  We present a model-independent technique for calculating the time of
mid-transits. This technique, named "barycenter method", uses the light-curve's
symmetry to determine the transit timing by calculating the transit light-curve
barycenter. Unlike the other methods of calculating mid-transit timing, this
technique does not depend on the parameters of the system and central star. We
demonstrate the capabilities of the barycenter method by applying this
technique to some known transiting systems including several \emph{Kepler}
confirmed planets. Results indicate that for complete and symmetric transit
lightcurves, the barycenter method achieves the same precision as other
techniques, but with fewer assumptions and much faster. Among the transiting
systems studied with the barycenter method, we focus in particular on LHS
6343C, a brown dwarf that transits a member of an M+M binary system, LHS
6343AB. We present the results of our analysis, which can be used to set an
upper limit on the period and mass of a possible second small perturber.
