2006MNRAS.371..424L

The classical nova V4743 Sgr was observed with XMM-Newton for about 10h on 2003 April 4, 6.5 months after optical maximum. At this time, this nova had become the brightest supersoft X-ray source ever observed. In this paper, we present the results of a time-series analysis performed on the X-ray light curve (LC) obtained in this observation, and in a previous shorter observation done with Chandra 16d earlier. Intense variability, with amplitude as large as 40 per cent of the total flux, was observed both times. Similarities can be found between the two observations in the structure of the variations. Most of the variability is well represented as a combination of oscillations at a set of discrete frequencies lower than 1.7mHz. At least five frequencies are constant over the 16d time interval between the two observations. We suggest that a period in the power spectrum of both LCs at the frequency of 0.75mHz and its first harmonic are related to the spin period of the white dwarf (WD) in the system, and that other observed frequencies are signatures of non-radial WD pulsations. A possible signal with a 24000s period is also found in the XMM-Newton LC: a cycle and a half are clearly identified. This period is consistent with the 24278s periodicity discovered in the optical LC of the source and thought to be the orbital period of the nova binary stellar system.