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dc.contributor.authorVos, Etienne Ebenen_US
dc.date.accessioned2012-09-10T16:14:38Z
dc.date.available2012-09-10T16:14:38Z
dc.date.issued2011en_US
dc.identifier.urihttp://hdl.handle.net/10394/7266
dc.descriptionThesis (M.Sc. (Physics))--North-West University, Potchefstroom Campus, 2012.
dc.description.abstractThe solar minimum of 2009 has been identified as an exceptional event with regard to cosmic ray (CR)modulation, since conditions in the heliosphere have reached unprecedented quiet levels. This unique minimum has been observed by the Earth–orbiting satellite, PAMELA, launched in June, 2006, from which vast sets of accurate proton and electron preliminary observations have been made available. These simultaneous measurements from PAMELA provide the ideal opportunity to conduct an in–depth study of CR modulation, in particular charge–sign dependent modulation. In utilizing this opportunity, a three–dimensional, steady–state modulation model was used to reproduce a selection of consecutive PAMELA proton and electron spectra from 2006 to 2009. Thiswas done by assuming full drifts and simplified diffusion coefficients, where the rigidity dependence and absolute value of themean free paths for protons and electrons were sequentially adjusted below 3 GV and 300 MV, respectively. Care has been taken in calculating yearly–averaged current–sheet tilt angle and magnetic field values that correspond to the PAMELA spectra. Following this study where the numerical model was used to investigate the individual effects resulting from changes in the tilt angle, diffusion coefficients, and global drifts, it was found that all these modulation processes played significant roles in contributing to the total increase in CR intensities from 2006 to 2009, as was observed by PAMELA. Furthermore, the effect that drifts has on oppositely charged particles was also evident from the difference between the peak–shaped time profiles of protons and the flatter time profiles of electrons, as is expected for an A < 0 polarity cycle. Since protons, which drift into the heliosphere along the heliospheric current–sheet, haven’t yet reached maximum intensity levels by 2008, their intensities increased notably more than electrons toward the end of 2009. The time and energy dependence of the electron to proton ratios were also studied in order to further illustrate and quantify the effect of drifts during this remarkable solar minimum period.en_US
dc.publisherNorth-West University
dc.subjectCosmic raysen_US
dc.subjectModulationen_US
dc.subjectHeliosphereen_US
dc.subjectSolar minimumen_US
dc.subjectParticle diffusionen_US
dc.subjectParticle driftsen_US
dc.subjectGalactic protonsen_US
dc.subjectGalactic electronsen_US
dc.subjectKosmiese straleen_US
dc.subjectModulasieen_US
dc.subjectHeliosfeeren_US
dc.subjectSonminimumen_US
dc.subjectDeeltjie diffusieen_US
dc.subjectDeeltjie dryfen_US
dc.subjectGalaktiese protoneen_US
dc.subjectGalaktiese elektroneen_US
dc.titleCosmic ray modulation processes in the heliosphereen
dc.typeThesisen_US
dc.description.thesistypeMastersen_US


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    This collection contains the original digitized versions of research conducted at the North-West University (Potchefstroom Campus)

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