  High-resolution optical spectra (UES/WHT) of the extreme metal-poor post-AGB
star HR4049 were obtained at four different orbital phases. The spectra cover
the wavelength region from 3650ang to 10850ang at a resolution of R=5.2x10^4.
These observations are supplemented with four high-resolution spectra of the
NaI D1 & D2 and CaII K lines at R=10^5 (CAT/CES). The optical spectrum shows
217 spectral lines: the Balmer series (H alpha - H35), the Paschen series (P9 -
P23), NI, OI and numerous CI lines. We show that the lines of H alpha, H beta,
H gamma and NaI D show significant changes in profile between different
observation dates. Nine components were identified in the profile of the NaI D
lines of which three are circumstellar and six interstellar. The stronger CI
lines are asymmetric and we derive a post-AGB mass-loss of Mdot= 6x10^-7Msol/yr
from the asymmetry. The [OI] 6300ang line has been detected in emission at the
system velocity and we argue that the emission is from an almost edge-on disk
with a radius of about 20 Rstar.
