Nearby stars have two properties that make them potentially useful as gravitational lenses. The first is that their proximity makes their Einstein radius for very distant sources large enough to be resolved by modern telescopes. When the distance between the source and lens \(D_{\rm LS} \approx D_{\rm S}\), the distance to the source, we are in the mesolensing regime: \[\theta_E = \sqrt{\frac{4GM}{c^2} \frac{D_{\rm LS}}{D_{\rm L}D_{\rm S}}} \approx 90.3 \mbox{mas} \sqrt{\frac{(M/M_\odot)}{(D_{\rm L}/\mbox{pc})}}\]
The second is that their high proper motions mean they will lens very faint, extragalactic background sources more frequently than more distant stars.
The possibility of mesolensing by vB10 was discussed by \citep{L_pine_2012}, and the overall statistics of detecting such events has been analyzed by \cite{Di_Stefano_2008,Di_Stefano_2008a}.