Fig. 5.

Grain mass distribution for interstellar grains in the heliosphere observed by the Ulysses and Galileo spacecrafts (updated, H. Krueger private communication). As an example, the purple line shows the MRN power law size distribution (Mathis et al., 1977) but with higher upper and lower size cutoffs and using a gas-to-dust mass ratio of 150. The blue points show the grain mass distribution that results in our model (focusing SWMF). This model clearly overpredicts the density of large grains, but is promising for linking the observed grain size distribution with the initial one in the Local Interstellar Cloud.