We present new high-resolution spectroscopic observations ( \lambda / \Delta \lambda \approx 40000 ) of 18 bright northern Cepheids carried out at David Dunlap Observatory , in 1997 .
The measurements mainly extend those of presented in Paper I ( Kiss 1998 ) adding three more stars ( AW Per , SV Vul , T Mon ) .
The spectra were obtained in the yellow-red spectral region in the interval of 5900 Å and 6660 Å , including strong lines of sodium D and H \alpha .
New radial velocities determined with the cross-correlation technique and the bisector technique are presented .
The new data are compared with those recently published by several groups .
We found systematic differences between the spectroscopic and CORAVEL-type measurements as large as 1–3 km s ^ { -1 } in certain phases .

We performed Baade-Wesselink analysis for CK Cam discovered by the Hipparcos satellite .
The resulting radius is 31 \pm 1 R _ { \odot } , which is in very good agreement with recent period-radius relation by Gieren et al .
( 1999 ) .
It is shown that the systematic velocity differences do not affect the Baade-Wesselink radius more than 1 % for CK Cam .

Observational pieces of evidence of possible velocity gradient affecting the individual line profiles are studied .
The full-width at half minimum ( FWHM ) of the metallic lines , similarly to the velocity differences , shows a very characteristic phase dependence , illustrating the effect of global compression in the atmosphere .
The smallest line widths always occur around the maximal radius , while the largest FWHM is associated with the velocity reversal before the minimal radius .
Three first overtone pulsators do not follow the general trend : the largest FWHM in SU Cas and SZ Tau occurs after the smallest radius , during the expansion , while in V1334 Cyg there are only barely visible FWHM-variations .
The possibility of a bright yellow companion of V1334 Cyg is briefly discussed .
The observed line profile asymmetries exceed the values predicted with a simple projection effect by a factor of 2–3 .
This could be associated with the velocity gradient , which is also supported by the differences between individual line velocities of different excitation potentials .