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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| Veröffentlicht in: | Monthly notices of the Royal Astronomical Society Jg. 489; H. 4; S. 4465 - 4496 |
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| Format: | Journal Article |
| Sprache: | Englisch |
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Oxford University Press
11.11.2019
Royal Astronomical Society |
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| Abstract | 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. |
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| AbstractList | 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. 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. |
| Author | Barlow, M J Fogerty, Erica L Schmidt, Franziska D Bevan, Antonia Priestley, Felix D Kirchschlager, Florian |
| Author_xml | – sequence: 1 givenname: Florian orcidid: 0000-0002-3036-0184 surname: Kirchschlager fullname: Kirchschlager, Florian email: f.kirchschlager@ucl.ac.uk organization: Department of Physics and Astronomy, University College London, Gower Street, London WC1E 6BT, UK – sequence: 2 givenname: Franziska D surname: Schmidt fullname: Schmidt, Franziska D organization: Department of Physics and Astronomy, University College London, Gower Street, London WC1E 6BT, UK – sequence: 3 givenname: M J orcidid: 0000-0002-3875-1171 surname: Barlow fullname: Barlow, M J organization: Department of Physics and Astronomy, University College London, Gower Street, London WC1E 6BT, UK – sequence: 4 givenname: Erica L orcidid: 0000-0003-1242-3898 surname: Fogerty fullname: Fogerty, Erica L organization: Center for Theoretical Astrophysics, Los Alamos National Lab, Los Alamos, NM 87545, USA – sequence: 5 givenname: Antonia orcidid: 0000-0001-7188-6142 surname: Bevan fullname: Bevan, Antonia organization: Department of Physics and Astronomy, University College London, Gower Street, London WC1E 6BT, UK – sequence: 6 givenname: Felix D surname: Priestley fullname: Priestley, Felix D organization: Department of Physics and Astronomy, University College London, Gower Street, London WC1E 6BT, UK |
| BackLink | https://www.osti.gov/biblio/1563015$$D View this record in Osti.gov |
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| ContentType | Journal Article |
| Copyright | 2019 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society 2019 |
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| Keywords | ISM: supernova remnants dust, extinction supernovae: individual: Cassiopeia A hydrodynamics methods: numerical supernovae: general shock waves |
| Language | English |
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| Notes | 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 |
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| Score | 2.6099718 |
| Snippet | 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... 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... |
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| SourceType | Open Access Repository Enrichment Source Index Database Publisher |
| StartPage | 4465 |
| SubjectTerms | ASTRONOMY AND ASTROPHYSICS dust, extinction hydrodynamics ISM: supernova remnants methods: numerical shock waves supernovae: general supernovae: individual: Cassiopeia A |
| Title | Dust survival rates in clumps passing through the Cas A reverse shock – I. Results for a range of clump densities |
| URI | https://www.osti.gov/biblio/1563015 |
| Volume | 489 |
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