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dc.provenanceCONICET-
dc.creatorLuna, Gerardo Juan Manuel-
dc.creatorDiaz, M. P.-
dc.creatorBrickhouse, N. S.-
dc.creatorMoraes, M.-
dc.date2017-06-30T19:10:40Z-
dc.date2017-06-30T19:10:40Z-
dc.date2012-06-
dc.date2017-06-30T17:28:14Z-
dc.date.accessioned2019-04-29T15:36:25Z-
dc.date.available2019-04-29T15:36:25Z-
dc.date.issued2012-06-
dc.identifierLuna, Gerardo Juan Manuel; Diaz, M. P.; Brickhouse, N. S.; Moraes, M.; XMM-Newton EPIC and OM observation of Nova Centauri 1986 (V842 Cen); Wiley; Monthly Notices of the Royal Astronomical Society; 423; 1; 6-2012; L75-L78-
dc.identifier0035-8711-
dc.identifierhttp://hdl.handle.net/11336/19303-
dc.identifierCONICET Digital-
dc.identifierCONICET-
dc.identifier.urihttp://rodna.bn.gov.ar:8080/jspui/handle/bnmm/297616-
dc.descriptionWe report the results from the temporal and spectral analysis of an XMM–Newton observation of Nova Centauri 1986 (V842 Cen). We detect a period at 3.51 ± 0.4 h in the EPIC data and at 4.0 ± 0.8 h in the Optical Monitor (OM) data. The X-ray spectrum is consistent with the emission from an absorbed thin thermal plasma with a temperature distribution given by an isobaric cooling flow. The maximum temperature of the cooling flow model is kTmax = 43+23 −12 keV. Such a high temperature can be reached in a shocked region and, given the periodicity detected, most likely arises in a magnetically channelled accretion flow characteristic of intermediate polars. The pulsed fraction of the 3.51-h modulation decreases with energy as observed in the X-ray light curves of magnetic cataclysmic variables, possibly due either to occultation of the accretion column by the white dwarf body or phase-dependent to absorption. We do not find the 57-s white dwarf spin period, with a pulse amplitude of 4 mmag, reported by Woudt et al. in either the OM data, which are sensitive to pulse amplitudes 0.03 mag, or the EPIC data, sensitive to pulse fractions p 14 ± 2 per cent.-
dc.descriptionFil: Luna, Gerardo Juan Manuel. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina-
dc.descriptionFil: Diaz, M. P.. Universidade de Sao Paulo; Brasil-
dc.descriptionFil: Brickhouse, N. S.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos-
dc.descriptionFil: Moraes, M.. Universidade de Sao Paulo; Brasil-
dc.formatapplication/pdf-
dc.formatapplication/pdf-
dc.languageeng-
dc.publisherWiley-
dc.relationinfo:eu-repo/semantics/altIdentifier/doi/http://dx.doi.org/10.1111/j.1745-3933.2012.01260.x-
dc.relationinfo:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/1203.4804-
dc.relationinfo:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article-lookup/doi/10.1111/j.1745-3933.2012.01260.x-
dc.rightsinfo:eu-repo/semantics/openAccess-
dc.rightshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/-
dc.sourcereponame:CONICET Digital (CONICET)-
dc.sourceinstname:Consejo Nacional de Investigaciones Científicas y Técnicas-
dc.sourceinstacron:CONICET-
dc.source.urihttp://hdl.handle.net/11336/19303-
dc.subjectnovae-
dc.subjectcataclysmic variables-
dc.subjectX-rays-
dc.subjectgeneral-
dc.subjectAstronomía-
dc.subjectCiencias Físicas-
dc.subjectCIENCIAS NATURALES Y EXACTAS-
dc.titleXMM-Newton EPIC and OM observation of Nova Centauri 1986 (V842 Cen)-
dc.typeinfo:eu-repo/semantics/article-
dc.typeinfo:eu-repo/semantics/publishedVersion-
dc.typeinfo:ar-repo/semantics/articulo-
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