Utilizza questo identificativo per citare o creare un link a questo documento:
http://hdl.handle.net/20.500.12386/25186
Campo DC | Valore | Lingua |
---|---|---|
dc.contributor.author | Coti Zelati, F. | en_US |
dc.contributor.author | Rea, N. | en_US |
dc.contributor.author | CAMPANA, Sergio | en_US |
dc.contributor.author | DE MARTINO, Domitilla | en_US |
dc.contributor.author | PAPITTO, ALESSANDRO | en_US |
dc.contributor.author | Safi-Harb, S. | en_US |
dc.contributor.author | Torres, D. F. | en_US |
dc.date.accessioned | 2020-05-26T13:47:44Z | - |
dc.date.available | 2020-05-26T13:47:44Z | - |
dc.date.issued | 2016 | en_US |
dc.identifier.issn | 0035-8711 | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/25186 | - |
dc.description.abstract | The X-ray source RX J2015.6+3711 was discovered by ROSAT in 1996 and recently proposed to be a cataclysmic variable (CV). Here, we report on an XMM-Newton observation of RX J2015.6+3711 performed in 2014, where we detected a coherent X-ray modulation at a period of 7196 ± 11 s and discovered other significant (>6σ) small-amplitude periodicities which we interpret as the CV spin period and the sidebands of a possible ∼12-h periodicity, respectively. The 0.3-10 keV spectrum can be described by a power law (Γ = 1.15 ± 0.04) with a complex absorption pattern, a broad emission feature at 6.60 ± 0.01 keV, and an unabsorbed flux of (3.16 ± 0.05) × 10<SUP>-12</SUP> erg cm<SUP>-2</SUP> s<SUP>-1</SUP>. We observed a significant spectral variability along the spin phase, which can be ascribed mainly to changes in the density of a partial absorber and the power law normalization. Archival X-ray observations carried out by the Chandra satellite, and two simultaneous X-ray and UV/optical pointings with Swift, revealed a gradual fading of the source in the soft X-rays over the last 13 yr, and a rather stable X-ray-to-optical flux ratio (F<SUB>X</SUB>/F<SUB>V</SUB> ≈ 1.4-1.7). Based on all these properties, we identify this source with a magnetic CV, most probably of the intermediate polar type. The 2-h spin period makes RX J2015.6+3711, the second slowest rotator of the class, after RX J0524+4244 (`Paloma'; P<SUB>spin</SUB> ∼ 2.3 h). Although we cannot unambiguously establish the true orbital period with these observations, RX J2015.6+3711 appears to be a key system in the evolution of magnetic CVs. | en_US |
dc.language.iso | eng | en_US |
dc.title | Multiwavelength study of RX J2015.6+3711: a magnetic cataclysmic variable with a 2-h spin period | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.1093/mnras/stv2803 | en_US |
dc.identifier.scopus | 2-s2.0-84960837139 | en_US |
dc.identifier.isi | 000372264200055 | en_US |
dc.identifier.url | https://academic.oup.com/mnras/article/456/2/1913/1070142 | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 456 | en_US |
dc.relation.issue | 2 | en_US |
dc.relation.firstpage | 1913 | en_US |
dc.relation.lastpage | 1923 | en_US |
dc.relation.numberofpages | 11 | en_US |
dc.type.referee | REF_1 | en_US |
dc.description.numberofauthors | 7 | en_US |
dc.description.international | sì | en_US |
dc.contributor.country | ITA | en_US |
dc.contributor.country | ESP | en_US |
dc.contributor.country | CAN | en_US |
dc.contributor.country | NLD | 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.456.1913C | 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_11 Relativistic astrophysics | 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.fulltext | With Fulltext | - |
item.cerifentitytype | Publications | - |
item.grantfulltext | open | - |
crisitem.journal.journalissn | 0035-8711 | - |
crisitem.journal.ance | E112946 | - |
crisitem.author.dept | O.A. Brera | - |
crisitem.author.dept | O.A. Capodimonte | - |
crisitem.author.dept | O.A. Roma | - |
crisitem.author.orcid | 0000-0001-6278-1576 | - |
crisitem.author.orcid | 0000-0002-5069-4202 | - |
crisitem.author.orcid | 0000-0001-6289-7413 | - |
È visualizzato nelle collezioni: | 1.01 Articoli in rivista |
File in questo documento:
File | Descrizione | Dimensioni | Formato | |
---|---|---|---|---|
stv2803.pdf | Pdf editoriale | 2.11 MB | Adobe PDF | Visualizza/apri |
Page view(s)
53
controllato il 5-ago-2024
Download(s)
29
controllato il 5-ago-2024
Google ScholarTM
Check
Altmetric
Altmetric
Tutti i documenti in DSpace sono pubblicati ad Accesso Aperto, salvo diversa indicazione per alcuni documenti specifici.