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We aim to probe the dynamic structure of the extended Solar neighbourhood bycalculating the radial metallicity gradients from orbit properties, which areobtained for axisymmetric and non-axisymmetric potential models, of red clump(RC) stars selected from the RAdial Velocity Experiment's Fourth Data Release.Distances are obtained by assuming a single absolute magnitude value innear-infrared, i.e. $M_{Ks}=-1.54\pm0.04$ mag, for each RC star. Stellar orbitparameters are calculated by using the potential functions: (i) for theMWPotential2014 potential, (ii) for the same potential with perturbationfunctions of the Galactic bar and transient spiral arms. The stellar age iscalculated with a method based on Bayesian statistics. The radial metallicitygradients are evaluated based on the maximum vertical distance ($z_{max}$) fromthe Galactic plane and the planar eccentricity ($e_p$) of RC stars for both ofthe potential models. The largest radial metallicity gradient in the $0<z_{max}\leq0.5$ kpc distance interval is $-0.065\pm0.005$ dex kpc$^{-1}$ for asubsample with $e_p\leq0.1$, while the lowest value is $-0.014\pm0.006$ dexkpc$^{-1}$ for the subsample with $e_p\leq0.5$. We find that at $z_{max}>1$kpc, the radial metallicity gradients have zero or positive values and they donot depend on $e_p$ subsamples. There is a large radial metallicity gradientfor thin disc, but no radial gradient found for thick disc. Moreover, thelargest radial metallicity gradients are obtained where the outer Lindbladresonance region is effective. We claim that this apparent change in radialmetallicity gradients in the thin disc is a result of orbital perturbationoriginating from the existing resonance regions.

Local Stellar Kinematics from RAVE data -- VIII. Effects of the Galactic Disc Perturbations on Stellar Orbits of Red Clump Stars