Please use this identifier to cite or link to this item:
http://hdl.handle.net/20.500.12386/25194
DC Field | Value | Language |
---|---|---|
dc.contributor.author | Pintore, Fabio | en_US |
dc.contributor.author | BERNARDINI, Federico | 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 | Rea, Nanda | en_US |
dc.contributor.author | Coti Zelati, Francesco | en_US |
dc.contributor.author | ISRAEL, Gian Luca | en_US |
dc.contributor.author | TIENGO, ANDREA | en_US |
dc.contributor.author | Zane, Silvia | en_US |
dc.date.accessioned | 2020-05-26T15:15:42Z | - |
dc.date.available | 2020-05-26T15:15:42Z | - |
dc.date.issued | 2016 | en_US |
dc.identifier.issn | 0035-8711 | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/25194 | - |
dc.description.abstract | We have analysed XMM-Newton and Chandra observations of the transient magnetar XTE J1810-197 spanning more than 11 yr, from the initial phases of the 2003 outburst to the current quiescent level. We investigated the evolution of the pulsar spin period and we found evidence for two distinct regimes: during the outburst decay, dot{ν } was highly variable in the range -(2-4.5) × 10<SUP>-13</SUP> Hz s<SUP>-1</SUP>, while during quiescence the spin-down rate was more stable at an average value of -1 × 10<SUP>-13</SUP> Hz s<SUP>-1</SUP>. Only during ∼3000 d (from MJD 54165 to MJD 56908) in the quiescent stage it was possible to find a phase-connected timing solution, with dot{ν }=-4.9× 10^{-14} Hz s<SUP>-1</SUP>, and a positive second frequency derivative, ddot{ν }=1.8× 10^{-22} Hz s<SUP>-2</SUP>. These results are in agreement with the behaviour expected if the outburst of XTE J1810-197 was due to a strong magnetospheric twist. | en_US |
dc.language.iso | eng | en_US |
dc.title | The variable spin-down rate of the transient magnetar XTE J1810-197 | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.1093/mnras/stw351 | en_US |
dc.identifier.scopus | 2-s2.0-84963800439 | en_US |
dc.identifier.isi | 000374569600077 | en_US |
dc.identifier.url | https://academic.oup.com/mnras/article/458/2/2088/2589042 | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 458 | en_US |
dc.relation.issue | 2 | en_US |
dc.relation.firstpage | 2088 | en_US |
dc.type.referee | REF_1 | en_US |
dc.description.numberofauthors | 10 | en_US |
dc.description.international | no | en_US |
dc.contributor.country | ITA | en_US |
dc.contributor.country | USA | en_US |
dc.contributor.country | GBR | 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 | 2016MNRAS.458.2088P | 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 | 0000-0001-5326-2010 | - |
crisitem.author.orcid | 0000-0003-3259-7801 | - |
crisitem.author.orcid | 0000-0001-5480-6438 | - |
crisitem.journal.journalissn | 0035-8711 | - |
crisitem.journal.ance | E112946 | - |
Appears in Collections: | 1.01 Articoli in rivista |
Files in This Item:
File | Description | Size | Format | |
---|---|---|---|---|
stw351.pdf | Pdf editoriale | 315.69 kB | Adobe PDF | View/Open |
Page view(s)
58
checked on Apr 26, 2024
Download(s)
13
checked on Apr 26, 2024
Google ScholarTM
Check
Altmetric
Altmetric
Items in DSpace are published in Open Access, unless otherwise indicated.