A Possible Approach to Three‐Dimensional Cosmic‐Ray Propagation in the Galaxy. I. Stable Nuclei without Energy Change

Production cross-section of antiprotons for the study of cosmic-ray propagation in the Galaxy

“…p ðr; E p Þ will be presented separately, taking the position dependency into account, where one should note that the CR-proton density at the solar system, N p ðr ; E p Þ, is of approximately 35% lower than that at the Galactic center, N p ð0; E p Þ [28]. We will present the CR-p flux in the near future, based on the present result by combining with the CR density as summarized in our previous papers [25,26], and compare it with those obtained by recent experimental data, particularly the BESS data.…”

“…(25) with the data. Unfortunately, p data in nucleus-nucleus collisions are very limited, and we use those at P 0 ¼ 19:2 GeV/c [5] for the incident proton irradiated against various kinds of nuclear targets.…”

“…has developed a model of the three-dimensional CR propagation in the Galaxy, which reproduces very well both the stable [25,26], and unstable [27] CR nuclear components, and also the diffuse c-ray 0927-6505/$ -see front matter Ó 2007 Elsevier B.V. All rights reserved. doi:10.1016/j.astropartphys.2007.…”

Tracking method for the measurement of projectile charge changing cross-section using CR-39 detector with a high speed imaging microscope

“…In propagation models of GCR, the secondary/primary ratios strongly depend on the PCCSs of heavy ions (e.g. Shibata et al, 2004). In case of the (Sc + Ti + V)/Fe ratio, the PCCSs given by Webber et al (1990) are usually used in the energy interval of 0.3-1.6 GeV/n.…”

Cosmic-rays and diffuse γ-rays: Spatial gradients of Galactic parameters

“…We have studied the three-dimensional CR propagation model in three papers [56][57][58], hereafter called Papers I-III, respectively, and presented the numerical values of Galactic parameters such as the ISM gas density and the diffusion coefficient at the solar system (SS), using both the stable and the unstable CR nuclear components. The scale heights of the spatial gradient in these parameters, however, are difficult to obtain uniquely from the nuclear components alone, although we have shown that the ratio of the latitudinal scale height for the gas density against that for the diffusion coefficient equals to approximately 0.1, namely the Galactic halo thickness is of approximately ten times larger than the disk thickness.…”