Dust survival rates in clumps passing through the Cas A reverse shock – I. Results for a range of clump densities

ABSTRACT The reverse shock in the ejecta of core-collapse supernovae is potentially able to destroy newly formed dust material. In order to determine dust survival rates, we have performed a set of hydrodynamic simulations using the grid-based code astrobear in order to model a shock wave interactin...

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Bibliographic Details
Published in:Monthly notices of the Royal Astronomical Society Vol. 489; no. 4; pp. 4465 - 4496
Main Authors: Kirchschlager, Florian, Schmidt, Franziska D, Barlow, M J, Fogerty, Erica L, Bevan, Antonia, Priestley, Felix D
Format: Journal Article
Language:English
Published: United Kingdom Oxford University Press 11.11.2019
Royal Astronomical Society
Subjects:
ASTRONOMY AND ASTROPHYSICS
dust, extinction
hydrodynamics
ISM: supernova remnants
methods: numerical
shock waves
supernovae: general
supernovae: individual: Cassiopeia A
ISM: supernova remnants
dust, extinction
supernovae: individual: Cassiopeia A
hydrodynamics
methods: numerical
supernovae: general
shock waves
ISSN:0035-8711, 1365-2966
Online Access:Get full text
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Summary:ABSTRACT The reverse shock in the ejecta of core-collapse supernovae is potentially able to destroy newly formed dust material. In order to determine dust survival rates, we have performed a set of hydrodynamic simulations using the grid-based code astrobear in order to model a shock wave interacting with clumpy supernova ejecta. Dust motions and destruction rates were computed using our newly developed external, post-processing code paperboats, which includes gas drag, grain charging, sputtering, and grain–grain collisions. We have determined dust destruction rates for the oxygen-rich supernova remnant Cassiopeia A as a function of initial grain sizes and clump gas density. We found that up to $30\,\mathrm{{{\ \rm per\ cent}}}$ of the carbon dust mass is able to survive the passage of the reverse shock if the initial grain size distribution is narrow with radii around ∼10–50 nm for high gas densities, or with radii around $\sim 0.5\!-\!1.5\,\mathrm{\mu m}$ for low and medium gas densities. Silicate grains with initial radii around 10–30 nm show survival rates of up to $40\,\mathrm{{{\ \rm per\ cent}}}$ for medium- and high-density contrasts, while silicate material with micron-sized distributions is mostly destroyed. For both materials, the surviving dust mass is rearranged into a new size distribution that can be approximated by two components: a power-law distribution of small grains and a lognormal distribution of grains having the same size range as the initial distribution. Our results show that grain–grain collisions and sputtering are synergistic and that grain–grain collisions can play a crucial role in determining the surviving dust budget in supernova remnants.
Bibliography:European Research Council (ERC)
USDOE National Nuclear Security Administration (NNSA)
Science and Technology Facilities Council (STFC) (United Kingdom)
LA-UR-19-27511
89233218CNA000001; ERC-2015-AdG-694520; ST/P002307/1; ST/R002452/1; ST/R00689X/1
ISSN:0035-8711
1365-2966
DOI:10.1093/mnras/stz2399