Please use this identifier to cite or link to this item: http://hdl.handle.net/2307/525
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dc.contributor.authorDi Salvo, T.-
dc.contributor.authorD'Ai, A.-
dc.contributor.authorIaria, R.-
dc.contributor.authorBurderi, L.-
dc.contributor.authorDovciak, M.-
dc.contributor.authorKaras, V.-
dc.contributor.authorMatt, Giorgio-
dc.contributor.authorPapitto, A.-
dc.contributor.authorPiraino, S.-
dc.contributor.authorRiggio, A.-
dc.contributor.authorRobba, N. R.-
dc.contributor.authorSantangelo, A.-
dc.date.accessioned2011-07-18T13:24:44Z-
dc.date.available2011-07-18T13:24:44Z-
dc.date.issued2009-10-
dc.identifier.issn0035-8711-
dc.identifier.urihttp://hdl.handle.net/2307/525-
dc.descriptionThe Authors. Journal compilation RASit_IT
dc.description.abstractIron emission lines at 6.4-6.97 keV, identified with fluorescent Kalpha transitions, are among the strongest discrete features in the X-ray band. These are therefore one of the most powerful probes to infer the properties of the plasma in the innermost part of the accretion disc around a compact object. In this paper, we present a recent XMM-Newton observation of the X-ray burster 4U 1705-44, where we clearly detect a relativistically smeared iron line at about 6.7 keV, testifying with high statistical significance that the line profile is distorted by high-velocity motion in the accretion disc. As expected from disc reflection models, we also find a significant absorption edgeat about 8.3 keV; this feature appears to be smeared, and is compatible with being produced in the same region where the iron line is produced. From the line profile, we derive the physical parameters of the inner accretion disc with large precision. The line is identified with the Kalpha transition of highly ionized iron, Fe xxv, the inner disc radiusis R-in = 14 +/- 2 R-g (where R-g is the Gravitational radius, GM/c2), the emissivity dependence from the disc radius is r-2.27 +/- 0.08, theinclination angle with respect to the line of sight is i = 39 degrees+/- 1 degrees. Finally, the XMM-Newton spectrum shows evidences of other low-energy emission lines, which again appear broad and their profiles are compatible with being produced in the same region where the iron line is produced.it_IT
dc.language.isoenit_IT
dc.publisherWiley-Blackwellit_IT
dc.relation.ispartofMonthly Notices of the Royal Astronomical Societyit_IT
dc.subjectIRON EMISSION-LINEit_IT
dc.subjectXMM-NEWTON/EPIC-PNit_IT
dc.subjectBLACK-HOLE SPINit_IT
dc.subjectSAXit_IT
dc.subjectJ1808.4-3658it_IT
dc.subjectMCG-6-30-15it_IT
dc.subject4U-1705-44it_IT
dc.subjectCOMPTONIZATIONit_IT
dc.subjectMODELSit_IT
dc.subjectHARDit_IT
dc.titleA relativistically smeared spectrum in the neutron star X-ray binary 4U1705-44: looking at the inner accretion disc with X-ray spectroscopyit_IT
dc.typeArticleen
dc.subject.miurSettori Disciplinari MIUR::Scienze fisiche::ASTRONOMIA E ASTROFISICAit_IT
dc.subject.miurScienze fisiche-
dc.subject.isicruiCategorie ISI-CRUI::Scienze fisiche::Physicsit_IT
dc.subject.isicruiScienze fisiche-
dc.subject.anagraferoma3Scienze fisicheit_IT
dc.relation.volumenumber398it_IT
dc.relation.pagenumber2022-2027it_IT
dc.identifier.doi10.1111/j.1365-2966.2009.15240.x-
dc.relation.issuenumber4it_IT
dc.description.romatrecurrentDipartimento di Fisica 'Edoardo Amaldi'*
item.languageiso639-1other-
item.fulltextWith Fulltext-
item.grantfulltextrestricted-
Appears in Collections:A - Articolo su rivista
X_Dipartimento di Fisica 'Edoardo Amaldi'
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