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dc.contributor.authorLuo, Xi
dc.contributor.authorZhang, Ming
dc.contributor.authorPotgieter, Marius S.
dc.contributor.authorFeng, Xueshang
dc.contributor.authorPOGORELOV, NIKOLAI V.
dc.date.accessioned2016-10-21T21:18:59Z
dc.date.available2016-10-21T21:18:59Z
dc.date.issued2015-07-20
dc.identifier.citationLuo, X., Zhang, M., Potgieter, M., Feng, X., & Pogorelov, N. V. (2015). A NUMERICAL SIMULATION of COSMIC-RAY MODULATION NEAR the HELIOPAUSE. Astrophysical Journal, 808(1) doi:10.1088/0004-637X/808/1/82en_US
dc.identifier.urihttp://hdl.handle.net/11141/1093
dc.description.abstractBased on a hybrid galactic cosmic-ray transport model, which incorporated MHD global heliospheric data into Parker's cosmic-ray transport equation, we studied the behavior of the transport of galactic cosmic rays and the corresponding gradients in their flux 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 the ratio multiplying factor reached 10^10, the radial flux experienced a sudden jump near the HP, similar to what Voyager 1 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.en_US
dc.language.isoen_USen_US
dc.rightsThis published article is made available in accordance with the publisher's policy. It may be subject to U.S. copyright law.en_US
dc.rights.urihttps://aas.org/publications/aas-copyright-policyen_US
dc.titleA NUMERICAL SIMULATION of COSMIC-RAY MODULATION NEAR the HELIOPAUSEen_US
dc.typeArticleen_US
dc.identifier.doi10.1088/0004-637X/808/1/82


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