Please use this identifier to cite or link to this item:
http://hdl.handle.net/20.500.12386/27132
DC Field | Value | Language |
---|---|---|
dc.contributor.author | D'AI', ANTONINO | en_US |
dc.contributor.author | CUSUMANO, GIANCARLO | en_US |
dc.contributor.author | DEL SANTO, MELANIA | en_US |
dc.contributor.author | LA PAROLA, VALENTINA | en_US |
dc.contributor.author | SEGRETO, ALBERTO | en_US |
dc.date.accessioned | 2020-09-04T09:50:02Z | - |
dc.date.available | 2020-09-04T09:50:02Z | - |
dc.date.issued | 2017 | en_US |
dc.identifier.issn | 0035-8711 | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/27132 | - |
dc.description.abstract | The accretion-powered X-ray pulsar 4U 1626-67 is one of the few highly magnetized pulsars that accretes through Roche lobe overflow from a low-mass companion. The characteristics of its broad-band spectrum are similar to those of X-ray pulsars hosted in a high-mass X-ray binary system, with a broad resonant cyclotron scattering feature (CRSF) at ∼37 keV. In this work, we examine the pulse-resolved and the pulse-averaged broad-band spectrum using data from NuSTAR and Swift. We use the Becker & Wolff model of bulk+thermal Comptonization to infer key physical parameters of the accretion column flow and a broad-band model for the disc-reflected spectrum. In the softer X-ray band, we need to add a soft blackbody component with kT<SUB>bb</SUB> ∼ 0.5 keV, whose characteristics indicate a possible origin from the neutron star surface. Residuals suggest that the shape of the cyclotron line could be more satisfactorily fitted using a narrow core and broader wings and, at higher energies, a second harmonic could be present at ∼61 keV. | en_US |
dc.language.iso | eng | en_US |
dc.title | A broad-band self-consistent modelling of the X-ray spectrum of 4U 1626-67 | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.1093/mnras/stx1146 | en_US |
dc.identifier.scopus | 2-s2.0-85023769732 | en_US |
dc.identifier.isi | 000406839900087 | en_US |
dc.identifier.url | https://academic.oup.com/mnras/article-abstract/470/2/2457/3815540?redirectedFrom=fulltext | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 470 | en_US |
dc.relation.issue | 2 | en_US |
dc.relation.firstpage | 2457 | en_US |
dc.relation.lastpage | 2468 | en_US |
dc.type.referee | REF_1 | en_US |
dc.description.numberofauthors | 5 | en_US |
dc.description.international | no | en_US |
dc.contributor.country | ITA | en_US |
dc.relation.scientificsector | FIS/05 - ASTRONOMIA E ASTROFISICA | en_US |
dc.relation.journal | MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | en_US |
dc.type.miur | 262 Articolo in rivista | - |
dc.identifier.adsbibcode | 2017MNRAS.470.2457D | en_US |
dc.relation.ercsector | ERC sectors::Physical Sciences and Engineering | en_US |
dc.description.apc | no | en_US |
dc.description.oa | 1 – prodotto con file in versione Open Access (allegare il file al passo 5-Carica) | en_US |
item.openairecristype | http://purl.org/coar/resource_type/c_18cf | - |
item.openairetype | Article | - |
item.languageiso639-1 | en | - |
item.cerifentitytype | Publications | - |
item.grantfulltext | open | - |
item.fulltext | With Fulltext | - |
crisitem.author.dept | IASF Palermo | - |
crisitem.author.dept | IASF Palermo | - |
crisitem.author.dept | IASF Palermo | - |
crisitem.author.dept | IASF Palermo | - |
crisitem.author.dept | IASF Palermo | - |
crisitem.author.orcid | 0000-0002-5042-1036 | - |
crisitem.author.orcid | 0000-0002-8151-1990 | - |
crisitem.author.orcid | 0000-0002-1793-1050 | - |
crisitem.author.orcid | 0000-0002-8087-6488 | - |
crisitem.author.orcid | 0000-0001-7341-6603 | - |
crisitem.journal.journalissn | 0035-8711 | - |
crisitem.journal.ance | E112946 | - |
Appears in Collections: | 1.01 Articoli in rivista |
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