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The symbiotic nova V745 Sco was observed in outburst on 2014 February 6. Itsobservations by the Chandra X-ray Observatory at days 16 and 17 have revealed aspectrum characterized by asymmetric and blue-shifted emission lines. Here weinvestigate the origin of these asymmetries through three-dimensionalhydrodynamic simulations describing the outburst during the first 20 days ofevolution. The model takes into account thermal conduction and radiativecooling and assumes a blast wave propagates through an equatorial densityenhancement. From the simulations, we synthesize the X-ray emission and derivethe spectra as they would be observed with Chandra. We find that both the blastwave and the ejecta distribution are efficiently collimated in polar directionsdue to the presence of the equatorial density enhancement. The majority of theX-ray emission originates from the interaction of the blast with the equatorialdensity enhancement and is concentrated on the equatorial plane as a ring-likestructure. Our "best-fit" model requires a mass of ejecta in the outburst$M_{ej} \approx 3\times 10^{-7}\,M_{\odot}$ and an explosion energy $E_b\approx 3 \times 10^{43}$ erg and reproduces the distribution of emissionmeasure vs temperature and the evolution of shock velocity and temperatureinferred from the observations. The model predicts asymmetric and blue-shiftedline profiles similar to those observed and explains their origin as due tosubstantial X-ray absorption of red-shifted emission by ejecta material. Thecomparison of predicted and observed Ne and O spectral line ratios reveals nosigns of strong Ne enhancement and suggests the progenitor is a CO white dwarf.

Origin of asymmetries in X-ray emission lines from the blast wave of the 2014 outburst of nova V745 Sco