Particle drift effects on cosmic ray modulation during solar maximum

DC FieldValueLanguage
dc.contributor.authorFerreira, SES
dc.contributor.authorPotgieter, MS
dc.contributor.authorHeber, B
dc.contributor.editorPotgieter, MS
dc.contributor.editorHeber, B
dc.contributor.editorFichtner, H
dc.contributor.editorMarsden, RG
dc.date.accessioned2021-12-23T16:09:20Z-
dc.date.available2021-12-23T16:09:20Z-
dc.date.issued2003
dc.identifier.issn02731177
dc.identifier.urihttps://osnascholar.ub.uni-osnabrueck.de/handle/unios/8742-
dc.descriptionD1 1/D2 1/E3 1 Symposium of COSPAR Scientific Commission D held at the 34th COSPAR Scientific Assembly/2nd Space Congress, HOUSTON, TX, OCT 10-19, 2002
dc.description.abstractA fully time-dependent cosmic ray modulation model based on the numerical solution of Parker's transport equation is used to study the amount of particle drifts needed to explain the observed 1.2 GV electron to Helium ratio at Earth and the 2.5 GV electron to proton ratio (e/p) observed by the KET instrument on the Ulysses spacecraft. The model successfully simulates the modulation of protons, electrons and Helium ions for 11-year and 22-year cycles. It is based on the compound approach that incorporates the concept of propagation diffusion barriers combined with global increases in the HMF when propagated from the Sun throughout the heliosphere, as well as drifts and the other basic modulation mechanisms. It is found that less than 10% drifts is needed at solar maximum, when the solar magnetic field reverses, to explain the observed e/p along the Ulysses trajectory. (C) 2003 COSPAR. Published by Elsevier Ltd. All rights reserved.
dc.language.isoen
dc.publisherPERGAMON-ELSEVIER SCIENCE LTD
dc.relation.ispartofHELIOSPHERE AT SOLAR MAXIMUM
dc.relation.ispartofADVANCES IN SPACE RESEARCH-SERIES
dc.subject11-YEAR
dc.subjectAstronomy & Astrophysics
dc.subjectCYCLES
dc.subjectELECTRONS
dc.subjectEngineering
dc.subjectEngineering, Aerospace
dc.subjectGeology
dc.subjectGeosciences, Multidisciplinary
dc.subjectHELIOSPHERIC MODULATION
dc.subjectMAGNETIC-FIELD
dc.subjectMeteorology & Atmospheric Sciences
dc.subjectMINIMUM
dc.subjectPERPENDICULAR DIFFUSION
dc.subjectSIMULATION
dc.subjectTRANSPORT
dc.titleParticle drift effects on cosmic ray modulation during solar maximum
dc.typeconference paper
dc.identifier.doi10.1016/S0273-1177(03)00350-8
dc.identifier.isiISI:000186667900029
dc.description.volume32
dc.description.issue4
dc.description.startpage645
dc.description.endpage650
dc.contributor.researcheridAAY-9785-2021
dc.publisher.placeTHE BOULEVARD, LANGFORD LANE,, KIDLINGTON OX5 1GB, OXFORD, ENGLAND
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