Formation and Evolution of Dust in Various Types of Supernovae

We demonstrate how the formation and destruction processes of dust in supernovae (SNe) depend on the type of SNe classified through the mass of their outer envelopes. We show that, for Type II-P SNe with massive hydrogen envelopes, relatively large grains (greater than or similar to 0.01 mu m) can condense in the ejecta, and that similar to 0.1-1 M-circle dot of dust can be injected into the interstellar medium. On the other hand, for Type IIb/Ib/Ia SNe with no massive envelope, the radii of newly formed grains are considerably small, less than 0.01 mu m, so the dust grains are almost completely destroyed in the shocked hot gas. These results suggest that envelope-retaining SNe can be major sources of dust, whereas envelope-deficient SNe are likely to be minor dust sources.