| Abstract: | We deduce the mass distribution and total mass density of interstellar dust streaming into the solar system and compare the
results to the conditions of the very local interstellar medium (VLISM). The mass distribution derived from in situ measurements
shows a gentler slope and includes larger grains, compared to a model distribution proposed for the wavelength dependence
of the interstellar extinction. The mass density of grains in the solar system is consistent with that expected from measurements
of the visible interstellar extinction and the abundance constraints of elements in the diffuse interstellar medium (ISM),
instead of those in the VLISM. This may imply that interstellar dust grains are not associated with the VLISM and that the
conditions of the grains are better represented by the ones expected in the diffuse ISM. If this is the case, then the flatter
slope in the mass distribution and the detection of larger interstellar grains in the solar system may even indicate that
coagulation growth of dust in the diffuse ISM is more effective than previously inferred.
This revised version was published online in July 2006 with corrections to the Cover Date. |
