Speaker
Nicholas Eugene Engelbrecht
(SANSA)
Description
The stochastic approach to solving the Parker transport equation has relatively recently become a popular means of furthering the numerical study of cosmic ray modulation. This is in part due to the fact that this approach allows for three-dimensional, time-dependent simulations over a range of energies that could not be performed using earlier finite difference techniques. We present here preliminary results from one such study, showing galactic cosmic ray proton intensities computed using a time-dependent stochastic modulation code, employing observationally motivated solar cycle-dependent expressions for the heliospheric magnetic field, tilt angle, and solar wind speed. Qualitative comparisons with spacecraft observations of cosmic ray intensities will also be made.
| Registration number following "ICRC2015-I/" | 117 |
|---|---|
| Collaboration | -- not specified -- |
Author
Nicholas Eugene Engelbrecht
(SANSA)
Co-authors
Luo
(North West University, South Africa)
Marthinus Potgieter
(North-West Uiversity)
Roelf Du Toit Strauss
(North-West University, Potchefstroom)
