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We have analysed a series of Suzaku data and one dataset of XMM-Newton of theSU UMa type dwarf nova VW Hyi in optical quiescence. The observed spectra inthe 0.2-10 keV band are moderately well represented by multi-temperaturethermal plasma emission models with a maximum temperature of 5-9 keV andbolometric luminosity of 2.4-5.2 $\times$ 10$^{30}$ erg s$^{-1}$. The massaccretion rate derived from the hard X-ray spectra does not show any cleartrend as a function of time since the last superoutburst, in contradiction totheoretical predictions of the disc behaviour of a SU UMa type dwarf nova. Themass accretion rate, on the other hand, shows a clear declining trend with timesince the last outburst (including the superoutburst). The rate of decline isof the same order as that evaluated from the hard X-ray light curves of theother two dwarf novae SS Cyg and SU UMa. The standard disc instability model,on the other hand, predicts that the mass accretion rate should increasethroughout the optically-quiescent phase. We need further observation andtheoretical consideration to resolve this discrepancy.

Variation of mass accretion rate onto the white dwarf in the dwarf nova VW Hyi in quiescence