{"@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/1361699994847799168.json","@type":"Article","productIdentifier":[{"identifier":{"@type":"DOI","@value":"10.3847/2041-8213/aa6745"}},{"identifier":{"@type":"URI","@value":"https://iopscience.iop.org/article/10.3847/2041-8213/aa6745"}},{"identifier":{"@type":"URI","@value":"https://iopscience.iop.org/article/10.3847/2041-8213/aa6745/pdf"}}],"dc:title":[{"@value":"Radio Emission from Pulsar Wind Nebulae without Surrounding Supernova Ejecta: Application to FRB 121102"}],"description":[{"type":"abstract","notation":[{"@value":"<jats:title>Abstract</jats:title>\n               <jats:p>In this paper, we propose a new scenario in which a rapidly rotating strongly magnetized pulsar without any surrounding supernova ejecta repeatedly produces fast radio bursts (FRBs) via a range of possible mechanisms; simultaneously, an ultra-relativistic electron/positron pair wind from the pulsar sweeps up its ambient dense interstellar medium, giving rise to a non-relativistic pulsar wind nebula (PWN). We show that the synchrotron radio emission from such a PWN is bright enough to account for the recently discovered persistent radio source associated with the repeating FRB 121102 within reasonable ranges of the model parameters. Our PWN scenario is consistent with the non-evolution of the dispersion measure inferred from all of the repeating bursts observed in four years.</jats:p>"}]}],"creator":[{"@id":"https://cir.nii.ac.jp/crid/1381699994847799169","@type":"Researcher","foaf:name":[{"@value":"Z. G. Dai"}]},{"@id":"https://cir.nii.ac.jp/crid/1381699994847799170","@type":"Researcher","foaf:name":[{"@value":"J. S. Wang"}]},{"@id":"https://cir.nii.ac.jp/crid/1381699994847799168","@type":"Researcher","foaf:name":[{"@value":"Y. W. Yu"}]}],"publication":{"publicationIdentifier":[{"@type":"PISSN","@value":"20418205"},{"@type":"EISSN","@value":"20418213"}],"prism:publicationName":[{"@value":"The Astrophysical Journal Letters"}],"dc:publisher":[{"@value":"American Astronomical Society"}],"prism:publicationDate":"2017-03-20","prism:volume":"838","prism:number":"1","prism:startingPage":"L7"},"reviewed":"false","dc:rights":["https://iopscience.iop.org/page/copyright","https://iopscience.iop.org/info/page/text-and-data-mining"],"url":[{"@id":"https://iopscience.iop.org/article/10.3847/2041-8213/aa6745"},{"@id":"https://iopscience.iop.org/article/10.3847/2041-8213/aa6745/pdf"}],"createdAt":"2017-03-24","modifiedAt":"2024-01-08","relatedProduct":[{"@id":"https://cir.nii.ac.jp/crid/1360002217650943232","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Constraints on pulsed emission model for repeating FRB 121102"}]},{"@id":"https://cir.nii.ac.jp/crid/1360294643715217152","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Can primordial black holes as all dark matter explain fast radio bursts?"}]},{"@id":"https://cir.nii.ac.jp/crid/1360565167604469632","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Repeating and non-repeating fast radio bursts from binary neutron star mergers"}]},{"@id":"https://cir.nii.ac.jp/crid/1360565170738309504","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Rapidly Rising Optical Transients from the Birth of Binary Neutron Stars"}]},{"@id":"https://cir.nii.ac.jp/crid/1360857593760174976","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Binary Comb Models for FRB 121102"}]}],"dataSourceIdentifier":[{"@type":"CROSSREF","@value":"10.3847/2041-8213/aa6745"},{"@type":"CROSSREF","@value":"10.1093/pasj/psx093_references_DOI_Z5x17w4zL9ydrd4ZKJVe2WNfj5b"},{"@type":"CROSSREF","@value":"10.1103/physrevd.104.123033_references_DOI_Z5x17w4zL9ydrd4ZKJVe2WNfj5b"},{"@type":"CROSSREF","@value":"10.1093/pasj/psy029_references_DOI_Z5x17w4zL9ydrd4ZKJVe2WNfj5b"},{"@type":"CROSSREF","@value":"10.3847/1538-4357/aa8c7d_references_DOI_Z5x17w4zL9ydrd4ZKJVe2WNfj5b"},{"@type":"CROSSREF","@value":"10.3847/1538-4357/ac127a_references_DOI_Z5x17w4zL9ydrd4ZKJVe2WNfj5b"}]}