  High-resolution optical spectra of R CrB obtained in 2003 March is discussed.
The 2003 spectra are compared with the extensive collection of spectra from the
1995-1996 minimum. Spectroscopic features common to the two minima include
sharp emission lines of neutral and singly-ionized atoms, broad emission lines
including He {\sc i}, [N {\sc ii}] 6583 \AA, Na D, and Ca {\sc ii} H & K lines,
and blueshifted aborption lines of Na D, and K {\sc i} resonance lines.
Prominent differences between the 2003 and 1995-96 spectra are seen. The 2003
profiles of Na D, Ca II H & K are fit by a single Gaussian but in 1995-1996 two
Gaussians separated by about 200 km s$^{-1}$ were required. However, the He
{\sc i} broad emission lines are fit by a single Gaussian at all times; the
emitting He and Na-Ca atoms are probably not colocated. The C$_2$ Phillips 2-0
lines are detected as sharp absorption lines in 2003 indicating presence of gas
at 1300 K.The 2003 spectra show C {\sc i} sharp emission lines at minimum light
with a velocity changing in five days by about 20 km s$^{-1}$ when the velocity
of `metal' sharp lines is unchanged; the C {\sc i} emission may arise from
shock-heated gas. Spectra at maximum shows extended blue wings to strong lines
with the extension dependent on a line's lower excitation potential a signature
of stellar wind. Changes in the cores of the resonance lines of Al {\sc i} and
Na D and the Ca {\sc ii} IR lines suggest complex flow patterns near the
photosphere. The spectroscopic differences at the two mimima show the
importance of continued scrutiny of the declines of R CrB.
