Astronomy and Astrophysics, volume 592A, 58-58 (2016/8-1)
RT Crucis: a look into the X-ray emission of a peculiar symbiotic star.
DUCCI L., DOROSHENKO V., SULEIMANOV V., NIKOLAJUK M., SANTANGELO A. and FERRIGNO C.
Abstract (from CDS):
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 ∼20keV. We analyse ∼8.6Ms of archival INTEGRAL data collected during the period 2003-2014, ∼140ks of Swift/XRT data, and a Suzaku observation of 39ks, 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 1.2-2.4kpc. 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☉.
© ESO, 2016
X-rays: binaries - white dwarfs - stars: individual: RT Cru - stars: individual: IGR J12349-6434
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