The Sun's velocity relative to the Local Standard of Rest (LSR) is crucial for transforming observed heliocentric velocities into a local galactic frame. The classical method for determining the solar motion uses Strömberg's relation, which links the mean heliocentric azimuthal velocity of a stellar sample to its velocity dispersion. However, this method is flawed due to the metallicity gradient in the Galactic disc, which introduces a correlation between the colour of a group of stars and radial gradients of their properties. A chemodynamical model, SB09a, was used to re-examine the local stellar kinematics and determine the solar motion. The results show that the solar motion components are (U,V,W) = (11.1±0.69, 12.24±0.47, 7.25±0.37) km/s, with additional systematic uncertainties of ~ (1, 2, 0.5) km/s. The V component is 7 km/s larger than previously estimated. The new values are insensitive to the metallicity gradient in the disc. The classical method is invalid because the metallicity gradient causes the relationship between mean rotation speed and velocity dispersion to deviate from the linear form predicted by Strömberg's relation. The SB09a model predicts that a linear relationship underestimating the solar azimuthal motion by ~7 km/s will be mimicked redwards of the turnoff region, consistent with Hipparcos data. The solar motion components agree with earlier estimates, but the V component is larger than the DB98 value by ~7 km/s. This is in agreement with model expectations for systematic errors from using Strömberg's relation and with the value obtained by B09. The result is not sensitive to assumptions about star formation and chemical evolution in SB09a. Further revisions in the solar motion value are expected as more elaborate models are developed.The Sun's velocity relative to the Local Standard of Rest (LSR) is crucial for transforming observed heliocentric velocities into a local galactic frame. The classical method for determining the solar motion uses Strömberg's relation, which links the mean heliocentric azimuthal velocity of a stellar sample to its velocity dispersion. However, this method is flawed due to the metallicity gradient in the Galactic disc, which introduces a correlation between the colour of a group of stars and radial gradients of their properties. A chemodynamical model, SB09a, was used to re-examine the local stellar kinematics and determine the solar motion. The results show that the solar motion components are (U,V,W) = (11.1±0.69, 12.24±0.47, 7.25±0.37) km/s, with additional systematic uncertainties of ~ (1, 2, 0.5) km/s. The V component is 7 km/s larger than previously estimated. The new values are insensitive to the metallicity gradient in the disc. The classical method is invalid because the metallicity gradient causes the relationship between mean rotation speed and velocity dispersion to deviate from the linear form predicted by Strömberg's relation. The SB09a model predicts that a linear relationship underestimating the solar azimuthal motion by ~7 km/s will be mimicked redwards of the turnoff region, consistent with Hipparcos data. The solar motion components agree with earlier estimates, but the V component is larger than the DB98 value by ~7 km/s. This is in agreement with model expectations for systematic errors from using Strömberg's relation and with the value obtained by B09. The result is not sensitive to assumptions about star formation and chemical evolution in SB09a. Further revisions in the solar motion value are expected as more elaborate models are developed.