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RT Crucis: A look into the X-ray emission of a peculiar symbiotic star
Authors
Doroshenko V.
Ducci L.
+4 more
Ferrigno C.
Nikołajuk M.
Santangelo A.
Suleimanov V.
Publication date
1 January 2016
Publisher
Abstract
© 2016 ESO.Symbiotic stars are a heterogeneous class of interacting binaries. Among them, RT Cru has been classified as prototype of a subclass that is characterised by hard X-ray spectra that extend past ∼20 keV. We analyse ∼8.6 Ms of archival INTEGRAL data collected during the period 2003-2014, ∼ 140 ks of Swift/XRT data, and a Suzaku observation of 39 ks, to study the spectral X-ray emission and investigate the nature of the compact object. Based on the 2MASS photometry, we estimate the distance to the source of 1.2-2.4 kpc. The X-ray spectrum obtained with Swift/XRT, JEM-X, IBIS/ISGRI, and Suzaku data is well fitted by a cooling flow model modified by an absorber that fully covers the source and two partially covering absorbers. Assuming that the hard X-ray emission of RT Cru originates from an optically thin boundary layer around a non-magnetic white dwarf, we estimated a mass of the white dwarf of MWD ≈ 1.2M⊙. The mass accretion rate obtained for this source might be too high for the optically thin boundary layer scenario. Therefore we investigate other plausible scenarios to model its hard X-ray emission. We show that, alternatively, the observed X-ray spectrum can be explained with the X-ray emission from the post-shock region above the polar caps of a magnetised white dwarf with mass MWD ≈ 0.9-1.1M⊙
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Kazan Federal University Digital Repository
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oai:dspace.kpfu.ru:net/105002
Last time updated on 07/05/2019
Kazan Federal University Digital Repository
See this paper in CORE
Go to the repository landing page
Download from data provider
oai:dspace.kpfu.ru:net/142527
Last time updated on 07/05/2019