  We present optical and NIR spectroscopic observations of U Sco 2010 outburst.
From the analysis of lines profiles we identify a broad and a narrow component
and show that the latter originates from the reforming accretion disk. We show
that the accretion resumes shortly after the outburst, on day +8, roughly when
the super-soft (SSS) X-ray phase starts. Consequently U Sco SSS phase is fueled
(in part or fully) by accretion and should not be used to estimate
$m_{\mathrm{rem}}$, the mass of accreted material which has not been ejected
during the outburst. In addition, most of the He emission lines, and the HeII
lies in particular, form in the accretion flow/disk within the binary and are
optically thick, thus preventing an accurate abundance determination.
  A late spectrum taken in quiescence and during eclipse shows CaII H&K, the
G-band and MgI b absorption from the secondary star. However, no other
significant secondary star features have been observed at longer wavelengths
and in the NIR band.
