Formation of Dust in the Ejecta of Type Ia Supernovae

摘要: We investigate the formation of dust grains in ejecta Type Ia supernovae (SNe Ia), adopting carbon-deflagration W7 model. In calculations formation, we apply nucleation and grain growth theory consider two extreme cases CO SiO molecules: complete no formation. The results show that for sticking probability ? j = 1, C, silicate, Si, FeS can condense at early times ~100-300?days after explosion, whereas Fe SiC cannot form substantially. Due to low gas density SNe with H-envelope, average radii newly formed are generally below 0.01 ?m, being much smaller than those II-P SNe. This supports our previous conclusion radius is less massive envelopes. total mass ranges from 3 10?4 M 0.2 0.1-1, depending on whether or not molecules formed. also estimate optical depths thermal emission by compare them relevant observations Ia. find C must be suppressed consistent observational constraints. implies energetic photons electrons heavily depress efficiency outermost C-O layer almost fully burned. Finally, calculate destruction SN remnants completely destroyed shocked before injected into interstellar medium. indicates unlikely major sources dust.