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Eight X-ray observations of V4743 Sgr (2002), observed with Chandra andXMM-Newton are presented. The nova turned off some time between days 301.9 and371, and the X-ray flux subsequently decreased from day 301.9 to 526 followingan exponential decline time scale of $(96 \pm 3)$ days. We use the absorptionlines present in the SSS spectrum for diagnostic purposes, and characterize thephysics and the dynamics of the expanding atmosphere during the explosion ofthe nova. The information extracted from this first stage is then used as inputfor computing full photoionization models of the ejecta in V4743 Sgr. The SSSspectrum is modeled with a simple black-body and multiplicative Gaussian lines,which provides us of a general kinematical picture of the system, before itdecays to its faint phase (Ness et al. 2003). In the grating spectra takenbetween days 180.4 and 370, we can resolve the line profiles of absorptionlines arising from H-like and He-like C, N, and O, including transitionsinvolving higher principal quantum numbers. Except for a few interstellarlines, all lines are significantly blue-shifted, yielding velocities between1000 and 6000 km/s which implies an ongoing mass loss. It is shown thatsignificant expansion and mass loss occur during this phase of the explosion,at a rate $\dot{M} \approx (3-5) \times 10^{-4} ~ (\frac{L}{L_{38}}) ~M_{\odot}/yr$. Our measurements show that the efficiency of the amount ofenergy used for the motion of the ejecta, defined as the ratio between thekinetic luminosity $L_{\rm kin}$ and the radiated luminosity $L_{\rm rad}$, isof the order of one.

Astrophysical Fluids of Novae: High Resolution Pre-decay X-ray spectrum of V4743 Sagittarii