The angular distribution of cosmic rays at the boundary of the heliosphere

Details The angular distribution of cosmic rays at the boundary of the heliosphere The angular distribution of cosmic rays at the boundary of the heliosphere

Jun 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979p%26ss...27..733d&link_type=abstract

Planetary and Space Science, vol. 27, June 1979, p. 733-738. Research supported by the Science Research Council.

Physics

2

Angular Distribution, Diurnal Variations, Galactic Radiation, Primary Cosmic Rays, Energetic Particles, Harmonic Analysis, Milky Way Galaxy, Particle Motion, Particle Telescopes

Scientific paper

Measurements of the sidereal daily variation of the muon intensity at a depth of 60 mwe have been carried out in London using telescopes inclined at 70 deg to the zenith for the period 1972 to the present. The direction of maximum sensitivity for these telescopes lies in the earth's equatorial plane and the asymptotic directions of look at the boundary of the heliosphere have been determined by integrating the equation of motion of the primary particles in a model interplanetary magnetic field. In this way the measured sidereal variation can be related to the cosmic ray intensity distribution in interstellar space. It is shown that the observational data are consistent with an axially symmetric intensity distribution of the form Delta I = 0.09 (1 + cos alpha) % where Delta I is the direction from the mean intensity and alpha is measured from the direction of maximum intensity. The most likely interpretation of this result is that the axis of this distribution corresponds to the local direction of the interstellar magnetic field and that the cosmic rays have a bulk streaming motion of 65 plus or minus 15 km/sec along the field direction.

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