Please use this identifier to cite or link to this item:
http://hdl.handle.net/20.500.12386/28821
DC Field | Value | Language |
---|---|---|
dc.contributor.author | Pintore, Fabio | en_US |
dc.contributor.author | MEREGHETTI, Sandro | en_US |
dc.contributor.author | ESPOSITO, PAOLO | en_US |
dc.contributor.author | Turolla, Roberto | en_US |
dc.contributor.author | TIENGO, ANDREA | en_US |
dc.contributor.author | Rea, Nanda | en_US |
dc.contributor.author | BERNARDINI, Federico | en_US |
dc.contributor.author | ISRAEL, Gian Luca | en_US |
dc.date.accessioned | 2020-12-14T10:36:52Z | - |
dc.date.available | 2020-12-14T10:36:52Z | - |
dc.date.issued | 2019 | en_US |
dc.identifier.issn | 0035-8711 | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/28821 | - |
dc.description.abstract | In 2003, the magnetar XTE J1810-197 started an outburst that lasted until early 2007. In the following 11 yr, the source stayed in a quiescent/low-activity phase. XTE J1810-197 is one of the closest magnetars, hence its X-ray properties can be studied in detail even in quiescence and an extended monitoring has been carried out to study its long-term timing and spectral evolution. Here, we report the results of new X-ray observations, taken between 2017 September and 2018 April, with XMM-Newton, Chandra, and NICER. We derived a phase-connected timing solution yielding a frequency derivative of -9.26(6) × 10<SUP>-14</SUP> Hz s<SUP>-1</SUP>. This value is consistent with that measured between 2009 and 2011, indicating that the pulsar spin-down rate remained quite stable during the long quiescent period. A spectral analysis of all the X-ray observations taken between 2009 and 2018 does not reveal significant spectral and/or flux variability. The spectrum of XTE J1810-197 can be described by the sum of two thermal components with temperatures of 0.15 and 0.3 keV, plus a power-law component with photon index 0.6. We also found evidence for an absorption line at ∼1.2 keV and width of 0.1 keV. Due to the long exposure time of the summed XMM-Newton observations, we could also carry out a phase-resolved spectral analysis for this source in quiescence. This showed that the flux modulation can be mainly ascribed to the warmer of the two thermal components, whose flux varies by ∼45 per cent along the pulse phase. | en_US |
dc.language.iso | eng | en_US |
dc.title | The 11 yr of low activity of the magnetar XTE J1810-197 | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.1093/mnras/sty3378 | en_US |
dc.identifier.scopus | 2-s2.0-85064454928 | en_US |
dc.identifier.isi | 000462280000066 | en_US |
dc.identifier.url | https://academic.oup.com/mnras/article/483/3/3832/5238741 | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 483 | en_US |
dc.relation.issue | 3 | en_US |
dc.relation.firstpage | 3832 | en_US |
dc.type.referee | REF_1 | en_US |
dc.contributor.country | ITA | en_US |
dc.contributor.country | USA | en_US |
dc.contributor.country | ESP | 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 | 2019MNRAS.483.3832P | en_US |
dc.relation.ercsector | ERC sectors::Physical Sciences and Engineering::PE9 Universe sciences: astro-physics/chemistry/biology; solar systems; stellar, galactic and extragalactic astronomy, planetary systems, cosmology, space science, instrumentation::PE9_6 Stars and stellar systems | 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 Milano | - |
crisitem.author.dept | O.A. Roma | - |
crisitem.author.orcid | 0000-0002-3869-2925 | - |
crisitem.author.orcid | 0000-0003-3259-7801 | - |
crisitem.author.orcid | 0000-0003-4849-5092 | - |
crisitem.author.orcid | 0000-0002-6038-1090 | - |
crisitem.author.orcid | 0000-0001-5326-2010 | - |
crisitem.author.orcid | 0000-0001-5480-6438 | - |
crisitem.journal.journalissn | 0035-8711 | - |
crisitem.journal.ance | E112946 | - |
Appears in Collections: | 1.01 Articoli in rivista |
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sty3378.pdf | PDF editoriale | 491.21 kB | Adobe PDF | View/Open |
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