 |
| Titel |
On the heliolatitudinal variation of the galactic cosmic-ray intensity. Comparison with Ulysses measurements |
| VerfasserIn |
G. Exarhos, X. Moussas |
| Medientyp |
Artikel
|
| Sprache |
Englisch
|
| ISSN |
0992-7689
|
| Digitales Dokument |
URL |
| Erschienen |
In: Annales Geophysicae ; 21, no. 6 ; Nr. 21, no. 6, S.1341-1345 |
| Datensatznummer |
250014644
|
| Publikation (Nr.) |
 copernicus.org/angeo-21-1341-2003.pdf |
|
|
|
|
|
| Zusammenfassung |
We study the dependence
of cosmic rays with heliolatitude using a simple method and compare the results
with the actual data from Ulysses and IMP spacecraft. We reproduce the galactic
cosmic-ray heliographic latitudinal intensity variations, applying a
semi-empirical, 2-D diffusion-convection model for the cosmic-ray transport in
the interplanetary space. This model is a modification of our previous 1-D
model (Exarhos and Moussas, 2001) and includes not only the radial diffusion of
the cosmic-ray particles but also the latitudinal diffusion. Dividing the
interplanetary region into "spherical magnetic sectors" (a small
heliolatitudinal extension of a spherical magnetized solar wind plasma shell)
that travel into the interplanetary space at the solar wind velocity, we
calculate the cosmic-ray intensity for different heliographic latitudes as a
series of successive intensity drops that all these "spherical magnetic
sectors" between the Sun and the heliospheric termination shock cause the
unmodulated galactic cosmic-ray intensity. Our results are compared with the
Ulysses cosmic-ray measurements obtained during the first pole-to-pole passage
from mid-1994 to mid-1995.
Key words. Interplanetary physics
(cosmic rays; interplanetray magnetic fields; solar wind plasma) |
| |
|
| Teil von |
|
|
|
|
|
|
|
|