Speaker
Xi Luo
(SIGMA Weather Group, State Key Laboratory of Space Weather, Center for Space Science and Applied Research, CAS, Beijing, China)
Description
Based on a hybrid galactic cosmic ray transport model, which incorporated MagnetoHydroDynamics (MHD) global heliospheric data into Parker's cosmic ray transport equation, we studied the behaviour of the transport of galactic cosmic rays near the heliopause (HP). We found that: (1) By increasing the ratio of the parallel diffusion coefficient to the perpendicular diffusion coefficient in the interstellar magnetic field of the outer heliosheath, the simulated radial flux near the HP increases as well. As this ratio multiplying factor reaches 10e10, the radial flux experience a sudden jump near the HP, similar to what Voyager 1 had observed in 2012. (2) The effect of changing the diffusion coefficients ratio on the radial flux variation depends on the energy of the cosmic rays, the lower the energy, the more pronounced the effect is. (3) The magnitude of the diffusion coefficients also affect the radial flux near the HP; the modulation beyond the HP varies by adjusting the magnitude multiplying factor. (4) After increasing the ratio of the diffusion coefficients beyond the HP, more pseudo-particles in our SDE approach which have been traced from the upwind nose region exit in the downwind tail region. It is thus possible that they diffuse more directly from the tail region to the nose region.
| Registration number following "ICRC2015-I/" | 196 |
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Primary author
Xi Luo
(SIGMA Weather Group, State Key Laboratory of Space Weather, Center for Space Science and Applied Research, CAS, Beijing, China)
Co-authors
Marthinus Potgieter
(North-West Uiversity)
Ming Zhang
(Florida Institute of Technology)
N.V Pogorelov
(University of Alabama, Huntsville)
Xueshang Feng
(SIGMA Weather Group, State Key Laboratory of Space Weather, Center for Space Science and Applied Research, CAS, Beijing, China)
