Tidal tails of open clusters are the result of the stellar evaporation from the cluster due to the Galactic potential and the internal dynamics. With the recent availability of high precision data, tidal tails are being detected for most of the nearby open clusters. In this work, we aim to identify the tidal tail members for all open clusters within a distance of 400 pc which are older than 100 Myr and have >100 members using model-independent methods. We used the convergent point method to identify the co-moving stars near the open clusters using Gaia DR3 data. A new method called "self compact convergent point method" was proposed and applied to some of the clusters which performed better in tracing the tails. We also analysed the colour-magnitude diagrams and orbital energy to diagnose possible contamination. 19 out of 21 clusters have tidal tails. 5 of them have been discovered for the first time through this work. The typical span of the tidal tails is 20-200 pc with 30-700 member stars in the region inside the tidal radius and the tidal tails. 4 out of 19 tidal tails are tilted away from direction of the Galactic Centre which defy the known theory of the formation of the tidal tails. The luminosity function of the tails and clusters are consistent with each other and with the canonical stellar IMF, while systematically larger trailing tail radial velocities than the leading tail radial velocities were observed for the first time. The convergent point method is useful to detect tidal tails on ~=100pc scale for clusters closer than 400pc. Further analysis of theoretical N-body models is required to understand the incompleteness and biases in the current sample of tidal tails.