  A five year CCD photometric \emph{VI} time-series of NGC 7006 is employed to
perform a detailed analysis of the known population of variable stars. In the
process we have corrected inconsistent classifications, sky coordinates and
found ten new cluster member variables. An independent reddening estimate with
a value $E(B-V)=0.08\pm0.05$ is made. Using Fourier decompositions of RR Lyrae
light curves and well established calibrations, the cluster mean metallicity
and distance [Fe/H]$_{\rm ZW}= -1.53\pm0.15$ and $41.2\pm1.4$ kpc are estimated
based on an extended sample of cluster member RRab stars. Using the $Gaia$-DR3
data we performed an extensive membership analysis which leads to a clean
Colour-Magnitude diagram, and hence to the identification of variables that are
likely field stars, and to considerations on the variables distribution in the
Horizontal Branch (HB). A double mode RR Lyrae and three CW star are discussed.
The origin of CW stars from precursors in the blue tail of the HB with very
thin ($\sim 0.06 \pm 0.01 M_{\odot}$) envelopes is argued. Our models indicate
that the Main Sequence predecessor of RR Lyrae stars had a mass of 0.82-0.85
$M_{\odot}$ and lost about 25-35\% of its mass during the red giant branch
events before settling in the HB some 12-13.5 Gyrs later.
