Core-collapse supernovae (CCSNe) produce large ($\gtrsim 0.1 \, {\rm M}_\odot$) masses of dust, and are potentially the primary source of dust in the Universe, but much of this dust may be destroyed before reaching the interstellar medium. Cassiopeia A (Cas A) is the only supernova remnant where an observational measurement of the dust destruction efficiency in the reverse shock is possible at present. We determine the pre- and post-shock dust masses in Cas A using a substantially improved dust emission model. In our preferred models, the unshocked ejecta contains $0.6-0.8 \, {\rm M}_\odot$ of $0.1 \, {\rm μm}$ silicate grains, while the post-shock ejecta has $0.02-0.09 \, {\rm M}_\odot$ of $5-10 {\, {\rm nm}}$ grains in dense clumps, and $2 \times 10^{-3} \, {\rm M}_\odot$ of $0.1 \, {\rm μm}$ grains in the diffuse X-ray emitting shocked ejecta. The implied dust destruction efficiency is $74-94 \%$ in the clumps and $92-98 \%$ overall, giving Cas A a final dust yield of $0.05-0.30 \, {\rm M}_\odot$. If the unshocked ejecta grains are larger than $0.1 \, {\rm μm}$, the dust masses are higher, the destruction efficiencies are lower, and the final yield may exceed $0.5 \, {\rm M}_\odot$. As Cas A has a dense circumstellar environment and thus a much stronger reverse shock than is typical, the average dust destruction efficiency across all CCSNe is likely to be lower, and the average dust yield higher. This supports a mostly-stellar origin for the cosmic dust budget.
Survival or Destruction: Effects of Spheroidal Satellite Collisions on Bars in Milky Way-Like Galaxies
School of Astronomy and Space Science, Nanjing University（南京大学天文与空间科学学院）；Key Laboratory of Modern Astronomy and Astrophysics (Nanjing University), Ministry of Education（教育部现代天文与天体物理重点实验室（南京大学））；Institute of Science and Technology for Deep Space Exploration, Suzhou Campus, Nanjing University（南京大学苏州校区深空探测科学与技术研究院）；Lund Observatory, Division of Astrophysics, Department of Physics, Lund University（隆德大学物理系天体物理学部隆德天文台）；Departamento de Física de la Tierra y Astrofísica, Fac. de C.C. Físicas, Universidad Complutense de Madrid（马德里康普顿斯大学物理学院地球与天体物理学系）
P.N. Lebedev Physical Institute of the Russian Academy of Sciences（俄罗斯科学院列别杰夫物理研究所）；M.V. Lomonosov Moscow State University, Faculty of Space Research（莫斯科国立大学空间研究系）
