In D-term inflation models, the fluctuations fo squark fields in the flat directions give rise to isocurvature density fluctuations stored in the Affleck-Dine condensate. After the condensate break up in B-balls, these can be perturbations in the baryon number, or, in the case where the present neutralino density comes directly from B-ball decay, perturbations in the number of dark matter neutralinos. The latter case results in a large enhancement of the isocurvature perturbation. In this case, the requirement that the deviation of the adiabatic perturbations from scale invariance due to hte Affleck-Dine field is not too large imposes a lower bound on the magnitude of the isocurvature fluctuation of about 10~-2 times the adiabatic perturbation. This should be observable by MAP and PLANCK.
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