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The recovery of cosmic ray protons of energy ~150-250 MeV/nuc in solar cycle#23 from 2004 to 2010 has been followed at the Earth using IMP, ACE and balloondata and also at V2 between 74-92 AU and at V1 beyond the heliospherictermination shock (91-113 AU). The correlation coefficient between theintensities the Earth and V1 during this time period, is 0.936, allowing for a~0.9 year delay due to the solar wind propagation time from the Earth to theouter heliosphere. To describe these intensity changes and to predict theabsolute intensities measured at all three locations we have used a simplespherically symmetric (no drift) two-zone heliospheric transport model withspecific values for the diffusion coefficient in both the inner and outerzones. The diffusion coefficient in the outer zone, from about 90 to 120 (130)AU, is determined to be ~5-10 times smaller than that in the inner zone out to90 AU. This means that the outer zone acts much like a diffusing barrier inthis model. The absolute magnitude of the intensities and the intensity changesat V1 and the Earth are described to within a few percent by a diffusioncoefficient that varies with time by a factor ~4 in the inner zone and only~1.8 (1.25) in the outer zone over the time period from 2004-2010. Thesediffusion coefficients and their variations are essentially the same as thosederived earlier from a similar study using He nuclei of the same energy. Thismodel and the diffusion coefficients used provide a total modulation potentialat the Earth ~250 MV in 2009. The difference ~10-20% between calculated andobserved intensities at V2 can be explained if the heliosphere is squashed by~10% in distance (non-spherical) so that the HTS is closer to the Sun in thedirection of V2 compared to V1.

Recovery of 150-250 MeV Cosmic Ray Proton Intensities Between 2004-2010  as Measured Near the Earth, at Voyager 2 and also in the Heliosheath at  Voyager 1 - A Two Zone Heliosphere