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Evolution of broad-band SED during outburst rise in NS X-ray Nova Aql X-1

Tsygankov SS; Vlasyuk VV; Khamitov IM; Bikmaev IF; Shakura NI; Meshcheryakov AV; Pavlinsky MN; Eselevich MV

dc.contributor.authorTsygankov SS
dc.contributor.authorVlasyuk VV
dc.contributor.authorKhamitov IM
dc.contributor.authorBikmaev IF
dc.contributor.authorShakura NI
dc.contributor.authorMeshcheryakov AV
dc.contributor.authorPavlinsky MN
dc.contributor.authorEselevich MV
dc.date.accessioned2022-10-27T11:49:05Z
dc.date.available2022-10-27T11:49:05Z
dc.identifier.urihttps://www.utupub.fi/handle/10024/155152
dc.description.abstractThe observed evolution of the broad-band spectral energy distribution (SED) in NS X-ray Nova Aql X-1 during the rise phase of a bright Fast-Rise-Exponential-Decay-type outburst in 2013 can be understood in the framework of thermal emission from non-stationary accretion disc with radial temperature distribution transforming from a single-temperature blackbody emitting ring into the multicolour irradiated accretion disc. SED evolution during the hard to soft X-ray state transition looks unusual, as it cannot be reproduced by the standard disc irradiation model with a single irradiation parameter for NUV, Optical and NIR spectral bands. NIR (NUV) band is correlated with soft (hard) X-ray flux changes during the state transition interval, respectively. In our interpretation, at the moment of X-ray state transition UV-emitting parts of the accretion disc are screened from direct X-ray illumination from the central source and are heated primarily by hard X-rays (E > 10 keV), scattered in the hot corona or wind possibly formed above the optically thick outer accretion flow; the outer edge of multicolour disc, which emits in Optical-NIR, can be heated primarily by direct X-ray illumination. We point out that future simultaneous multiwavelength observations of X-ray Nova systems during the fast X-ray state transition interval are of great importance, as it can serve as 'X-ray tomograph' to study physical conditions in outer regions of accretion flow. This can provide an effective tool to directly test the energy-dependent X-ray heating efficiency, vertical structure and accretion flow geometry in transient low-mass X-ray binaries.
dc.language.isoen
dc.publisherOXFORD UNIV PRESS
dc.titleEvolution of broad-band SED during outburst rise in NS X-ray Nova Aql X-1
dc.identifier.urlhttps://academic.oup.com/mnras/article/473/3/3987/4331644#
dc.identifier.urnURN:NBN:fi-fe2021042718905
dc.relation.volume473
dc.contributor.organizationfi=Tuorlan observatorio|en=Tuorla Observatory|
dc.contributor.organization-code2606705
dc.converis.publication-id30311303
dc.converis.urlhttps://research.utu.fi/converis/portal/Publication/30311303
dc.format.pagerange4002
dc.format.pagerange3987
dc.identifier.eissn1365-2966
dc.identifier.jour-issn0035-8711
dc.okm.affiliatedauthorTsygankov, Sergey
dc.okm.discipline115 Astronomy and space scienceen_GB
dc.okm.discipline115 Avaruustieteet ja tähtitiedefi_FI
dc.okm.internationalcopublicationinternational co-publication
dc.okm.internationalityInternational publication
dc.okm.typeJournal article
dc.publisher.countryUnited Kingdomen_GB
dc.publisher.countryBritanniafi_FI
dc.publisher.country-codeGB
dc.publisher.placeOxford
dc.relation.doi10.1093/mnras/stx2565
dc.relation.ispartofjournalMonthly Notices of the Royal Astronomical Society
dc.relation.issue3
dc.year.issued2018


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