Formation of Dust Grains bySupernova Explosion
Takaya Nozawa(IPMU, University of Tokyo)
Collaborators:
T. Kozasa, A. Habe (Hokkaido Univ.),
K. Maeda, K. Nomoto, M. Tanaka (IPMU),
N. Tominaga (Konan Univ.), H. Umeda, I. Sakon (U.T.)
2011/2/25

Outline
1. Introduction
2. Formation and evolution of dust grains in
Type II-P and pair-instability SNe
3. Formation and evolution of dust grains invarious types of SNe
4. Missing-dust problem in SNe
5. Conclusion remarks

1. Introduction

1-1. Interstellar dust in our Galaxy
・ Dust in our Galaxy ➔ when and where is dust formed?
composition : graphite (carbonaceous)silicate (SiO2, Mg2SiO4, MgFeSiO4…)
size :

n(a) = f(a)da = a-3.5 da (0.005~0.25 μm)

amount :Mdust / Mgas ~ 1 / 140 (~109 Msun)(e.g., Mathis+77; Draine & Lee 84)

extinction curve

IR spectral featuredepletion of elements

1-2. Discovery of large amounts of dust at z > 5・ The submm observations have confirmed the presenceof dust in excess of 108 Msun in 30% of z > 5 quasars➔ We see warm dust grains heated by absorbing
stellar lights in the host galaxies of the quasars
SDSS J1148+5251 at z=6.4

Leipski+10, A&A, 518, L34－ age : 840-890 Myr－ IR luminosity : ~(1-3)x1013 Lsun
－ dust mass : (2-7)x108 Msun
－ SFR : ~3000 Msun/yr (Salpeter IMF)
－ gas mass : ~3x1010 Msun (Walter+04)－ metallicity : ~solar

1-3. What are sources of dust in high-z quasar?
・ Supernovae (Type II SNe)

➔ ~0.1 Msun per SN is sufficient(Morgan & Edmunds 2003; Maiolino+06; Li+08)➔ > 1 Msun per SN (Dwek+07)
・ AGB stars + SNe(Valiante+09; Gall+10; Dwek & Cherchneff 2011)➔ 0.01-0.05 Msun per AGB (Zhukovska & Gail 2008)➔ 0.01-1 Msun per SN・ Grain growth in the ISM + AGB stars + SNe(Draine 2009; Michalowski+10; Pipino+11)➔ τgrowth ~ 10^7 (Z / Zsun) yr
・ Quasar outflow (Elvis+02)

1-4. Extinction curves at high-z quasars
SDSS J1048+4637 at z=6.2

GRB 050904 at z=6.3

different dust properties at
high-z indicate SN-dust origin?

Maiolino+04, Nature, 431, 533Gallerani+10, A&A, 523, 85

Stratta+07, ApJ, 661, L9

7 among 33 quasars at
3.9 < z < 6.4 requires
significant dust extinction, which deviatesfrom those in the SMC

1-5. Death of single massive stars
Heger+03, ApJ, 591, 288

At high metallicity
・ Type II-P SNe:MZAMS=8-25 Msun?
massive H envelope
significant mass loss
little mass loss

・ Type IIb SNe:MZAMS = 25-35 Msun?
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:MZAMS=8-40 Msun

・ pair-instability SNe:MZAMS=140-260 Msun

・ Type Ia SNe :thermonuclear explosionof C+O white dwarfs
Mpre-explosion ~ 1.4 Msun

2. Formation and evolution ofdust in Population III SNe

2-1. Dust Formation in Supernovae
at ~1 days
He-coreH-envelope

NS or BH
He–layer (C>O)
O–Ne-Mg layer
Dust formation
Si–Satlayer~1-3 years
afterlayer
explosion
Fe–Ni2-1-1. Dust formation in primordial SNe
Nozawa+03, ApJ, 598, 785〇 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

・ nucleation and grain growth theory (Kozasa & Hasegawa 1988)

・ no mixing of elements within the He-core
・ complete formation of CO and SiO

2-1-2. Nucleation rate of dust
Steady-state classical homogeneous nucleation rate

Supersaturation ratio

2-1-3. Basic equations of dust formation
Equation of conservation for key species

Equation of grain growth2-1-4. Dust formed in primordial SNe
Nozawa+03, ApJ, 598, 785

・ 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

2-1-5. Size distribution of newly formed dust
Nozawa+03, ApJ, 598, 785

・ 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

2-2. Dust Evolution in SNRs
T = (1-2)x104 K
nH,0 = 0.1-1 cm-3

He coreFSRSCD

2-2-1. Temperature and density of gas in SNRs
Nozawa+07, ApJ, 666, 955
Model : M pr= 20 Msun (E51=1)
nH,0 = 1 cm-3

Downward-pointing arrows:
forward shock in upper panel
reverse shock in lower panel
The temperature of the gas
swept up by the shocks➔ 106-108 K↓
Dust grains residing in theshocked hot gas are erodedby sputtering2-2-2. Evolution of dust in SNRs
Nozawa+07, ApJ, 666, 955
Model : M pr= 20 Msun (E51=1)
nH,0 = 1 cm-3

Dust grains in the He core collidewith reverse shock at (3-13)x103 yr

The evolution of dust heavily
depends on the initial radiusand compositionaini = 0.01 μm (dotted lines)➔ completely destroyedaini = 0.1 μm (solid lines)➔ trapped in the shellaini = 1 μm (dashed lines)➔ injected into the ISM

2-2-3. Total mass and size of surviving dust
Nozawa+07, 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)

3. Formation and evolution ofdust in various types of SNe

3-1-1. Dust formation in Type IIb SN
Nozawa+10, 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

3-1-2. Dependence of dust radii on SN type
Nozawa+10, ApJ, 713, 356

SN IIbSN II-P

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

3-1-3. Destruction of dust in Type IIb SNR
constant-density CSM

stellar-wind CSM
330 yrNozawa+10, ApJ, nH,1 = 30, 120, 200 /cc➔ dM/dt = 2.0, 8.0, 13x10-5 Msun/yr for vw=10 km/s
713, 356
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

3-1-4. Dust in Cassiopeia A
Nozawa+10, ApJ, 713, 356

・ total mass of dust formed
Mdust = 0.167 Msun・ shocked dust : 0.095 Msun
Md,warm ~ 0.008 Msun
・ unshocked dust :Md,cool ~ 0.072 Msun
with Tdust ~ 40 K

AKARI corrected 90 μm image

AKARI observation
Md,cool = 0.03-0.06 Msun
Tdust = 33-41 K(Sibthorpe+10)

Herschel observation
Md,cool = 0.075 Msun
Tdust ~ 35 K (Barlow+10)

3-2-1. Dust formation in Type Ia SN○ Type Ia SN modelW7 model (C-deflagration) (Nomoto+84; Thielemann+86)－ Meje = 1.38 Msun

－ E51 = 1.3－ M(56Ni) = 0.6 Msun

3-2-2. Dust formation and evolution in SNe Ia
average radius

Nozawa+11, submitteddust destruction in SNRs

0.01 μm

・ condensation time :100-300 days
・ average radius of dust :aave <~ 0.01 μm
・ total dust mass :Mdust = 0.1-0.2 Msun

newly formed grains arecompletely destroyed for
ISM density of nH > 0.1 cm-3
➔ SNe Ia are unlikely to be
major sources of dust

4. Missing-dust problem in SNe4-1. SNe are important sources of dust?
・ Theoretical studies－ at dust formation : ~0.1-1 Msun in CCSNe (SNe II-P)(Nozawa+03; Todini & Ferrara 2001; Cherchneff & Dwek 2010)－ after destruction of dust by reverse shock :~0.01-0.5 Msun (Nozawa+07; Bianchi & Schneider 2007)

dust amount needed to explain massive dust at high-z!
・ Observational works－ MIR observations of dust-forming SNe : < 10-3 Msun(e.g., Ercolano+07; Sakon+09; Kotak+09)－ submm observations of SNRs : >1 Msun
(Dunne+03; Morgan+03; Dunne+09; Krause+05)－ MIR-FIR observation of Cas A SNR : 0.02-0.075 Msun
(Rho+08; Sibthorpe+09; Barlow+10)

4-2. Missing-dust problem in CCSNeTanaka, TN, +11, submitted
theory4-3. Detectability of dust with SPICA
Tanaka, TN, +11, submitted

extragalactic

Massive dust can behidden if Tdust < 100 K

4-4. Detectability of cold dust with ALMA
Md,warm = 0.008 Msun
Md,cool = 0.072 Msun
with Tdust = 43 K

－ SN 1987A in LMC
diameter : 2”, most feasible(Bouchet+04)－ 1E0102.2-7219 in SMC
diameter : 40”
too extended to be detected5. Conclusion remarks

5-1. Implication on evolution history of dust (1)〇 metal-poor (high-z or starbust) galaxies
・ massive stars (SNe) are dominate
・ mass loss of massive stars would be less efficient➔ Type II-P SNe might be major sources of dust
・ aave is relatively large (> 0.01 μm)
・ grain growth makes grain size larger➔ dust extinction curve might be grayz=0.69z=4
z=0.54z=1.16

Hirashita, TN,+08, MNRAS, 384, 1725

Li+08, ApJ, 678, 1136

5-2. Implication on evolution history of dust (2)〇 metal-rich (low-z or Milky Way) galaxies
・ low-mass stars are dominate
・ mass loss of massive stars would be more efficient➔ SNe (IIb, Ib/c, Ia) might be minor sources of dust
・ dust from AGB stars may also be large (0.01-0.1 μm)➔ How are small dust grains produced?
shattering process?
Dust size distribution at t=5 Myr (nH=1 /cc)

Hirashita, TN, +10, MNRAS, 404, 1437

5-3. Future prospects➔ SNe are important sources of dust?
・ maybe, Yes in the early universe・ at least, to serve the seeds for grain growth in the ISM➔ composition, size, and mass of dust?
・ SPICA will make great advances on this issue➔ theoretical and experimental approach is essential!
・ nucleation process, crystalization
・ dust temperature, optical properties➔ application to other dust formation site
・ novae, mass-loss wind of AGB and massive stars
・ grain growth and processing in the molecular clouds
evolution history of dust throughout the cosmic age!