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The recovery of cosmic ray Carbon nuclei of energy ~20-125 MeV/nuc in solarcycle #23 from 2004 to 2010 has been followed at three locations, near theEarth using ACE data and at V2 between 74-92 AU and also at V1 beyond theheliospheric termination shock at between 91-113 AU. To describe the observedintensity changes and to predict the absolute intensities measured at all threelocations we have used a simple spherically symmetric (no drift) two-zoneheliospheric transport model with specific values for the diffusion coefficientin both the inner and outer zones. The diffusion coefficient in the outer zoneis determined to be ~5-10 times smaller than that in the inner zone out to 90AU. For both V1 and V2 the calculated C nuclei intensities agree within anaverage of \pm 10% with the observed intensities. Because of this agreementbetween V1 and V2 observations and predictions there is no need to invoke anasymmetrical squashed heliosphere or other effects to explain the V2intensities relative to V1 as is the case for He nuclei. The combination of thediffusion parameters used in this model and the interstellar spectrum give anunusually low overall solar modulation parameter \phi = 250 MV to describe theCarbon intensities observed at the Earth in 2009. At all times both theobserved and calculated spectra are very closely ~ E1.0 as would be expected inthe adiabatic energy loss regime of solar modulation.

20-125 mev/nuc cosmic ray carbon nuclei intensities between 2004-2010 in  solar cycle #23 as measured near the earth, at voyager 2 and also in the  heliosheath at voyager 1 - modulation in a two zone heliospehre