cosmic ray neutrons in lead

1961 ◽  
Vol 24 (3) ◽  
pp. 412-421 ◽  
Author(s):  
G. Bozóki ◽  
E. Fenyves ◽  
L. Jánossy
Keyword(s):  
Free Path ◽  
Cosmic Ray ◽  
Mean Free Path

Interaction mean-free-path of cosmic-ray Fe in air

1983 ◽  
Vol 94 (1) ◽  
pp. 201-209 ◽  
Author(s):  
J. H. Crane ◽  
D. D. Guo ◽  
M. H. Israel ◽  
J. Klarmann
Keyword(s):  
Free Path ◽  
Cosmic Ray ◽  
Mean Free Path

Further Study of the Anomalous Behavior of Secondary Particles Emitted from Heavy Primary Interactions

1972 ◽  
Vol 50 (18) ◽  
pp. 2082-2095 ◽  
Author(s):  
B. Judek
Keyword(s):  
Free Path ◽  
Relative Intensity ◽  
Cosmic Ray ◽  
Mean Free Path ◽  
Anomalous Behavior ◽  
Tentative Conclusion ◽  
Secondary Particles ◽  
Anomalous Component ◽  
Angular Interval ◽  
Singly Charged

Interaction lengths of singly charged relativistic secondary particles emitted from interactions of very heavy cosmic ray nuclei in emulsions were measured by systematic following of their tracks through the stack. The primary energies were determined by the "knock on" electron method. The results show that particles from interactions with primary energies between 1 and 5 GeV/nucleon emitted in the angular interval [Formula: see text] (θev is the expected RMS angle for evaporation protons) have significantly shorter mean free paths. The variation of the observed mean free paths with distance from the primary interactions shows a transition from short to normal interaction lengths at about 3 cm which indicates the presence of some anomalous component interacting with a very short mean free path of a few cm and relative intensity of order of 10%. This result cannot be accounted for by any known particle or interaction. Considerations of emission angles and types of stars produced by the secondary particles lead to a tentative conclusion that particles exhibiting the anomalously short interaction lengths are scattered fragments of the incident nuclei.

Cosmic-ray particle transport in weakly turbulent plasmas. Part 2. Mean free path of cosmic-ray protons

1993 ◽  
Vol 50 (1) ◽  
pp. 85-107 ◽  
Author(s):  
Reinhard Schlickeiser ◽  
Ulrich Achat
Keyword(s):  
Free Path ◽  
Charged Particles ◽  
Cosmic Ray ◽  
Mean Free Path ◽  
Magnetized Plasma ◽  
Solar Particle Events ◽  
Background Magnetic Field ◽  
Uniform Background ◽  
In Situ Observations

We use the general Fokker–Planck coefficients derived in the first paper of this series, which describe the interaction of energetic charged particles with weak plasma turbulence in a magnetized plasma, to calculate the mean free path λ of cosmic-ray particles along the uniform background magnetic field. This quantity is a key parameter for confining energetic charged particles in cosmic plasmas, and can be experimentally inferred from interplanetary in-situ observations of solar particle events

Inelastic mean free path and phase-shift determinations in NiO, using EXELFS

1993 ◽  
Vol 3 (7) ◽  
pp. 1649-1659
Author(s):  
Mohammad A. Tafreshi ◽  
Stefan Csillag ◽  
Zou Wei Yuan ◽  
Christian Bohm ◽  
Elisabeth Lefèvre ◽  
...  
Keyword(s):  
Phase Shift ◽  
Free Path ◽  
Mean Free Path ◽  
Inelastic Mean Free Path
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