The large-scale morphology of the radio jets in microquasar GRS 1758-258 has been changing in the last decades. Available radio maps show hints of apparent precession. Here, we fit data with a simple kinematical model and perform an analysis of the possible origins and implications of precession in this system. From our study, that includes an additional observing epoch, we are able to confirm the previous detection of changes in the radio jets of GRS 1758-258 far from the core. However, we tentatively suggest that these changes are more probably due to instabilities instead of jet precession.