The proposed Interstellar Probe mission (ISP) will have unprecedented
capabilities to detect and characterize interstellar dust flowing into
the heliosphere from the surrounding interstellar medium (ISM).
Knowledge of that dust has the potential to substantially advance our
understanding of interstellar dust in general and the local ISM in
particular. However, the flux of dust that can be observed varies due to
the evolving heliosphere and the interaction of the charged grains with
the heliospheric magnetic field. We will present the results of
calculations of the dust density relative to that in the pristine ISM as
a function of time and position for a possible trajectory of ISP. We
will show how different polarities of the solar wind magnetic field
affect the observed flux and how these depend on distance from the Sun.