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)

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

NGC 6946

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

Dwek 1998

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

Dust Production

Dwek 1998

8

NGC 2397

9

SN 2003gd

Mdust = 0.02 Mo

10

SN 2007od

SN 2007it

SN 2007it

SN 2007od

2007od

SN 2007it

SN 2007od

SN When (d) Asymmetry

Vis. fading

IR Brighter

Mdust

1987A 526-589 yes yes yes 7.5 x 10-4

1990I ~250 yes yes ... …

1998S 249-474 yes ... yes 2 x 10-3

1999em 465-510 yes yes? ... > 10-4

2003gd 157-493 yes yes yes 2 x 10-2

2004et 277-313 yes yes yes 1.5 x 10-4

2005ip ~730 yes … yes …

2006jc ~50 yes … yes 3 x 10-4

2007it 350-500 Yes? yes yes < 10-3

2007od 130-232 yes yes? yes 1.7 x 10-4

Dust Formation in CCSNe

16

Matsuura et al. 2011

SN 1987A

0.4 – 0.7 M☉

<-- M = 8 - 40 M☉

M = 1.4 - 25 M ☉ -->

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☉

• 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