  We have used corresponding marker features in the intensity vs. time profile
of termination shock particles coming from within the heliosheath and also 5-12
MeV electrons which are coming from beyond the heliopause that are both
observed at both V1 and V2 in the outer N and S heliosheaths, to estimate the
thickness of the S heliosheath. These features in the N heliosheath have been
observed on the CRS instrument on V1 in the N heliosheath beyond 110 AU or
within 12 AU of the heliopause. Although the intensity-time features in the S
heliosheath are quite different overall, certain features stand out at both V1
and V2. The correspondence of these features in the N and S heliosheath allows
us to estimate that V2 will reach the S heliopause near the end of 2014.
