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Collaborators: Jen Andrews (UMass) Joe Gallagher ( UCinn ) Mike Barlow (UCL) Roger Wesson (ESO)

Dust Formation in Core-Collapse Supernovae Geoffrey C. Clayton Louisiana State University. Collaborators: Jen Andrews (UMass)

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Collaborators: Jen Andrews (UMass) Joe Gallagher ( UCinn ) Mike Barlow (UCL) Roger Wesson (ESO)

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  1. Dust Formation in Core-Collapse Supernovae Geoffrey C. Clayton Louisiana State University

  2. Collaborators: • Jen Andrews (UMass) • Joe Gallagher (UCinn) • Mike Barlow (UCL) • Roger Wesson (ESO) • Jo Fabbri (UCL) • Mikako Matsuura (UCL) • Margaret Meixner (STScI) • Nino Panagia (STScI) • MassakiOtsuka(IAA) • Barbara Ercolano(USM) • Ben Sugerman (Goucher) • Doug Welch (McMaster)

  3. NGC 6946

  4. QSO at z = 6.4 (Bertoldi et al. 2003).

  5. Dwek 1998

  6. Dust Production SNe II (solid), Low mass stars (dotted), SNe Ia (dashed), destruction rate by astration (thick solid) (Dwek 1998)

  7. Dwek 1998

  8. NGC 2397

  9. SN 2003gd Mdust = 0.02 Mo

  10. SN 2007od SN 2007it

  11. SN 2007od SN 2007it

  12. 2007od

  13. SN 2007it

  14. SN 2007od

  15. Dust Formation inCCSNe

  16. SN 1987A 0.4 – 0.7 M☉ Matsuura et al. 2011

  17. <-- M = 8 - 40 M☉ M = 1.4 - 25 M☉-->

  18. Mass loss = 10 M☉ Mgas/Mdust=200 Mgas = 9.95 M☉ Mdust = 0.05 M☉ So, Mdust = 0.4 – 0.7 M☉ Mgas = 80 to 140 M☉

  19. Things to think about • Is there accretion of dust in the ISM? • When do AGB stars become important dust makers? • Why does SN 1987A always have to be different? • Do SNe with significant CSM make more dust? • Do SNe destroy more dust than they make?

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