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

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Presentation on theme: "Dust Formation in Core-Collapse Supernovae Geoffrey C. Clayton Louisiana State University."— Presentation transcript:

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) Massaki Otsuka (IAA) Barbara Ercolano (USM) Ben Sugerman (Goucher) Doug Welch (McMaster)

3 3 NGC 6946

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

5 Dwek 1998

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

7 Dwek 1998

8 8 NGC 2397

9 9 SN 2003gd M dust = 0.02 M o

10 10 SN 2007od SN 2007it

11 SN 2007od

12 2007od

13 SN 2007it

14 SN 2007od

15 SNWhen (d)Asymmetr y Vis. fadingIR BrighterM dust 1987A yes 7.5 x I~250yes...… 1998S yes...yes2 x em yesyes?...> gd yes 2 x et yes 1.5 x ip~730yes… … 2006jc~50yes… 3 x it Yes?yes < od yesyes?yes1.7 x Dust Formation in CCSNe

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

17 <-- M = M ☉ M = M ☉ -->

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

19 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? Things to think about


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