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http://hdl.handle.net/20.500.12386/27023
Campo DC | Valore | Lingua |
---|---|---|
dc.contributor.author | SIDOLI, Lara | en_US |
dc.contributor.author | ISRAEL, Gian Luca | en_US |
dc.contributor.author | Esposito, P. | en_US |
dc.contributor.author | RODRIGUEZ CASTILLO, Guillermo Andres | en_US |
dc.contributor.author | Postnov, K. | en_US |
dc.date.accessioned | 2020-09-01T09:33:20Z | - |
dc.date.available | 2020-09-01T09:33:20Z | - |
dc.date.issued | 2017 | en_US |
dc.identifier.issn | 0035-8711 | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/27023 | - |
dc.description.abstract | Pulsations from the high-mass X-ray binary AX J1910.7+0917 were discovered during Chandra observations performed in 2011. We report here more details on this discovery and discuss the source nature. The period of the X-ray signal is P = 36200 ± 110 s, with a pulsed fraction, PF, of 63 ± 4 per cent. Given the association with a massive B-type companion star, we ascribe this long periodicity to the rotation of the neutron star (NS), making AX J1910.7+0917 the slowest known X-ray pulsar. We also report on the spectroscopy of XMM-Newton observations that serendipitously covered the source field, resulting in a highly absorbed (column density almost reaching 10<SUP>23</SUP> cm<SUP>-2</SUP>), power-law X-ray spectrum. The X-ray flux is variable on a time-scale of years, spanning a dynamic range ≳ 60. The very long NS spin period can be explained within a quasi-spherical settling accretion model that applies to low luminosity, wind-fed, X-ray pulsars. | en_US |
dc.language.iso | eng | en_US |
dc.title | AX J1910.7+0917: the slowest X-ray pulsar | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.1093/mnras/stx1105 | en_US |
dc.identifier.scopus | 2-s2.0-85041348736 | en_US |
dc.identifier.isi | 000406836200037 | en_US |
dc.identifier.url | https://arxiv.org/pdf/1705.01791.pdf | en_US |
dc.identifier.url | https://academic.oup.com/mnras/article/469/3/3056/3800702 | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 469 | en_US |
dc.relation.issue | 3 | en_US |
dc.relation.firstpage | 3056 | en_US |
dc.relation.lastpage | 3061 | en_US |
dc.relation.numberofpages | 6 | en_US |
dc.type.referee | REF_1 | en_US |
dc.description.numberofauthors | 5 | en_US |
dc.description.international | sì | en_US |
dc.contributor.country | ITA | en_US |
dc.contributor.country | RUS | 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.469.3056S | 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 Milano | - |
crisitem.author.dept | O.A. Roma | - |
crisitem.author.dept | IASF Palermo | - |
crisitem.author.orcid | 0000-0001-9705-2883 | - |
crisitem.author.orcid | 0000-0001-5480-6438 | - |
crisitem.author.orcid | 0000-0003-3952-7291 | - |
crisitem.journal.journalissn | 0035-8711 | - |
crisitem.journal.ance | E112946 | - |
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