  RR Tel is an interacting binary system in which a hot white dwarf (WD)
accretes matter from a Mira-type variable star via gravitational capture of its
stellar wind. This symbiotic nova shows intense Raman-scattered O VI 1032\r{A}
and 1038\r{A} features at 6825\r{A} and 7082\r{A}. We present high-resolution
optical spectra of RR Tel taken in 2016 and 2017 with the Magellan Inamori
Kyocera Echelle (MIKE) spectrograph at Magellan-Clay telescope, Chile. We aim
to study the stellar wind accretion in RR Tel from the profile analysis of
Raman O VI features. With an asymmetric O VI disk model, we derive a
representative Keplerian speed of $> 35{\rm km~s^{-1}}$, and the corresponding
scale < 0.8 au. The best-fit for the Raman profiles is obtained with a mass
loss rate of the Mira ${\dot M}\sim2\times10^{-6}~{\rm M_{\odot}~yr^{-1}}$ and
a wind terminal velocity $v_{\infty}\sim 20~{\rm km~s^{-1}}$. We compare the
MIKE data with an archival spectrum taken in 2003 with the Fibre-fed Extended
Range Optical Spectrograph (FEROS) at the MPG/ESO 2.2m telescope. It allows us
to highlight the profile variation of the Raman O VI features, indicative of a
change in the density distribution of the O VI disk in the last two decades. We
also report the detection of O VI recombination lines at 3811\r{A} and
3834\r{A}, which are blended with other emission lines. Our profile
decomposition suggests that the recombination of O VII takes place nearer to
the WD than the O VI 1032\r{A} and 1038\r{A} emission region.
