Experimental Determination of Electron Orbits in the Field of a Magnetic Dipole: Part II

Abstract

In the preceding issue of Tellus were pub- lished the first results of our investigations of cosmic ray orbits in the field of a magnetic dipole. The investigations were carried out by measurements o n a model with particle mo- mentum range corresponding to 1010-eV/c. A detailed description of the apparatus and the performance of the experiment is given in part I of the present paper.

41. The solar daily variation of the cosmic ray intensity

“…Using the data on the trajectories obtained in this way, Brunberg and Dattner [4] have shown that it is possible to account for the daily variation observed with counter telescopes pointing in the north and south directions at 30 0 to the vertical if it is assumed that the mean energy of the primary radiation responsible for the variation lies in the region 2 to 4 x io 10 eV. With this assumption, an anisotropy of the primary radiation with a direction lying near the plane of the ecliptic would produce a daily variation of nearly the same amplitude for the north and south directions but with a phase difference of about 2 hr as was indeed observed in 1948 and 1949 (Malmfors[2] 3 Elliot and Dolbear [i]). …”

“…The trajectories of cosmic ray particles in the earth's field have been investi gated by Brunberg and Dattner [3] by means of scale model experiments. Using the data on the trajectories obtained in this way, Brunberg and Dattner [4] have shown that it is possible to account for the daily variation observed with counter telescopes pointing in the north and south directions at 30 0 to the vertical if it is assumed that the mean energy of the primary radiation responsible for the variation lies in the region 2 to 4 x io 10 eV.…”

The Upper Limiting Primary Rigidity of the Cosmic Ray Solar Anisotropy

“…The primaries of rigidity R that are responsible for J (R, wr) will have approached the Earth's magnetic field from directions within some asymptotic volume element (Qr)R specified by latitude (Dr)R and longitude (<Pr)R. Such asymptotic coordinates are usually found either by computing the trajectories of the primaries outward from the direction (Zr, arJ at the geomagnetic location of the recorder (see McCracken, Rao, and Shea 1962), or else from observations of thc deflections of charged particles in a physical simulation of the geomagnetic field (see the terrella experiments of Brunberg and Dattner 1953). When J(R, wr) and the associated asymptotic coordinates (8 r )R and (</>r)R have been calculated for each of the volume elements Wr that make up the solid angle of the recorder, the distribution of the fractional f-L-meson intensity due to primaries of rigidity R can be determined with respect to both asymptotic latitude and asymptotic longitude of the primaries.…”

“…Consequently, the particle deflections were estimated from the diagrams of Brunberg and Dattner (1953) for the geomagnetic southern latitude of 50°. Considerable interpolation was necessary and for this reason it was found more convenient to express the asymptotic latitude and longitude data in the form of deflections in zenith angle and azimuth.…”