Core–collapsed supernovae ( CCSNe ) have been considered to be one of sources of dust in the universe .
What kind and how much mass of dust are formed in the ejecta and are injected into the interstellar medium ( ISM ) depend on the type of CCSNe , through the difference in the thickness ( mass ) of outer envelope .
In this review , after summarizing the existing results of observations on dust formation in CCSNe , we investigate formation of dust in the ejecta and its evolution in the supernova remnants ( SNRs ) of Type II–P and Type IIb SNe .
Then , the time evolution of thermal emission from dust in the SNR of Type IIb SN is demonstrated and compared with the observation of Cas A .
We find that the total dust mass formed in the ejecta does not so much depend on the type ; \sim 0.3 - 0.7 M _ { \odot } in Type II–P SNe and \sim 0.13 M _ { \odot } in Type IIb SN .
However the size of dust sensitively depends on the type , being affected by the difference in the gas density in the ejecta : the dust mass is dominated by grains with radii larger than 0.03 \mu m in Type II-P , and less than 0.006 \mu m in Type IIb , which decides the fate of dust in the SNR .
The surviving dust mass is \sim 0.04 - 0.2 M _ { \odot } in the SNRs of Type II–P SNe for the ambient hydrogen density of n _ { H } = 10.0 - 1.0 cm ^ { -3 } , while almost all dust grains are destroyed in the SNR of Type IIb .
The spectral energy distribution ( SED ) of thermal emission from dust in SNR well reflects the evolution of dust grains in SNR through erosion by sputtering and stochastic heating .
The observed SED of Cas A SNR is reasonably reproduced by the model of dust formation and evolution for Type IIb SN .