Context : The determination of the local standard of rest ( LSR ) , which corresponds to the measurement of the peculiar motion of the Sun based on the derivation of the asymmetric drift of stellar populations , is still a matter of debate .
The classical value of the tangential peculiar motion of the Sun with respect to the LSR was challenged in recent years , claiming a significantly larger value .

Aims : We present an improved Jeans analysis , which allows a better interpretation of the measured kinematics of stellar populations in the Milky Way disc .
We show that the RAdial Velocity Experiment ( RAVE ) sample of dwarf stars is an excellent data set to derive tighter boundary conditions to chemodynamical evolution models of the extended solar neighbourhood .

Methods : We propose an improved version of the Strömberg relation with the radial scalelengths as the only unknown .
We redetermine the asymmetric drift and the LSR for dwarf stars based on RAVE data .
Additionally , we discuss the impact of adopting a different LSR value on the individual scalelengths of the subpopulations .

Results : Binning RAVE stars in metallicity reveals a bigger asymmetric drift ( corresponding to a smaller radial scalelength ) for more metal-rich populations .
With the standard assumption of velocity-dispersion independent radial scalelengths in each metallicity bin , we redetermine the LSR .
The new Strömberg equation yields a joint LSR value of V _ { \mathrm { \sun } } = 3.06 \pm 0.68 km s ^ { -1 } , which is even smaller than the classical value based on Hipparcos data .
The corresponding radial scalelength increases from 1.6 kpc for the metal-rich bin to 2.9 kpc for the metal-poor bin , with a trend of an even larger scalelength for young metal-poor stars .
When adopting the recent Schönrich value of V _ { \mathrm { \sun } } = 12.24 km s ^ { -1 } for the LSR , the new Strömberg equation yields much larger individual radial scalelengths of the RAVE subpopulations , which seem unphysical in part .

Conclusions : The new Strömberg equation allows a cleaner interpretation of the kinematic data of disc stars in terms of radial scalelengths .
Lifting the LSR value by a few km s ^ { -1 } compared to the classical value results in strongly increased radial scalelengths with a trend of smaller values for larger velocity dispersions .