{"@context":{"@vocab":"https://cir.nii.ac.jp/schema/1.0/","rdfs":"http://www.w3.org/2000/01/rdf-schema#","dc":"http://purl.org/dc/elements/1.1/","dcterms":"http://purl.org/dc/terms/","foaf":"http://xmlns.com/foaf/0.1/","prism":"http://prismstandard.org/namespaces/basic/2.0/","cinii":"http://ci.nii.ac.jp/ns/1.0/","datacite":"https://schema.datacite.org/meta/kernel-4/","ndl":"http://ndl.go.jp/dcndl/terms/","jpcoar":"https://github.com/JPCOAR/schema/blob/master/2.0/"},"@id":"https://cir.nii.ac.jp/crid/1361418520831024256.json","@type":"Article","productIdentifier":[{"identifier":{"@type":"DOI","@value":"10.1063/1.4906356"}},{"identifier":{"@type":"URI","@value":"https://pubs.aip.org/aip/pop/article-pdf/doi/10.1063/1.4906356/13673876/012309_1_online.pdf"}}],"dc:title":[{"@value":"Electron vortex magnetic holes: A nonlinear coherent plasma structure"}],"description":[{"type":"abstract","notation":[{"@value":"<jats:p>We report the properties of a novel type of sub-proton scale magnetic hole found in two dimensional particle-in-cell simulations of decaying turbulence with a guide field. The simulations were performed with a realistic value for ion to electron mass ratio. These structures, electron vortex magnetic holes (EVMHs), have circular cross-section. The magnetic field depression is associated with a diamagnetic azimuthal current provided by a population of trapped electrons in petal-like orbits. The trapped electron population provides a mean azimuthal velocity and since trapping preferentially selects high pitch angles, a perpendicular temperature anisotropy. The structures arise out of initial perturbations in the course of the turbulent evolution of the plasma, and are stable over at least 100 electron gyroperiods. We have verified the model for the EVMH by carrying out test particle and PIC simulations of isolated structures in a uniform plasma. It is found that (quasi-)stable structures can be formed provided that there is some initial perpendicular temperature anisotropy at the structure location. The properties of these structures (scale size, trapped population, etc.) are able to explain the observed properties of magnetic holes in the terrestrial plasma sheet. EVMHs may also contribute to turbulence properties, such as intermittency, at short scale lengths in other astrophysical plasmas.</jats:p>"}]}],"creator":[{"@id":"https://cir.nii.ac.jp/crid/1381418520831024256","@type":"Researcher","foaf:name":[{"@value":"Christopher T. Haynes"}],"jpcoar:affiliationName":[{"@value":"Queen Mary University of London 1 School of Physics and Astronomy, , Mile End Road, London E1 4NS, United Kingdom"}]},{"@id":"https://cir.nii.ac.jp/crid/1381418520831024257","@type":"Researcher","foaf:name":[{"@value":"David Burgess"}],"jpcoar:affiliationName":[{"@value":"Queen Mary University of London 1 School of Physics and Astronomy, , Mile End Road, London E1 4NS, United Kingdom"}]},{"@id":"https://cir.nii.ac.jp/crid/1381418520831024259","@type":"Researcher","foaf:name":[{"@value":"Enrico Camporeale"}],"jpcoar:affiliationName":[{"@value":"Centrum Wiskunde & Informatica (CWI) 2 Multiscale Dynamics, , Amsterdam, The Netherlands"}]},{"@id":"https://cir.nii.ac.jp/crid/1381418520831024258","@type":"Researcher","foaf:name":[{"@value":"Torbjorn Sundberg"}],"jpcoar:affiliationName":[{"@value":"Queen Mary University of London 1 School of Physics and Astronomy, , Mile End Road, London E1 4NS, United Kingdom"}]}],"publication":{"publicationIdentifier":[{"@type":"PISSN","@value":"1070664X"},{"@type":"EISSN","@value":"10897674"}],"prism:publicationName":[{"@value":"Physics of Plasmas"}],"dc:publisher":[{"@value":"AIP Publishing"}],"prism:publicationDate":"2015-01-01","prism:volume":"22","prism:number":"1"},"reviewed":"false","url":[{"@id":"https://pubs.aip.org/aip/pop/article-pdf/doi/10.1063/1.4906356/13673876/012309_1_online.pdf"}],"createdAt":"2015-01-22","modifiedAt":"2023-07-02","relatedProduct":[{"@id":"https://cir.nii.ac.jp/crid/1360013168825261056","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"A Case for Electron-Astrophysics"}]},{"@id":"https://cir.nii.ac.jp/crid/2050307417125237632","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Unusual enhancement of ~ 30 MeV proton flux in an ICME sheath region"}]}],"dataSourceIdentifier":[{"@type":"CROSSREF","@value":"10.1063/1.4906356"},{"@type":"CROSSREF","@value":"10.1007/s10686-021-09761-5_references_DOI_bIACQl1OA5vKnwOnv25gGOv0sf"},{"@type":"CROSSREF","@value":"10.1186/s40623-021-01362-y_references_DOI_bIACQl1OA5vKnwOnv25gGOv0sf"}]}