Dust Formation in Various
Types of Supernovae
Takaya Nozawa(IPMU, University of Tokyo)
Collaborators;
T. Kozasa (Hokkaido Univ.)
K. Nomoto (IPMU)
K. Maeda (IPMU)
H. Umeda (Univ. of Tokyo)
N. Tominaga (Konan Univ./IPMU)
M. Tanaka (IPMU)
T. Suzuki (Univ. of Tokyo)
M. Limongi (INAF/IPMU)

H. Hirashita (ASIAA)
I. Sakon (Univ. of Tokyo)
T. Onaka (Univ. of Tokyo)
T. T. Takechi (Nagoya Univ.)
T. T. Ishi (Kyoto Univ.)
A. Habe (Hokkaido Univ.)
E. Dwek (NASA)
O. Krause (MPIA)

1-1. Introduction
SNe are important sources of interstellar dust?
－ Theoretical studies : 0.1-1 Msun in Type II-P SNe(Todini & Ferrara 2001; Nozawa et al. 2003)➔ 0.1-1 Msun of dust per SN is required to form toexplain a large content of dust at high-z galaxies(Morgan & Edmunds 2003; Dwek et al. 2007)－ Observations of dust-forming SNe : < 10-2 Msun(e.g., Meikle et al. 2007, Kotak et al. 2009)sophisticate radiation transfer model taking accountof dust distribution in the ejecta to estimate dust mass
(Sugarmann et al. 2006; Ercolano et al. 2007)

how dust formation process depends on SN type?

1-2. Classification of supernovae
Heger et al. (2003)

At high (solar) metallicity
・ Type II-P SNe:MZAMS=8-25 Msun?
massive H envelpe
・ Type IIb SNe:significant mass loss
MZAMS = 25-35 Msun?
little mass loss
very thin H-envelope
・ Type Ib/Ic SNe :MZAMS > 35 Msun?
no H / He envelope
At low metallicity (Z < 10-4 Zsun)
・ Type II-P SNe:・ Type Ia SNe :MZAMS=8-40 Msun
thermonuclear explosion
・ pair-instability SNe:of C+O white dwarfs
MZAMS=140-260 Msun
Mpre-explosion ~ 1.4 Msun

2-1. Dust formation in primordial SNe(Nozawa et al. 2003, ApJ, 598, 785)・ nucleation and grain growth theory (Kozasa & Hasegawa 1988)

・ no mixing of elements within the He-core
・ complete formation of CO and SiO, sticking probability=1〇 Population III SNe model (Umeda & Nomoto 2002)
・ SNe II-P ： MZAMS = 13, 20, 25, 30 Msun (E51=1)
・ PISNe ： MZAMS = 170 Msun (E51=20), 200 Msun (E51=28)

Menv ~ 12 Msun

Menv ~ 90 Msun

2-2. Dust formed in primordial SNe・ Various dust species (C, MgSiO3, Mg2SiO4, SiO2, Al2O3,MgO, Si, FeS, Fe) form in the unmixed ejecta, according
to the elemental composition of gas in each layer
・ The condensation time: 300-600 days for SNe II-P
400-800 days for PISNe2-3. Size distribution spectrum of dust

・ grain radii range from a few A up to 1 μm

・ average dust radius is smaller for PISNe than SNe II-P
amount of newly formed dust grains
SNe II-P： Mdust = 0.1-1 Msun, fdep = Mdust / Mmetal = 0.2-0.3
PISNe ： Mdust =20-40 Msun, fdep = Mdust / Mmetal = 0.3-0.4

2-4. Total mass and size of surviving dust
(Nozawa et al. 2007, ApJ, 666, 955)

Total dust mass surviving thedestruction in Type II-P SNRs;
0.08-0.8 Msun (nH,0 = 0.1-1 cm-3)

Size distribution of surviving
dust is domimated by large
grains (> 0.01 μm)

2-5. Flattened extinction curves(Hirashita, T. N., et al. 2008, MNRAS, 384, 1725)
20 Msunflat extinction curve at high-z !
z=0.69z=4z=0.54
z=1.16170 MsunLi et al. (2008)

3-1. Dust formation in Type IIb SN(Nozawa et al. 2010, ApJ, 713, 356)
○ SN IIb model (SN1993J-like model)－ MH-env = 0.08 Msun
MZAMS = 18 Msun
Meje = 2.94 Msun
－ E51 = 1－ M(56Ni) = 0.07 Msun

3-2. Dust formed in Type IIb SN
condensation time

average radius
0.01 μm－ condensation time of dust
300-700 d after explosion－ total mass of dust formed
・ 0.167 Msun in SN IIb
・ 0.1-1 Msun in SN II-P

－ the radius of dust formedin H-stripped SNe is small
・ SN IIb without massive
H-env ➔ adust < 0.01 μm

・ SN II-P with massive
H-env ➔ adust > 0.01 μm

3-3. Destruction of dust in Type IIb SNR
constant-density CSM

stellar-wind CSM
330 yrnH,1 = 30, 120, 200 /cc➔ dM/dt = 2.0, 8.0, 13x10-5 Msun/yr for vw=10 km/s

Almost all newly formed grains are destroyed in shockedgas within the SNR for CSM gas density of nH > 0.1 /cc➔ small radius of newly formed dust
➔ early arrival of the reverse shock at the He core

3-4. Comparison with observations of Cas A

Sibthorpe et al. 2009

observed IR SED canbe well reproduced！
↑・ Md,warm ~ 0.008 Msun
・ Md,cool ~ 0.07 Msun
with Tdust ~ 40 K

AKARI reduced 90μm image➔ centrally peaked cool
dust component↓
Md,cool = 0.03-0.06 Msun
with Tdust = 33-41 K

4-1. Peculiar dust-forming SN : SN 2006jc
Di Calro et al. (2008)
Tominaga et al. (2008)

800K aC
Sakon et al. (2008)

・ re-brightning of NIR
・ at 75-102 days
・ rapid decline of optical light➔ C grains of ~1600 K
・ blueshift of He I narrow lines
・ at 220 days
➔ C grains of 800 K

ongoing formation of dust
from ~50 days in SN2006jc

4-2. Dust formation in Type Ib SN : SN 2006jc(Nozawa et al. 2008, ApJ, 684, 1343)○ SN 2006jc model (Tominaga et al. 2008)－ Meje = 4.9 Msun (MZAMS = 40 Msun)－ E51 = 10 (hypernova-like)－ M(56Ni) = 0.22 Msun

The quick decrease of gas
temperature➔ C grains can form at 40-60
days in outermost ejecta

4-3. Average radius and temperature of dust
average radius

dust temperature

0.01 μm－ Average radius of dustis smaller than 0.01 μm
because of the low gas
density at dust formation－ Temperature of C grains
・ at 60 days
➔ 1200-1700 K
・ at 200 days
➔ 500-600 K

4-4. IR spectral energy distribution
best fitted result

・ fitting of IR SED
C grains ➔ 5.6 x 10-4 Msun FeS grains ➔ 2 x 10-3 Msun・ mass of cold silicates and oxides cannot be constrained
optical thin case can underestimate dust mass

5-1. Dust formation in Type Ia SN : W7 model○ Type Ia SN model(Nozawa et al. in preparation)

W7 model (C-deflagration) (Nomoto et al. 1984)－ Meje = 1.38 Msun

－ E51 = 1.3－ M(56Ni) = 0.56 Msun

5-2. Dust formation in Type Ia SN
condensation time

average radius
0.01 μm

・ condensation time: 100-300 days

・ average radius of other dust species : < 0.01 μm
because of low density of gas in the expanding ejecta
・ Fe grains cannot condense significantly < 10-4 Msun

5-3. Mass of dust formed in Type Ia SN
Mass of major dust

・ early formation of dustat 100-300 days

C: 0.03 Msun
Silicate : 0.03 Msun
FeS: 0.02 Msun
Si: 0.06 Msun
Total・ high M(56Ni) of ~0.6 Msun
➔ dust formation can beaffected by strong radiation
field in the ejecta: 0.14 Msun
➔ Si and FeS are inhibited

There is no evidence that C are detected in SN Ia

If we ignore C grains in SN Ia
Mdust ~ 0.03 Msun, consisting of silicate in Type Ia

Summary of this talk・Type II SNe and PISNe
Average grain radii are larger than 0.01 μm➔ primordial SNe may be important sources of dust・Type IIb, Type Ib/Ic, and Type Ia SNe
Average grain radii are smaller than 0.01 μm➔ envelope-stripped SNe may not be major sourcesof dustin future work
mixing of elements, formation of molecules such as CO and SiO,
sticking probability of atom, effects of radiation field in the ejcta,
non-spherical and/or clumpy structure …