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AstroSat soft X-ray observations of the symbiotic recurrent nova V3890 Sgr during its 2019 outburst

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dc.contributor.author Singh, K. P
dc.contributor.author Girish, V
dc.contributor.author Pavana, M
dc.contributor.author Ness, J.-U
dc.contributor.author Anupama, G. C
dc.contributor.author Orio, M
dc.date.accessioned 2021-02-14T06:02:58Z
dc.date.available 2021-02-14T06:02:58Z
dc.date.issued 2021-02
dc.identifier.citation Monthly Notices of the Royal Astronomical Society, Vol. 501, No. 1, pp. 36-49 en_US
dc.identifier.issn 1365-2966
dc.identifier.uri http://hdl.handle.net/2248/7627
dc.description Restricted Access © The Royal Astronomical Society https://doi.org/10.1093/mnras/staa3303 en_US
dc.description.abstract Two long AstroSat Soft X-ray Telescope observations were taken of the third recorded outburst of the symbiotic recurrent nova V3890 Sgr. The first observing run, 8.1–9.9 d after the outburst, initially showed a stable intensity level with a hard X-ray spectrum that we attribute to shocks between the nova ejecta and the pre-existing stellar companion. On day 8.57, the first, weak, signs appeared of supersoft source (SSS) emission powered by residual burning on the surface of the white dwarf. The SSS emission was observed to be highly variable on time-scales of hours. After day 8.9, the SSS component was more stable and brighter. In the second observing run, on days 15.9–19.6 after the outburst, the SSS component was even brighter but still highly variable. The SSS emission was observed to fade significantly during days 16.8–17.8 followed by re-brightening. Meanwhile, the shock component was stable, leading to increase in hardness ratio during the period of fading. AstroSat and XMM–Newton observations have been used to study the spectral properties of V3890 Sgr to draw quantitative conclusions even if their drawback is model dependent. We used the XSPEC to fit spectral models of plasma emission, and the best fits are consistent with the elemental abundances being lower during the second observing run compared to the first for spectra ≥1 keV. The SSS emission is well fitted by non-local thermal equilibrium model atmosphere used for white dwarfs. The resulting spectral parameters, however, are subject to systematic uncertainties such as completeness of atomic data. en_US
dc.language.iso en en_US
dc.publisher Oxford University Press on behalf of the Royal Astronomical Society en_US
dc.subject stars: abundances en_US
dc.subject (stars:) nova en_US
dc.subject cataclysmic variables en_US
dc.subject X-rays: stars en_US
dc.subject novae: individual (V3890 Sgr) en_US
dc.title AstroSat soft X-ray observations of the symbiotic recurrent nova V3890 Sgr during its 2019 outburst en_US
dc.type Article en_US

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