  We present new results on the classical T Tauri star RU Lupi based on three
observing runs collecting high-resolution spectra, complementary NIR spectra,
multicolour photometric data, and X-ray observations. The photospheric
absorption lines are weakened. This veiling becomes extremely strong on
occasion, and we show that this effect is due to narrow emission lines that
fill in the photospheric lines. The blue-shifted wings in the optical emission
lines of He I, attributed to a stellar wind, are remarkably stable in
equivalent width. In contrast, the red-shifted wings change dramatically in
strength depending on rotational phase. From the pattern of variability we
infer that these wings originate in accreting gas close to the star, and that
the accretion funnels are bent and trail the hot spot. Forbidden emission lines
are very stable over the entire observing period and originate in the disk
wind. A system of narrow blue-shifted absorption features seen in lines of Ca
II and Na I can be traced to a disk wind as well. Slightly blue-shifted
emission components are present in the forbidden lines and might be related to
a wide angle molecular disk wind.
