The Most Completely Observed Characteristics of Interstellar Grains are their ability to dim and polarize the light of distant stars in our own galaxy. The principal limitation in previous theoretical models of interstellar dust clouds has been the fact that the extinction and polarization have been calculated for different particles, the connection between these types of particles being semiquantitative at best. A knowledge of the electromagnetic scattering properties of the various proposed grains is a fundamental ingredient of any theory of extinction and polarization. All the types of grains which have been suggested, except those of reference 1, scatter electromagnetic radiation by a classical process, i.e., a process which is characterized by a classical application of Maxwell's equations and for which the particles are defined by a size, shape, and index of refraction. In spite of the fact that the methods of application of the classical theory are completely understood, numerical results for the particular range of application which appears to be needed in the interstellar dust problem have been somewhat limited.