dc.contributor.author | Kachelriess, Michael | |
dc.date.accessioned | 2020-01-16T09:32:32Z | |
dc.date.available | 2020-01-16T09:32:32Z | |
dc.date.created | 2019-07-11T14:07:34Z | |
dc.date.issued | 2019 | |
dc.identifier.citation | Journal of Physics: Conference Series. 2019, 1181 (1), . | nb_NO |
dc.identifier.issn | 1742-6588 | |
dc.identifier.uri | http://hdl.handle.net/11250/2636574 | |
dc.description.abstract | We argue that the diffusion of cosmic rays in the Galactic magnetic field has to be strongly anisotropic. As a result, the number of CR sources contributing to the local CR flux is strongly reduced. The CR density is therefore less smooth, and the contribution of individual sources to the CR dipole anisotropy becomes more prominent. In the case of anisotropic diffusion, the observed plateau in the CR dipole anisotropy around 2–20 TeV can be explained by a 2–3 Myr old CR source which dominates the local CR flux in this energy range. | nb_NO |
dc.language.iso | eng | nb_NO |
dc.publisher | IOP Publishing | nb_NO |
dc.rights | Navngivelse 4.0 Internasjonal | * |
dc.rights.uri | http://creativecommons.org/licenses/by/4.0/deed.no | * |
dc.title | Anisotropic diffusion and the cosmic ray anisotropy | nb_NO |
dc.type | Journal article | nb_NO |
dc.type | Peer reviewed | nb_NO |
dc.description.version | publishedVersion | nb_NO |
dc.source.pagenumber | 6 | nb_NO |
dc.source.volume | 1181 | nb_NO |
dc.source.journal | Journal of Physics: Conference Series | nb_NO |
dc.source.issue | 1 | nb_NO |
dc.identifier.doi | 10.1088/1742-6596/1181/1/012039 | |
dc.identifier.cristin | 1711292 | |
dc.description.localcode | Content from this work may be used under the terms of theCreative Commons Attribution 3.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. Published under licence by IOP Publishing Ltd | nb_NO |
cristin.unitcode | 194,66,20,0 | |
cristin.unitname | Institutt for fysikk | |
cristin.ispublished | true | |
cristin.fulltext | preprint | |
cristin.qualitycode | 1 | |