Supernovae as sources ofinterstellar dust
Takaya Nozawa(IPMU, University of Tokyo, Kashiwa, Japan)
Collaborators:
T. Kozasa (Hokkaido Univ.), N. Tominaga (Konan Univ.)
K. Maeda, M. Tanaka, K. Nomoto (IPMU, Univ. of Tokyo)
H. Umeda, I. Sakon (University of Tokyo)

2011/11/29

Outline
1. Introduction
2. Formation and evolution of dust in Population III
Type II-P and pair-instability SNe

3. Formation and destruction of dust in Type IIb SNewith application to Cassiopeia A SNR
4. Missing-dust problem in core-collapse SNe
5. Formation of dust in the ejecta of Type Ia SNe
6. Summary

1. Introduction

1-1. Discovery of massive dust at z > 5・ The submm observations have confirmed the presenceof dust in excess of 108 Msun in 30% of z > 5 quasars
SDSS J1148+5251 at z=6.4－ age : 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

stellaremission

dustemission** Herschel (3.5m) **・ PACS :70, 100, 160 μm
・ SPIRE
250, 350, 500 μm

Leipski+’10, A&A, 518, L34

1-2. What are dust sources in high-z quasar?
・ Supernovae (Type II SNe)

➔ ~0.1 Msun per SN is sufficient(Morgan & Edmunds’03; Maiolino+’06; Li+’08)➔ > 1 Msun per SN (Dwek+’07)
・ AGB stars + SNe(Valiante+’09; Gall+’11; Dwek & Cherchneff’11)➔ 0.01-0.05 Msun per AGB (Zhukovska & Gail ’08)
➔ 0.01-1 Msun per SN・ Grain growth in dense clouds + AGB stars + SNe(Draine’09; Michalowski+’10; Pipino+’11; Mattsson’11)➔ τgrowth ~ 10^7 (Z / Zsun) yr・ Quasar outflows (Elvis+’02)

1-3. Extinction curves at high-z quasars
Maiolino+’04, Nature, 431, 533
SDSS J1048+4637 at z=6.2
Broad absorption line (BAL) quasars

different dust properties
from those at low redshift1-4. Extinction curves at 3.9 < z < 6.4
Gallerani+’10, A&A,523, 85

7 of 33 requires
substantial dust
extinction,
which deviatesfrom the SMC
GRB 050904 at z=6.3

additional evidence fordifferent dust properties
at high-z
Stratta+’07, ApJ, 661, L9

1-5. Summary of Introduction
・ There is clear evidence for huge amounts of dust
at z > 5, but the dust sources remain unexplained➔ SNe? AGB stars? grain growth in the dense clouds?
quasar outflow? any other sources?

・ Properties (composition & size) of dust at high z
are likely to be different from those at low z➔ high-z quasars and GRBs are good targets to probe
the extinction curves in their host galaxies

At z > 4, short-lived SNe II (M = 8-40 Msun) dominate
the dust production over AGB stars (M < 8 Msun) ??

2-1. Dust Formation in Pop III SNe
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’02)
・ 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’88)

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

2-1-2. 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

2-1-3. 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, Mdust / Mmetal = 0.2-0.3
PISNe ： Mdust =20-40 Msun, Mdust / Mmetal = 0.3-0.4

2-2. Dust destruction in supernova remnants
・ a part of dust grains formed in SNe are destroyed due
to sputtering in the hot gas swept up by the shocks(e.g., Bianchi & Schneider’07; Nozawa+’07, 10)➔ destruction efficiency of dust depends on the initialsize distribution

・ It is necessary to treat formation and destruction ofdust self-consistently
He coreFSRSCD

2-2-1. Initial condition for shock waves
・ Hydrodynamical model of SNe (Umeda & Nomoto’02)
・ SNe II : Mpr=13, 20, 25, 30 Msun (E51=1)
・ PISNe : Mpr=170 (E51=20), 200 Msun (E51=28)

・ The ambient medium (homogeneous)・ gas temperature : T = 104 K・ gas density : nH,0 = 0.1, 1, and 10 cm-3

・ Dust Model・ initial size distribution and spatial distribution of dust➔ results of dust formation calculations
・ treating as a test particle
The calculation is performed from 10 yr up to ~106 yr

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. Dust mass and size ejected from SN II-P
PISNe
SNe II-P

total dust mass surviving thedestruction in Type II-P SNRs;
0.07-0.8 Msun (nH,0 = 0.1-1 cm-3)

size distribution of dust after
RS destruction is domimatedby large grains (> 0.01 μm)

Nozawa+’07, ApJ, 666, 955
at time of dust formation

after destruction of dust
by reverse shock2-3. Flattened extinction curves at high-z
Hirashita, TN, et al. 2008, MNRAS, 384, 1725

Dust extinction curves in the early
universe are expected to be flat

Gallerani+’10, A&A, 523, 85

Some studies have suggested thatthe extinction curve before thedestruction is more appropriate inhigh-z and star-forming galaxies(Kawara+2011, Shimizu+2011, Jang+2011)
Li+’08, ApJ, 678, 1136

2-4. Effect of dust on star formation history
efficient formation of H2 molecules on the surface(e.g., Cozaux & Spaans’04)➔ promoting formation of stars (Hirashita & Ferrara’02)
SN dust w/o RS destruction

SN dust with RS destruction

Yamasawa, …, TN, et al. 2011, ApJ, 735, 44Larger size of dust suppresses the formation rate of H2
and thus does not activate star formation significantly

3. Formation and evolution of dustin SNe IIb: Application to Cas A

3-1. Dust formation in Type IIb SN○ SN IIb model (SN1993J-like model)－ Meje = 2.94 Msun
MZAMS = 18 Msun
MH-env = 0.08 Msun
－ E51 = 1.0－ M(56Ni) = 0.07 Msun

3-2. Dependence of dust radii on SN type
SN IIbSN II-P

0.01 μm

SN Ib (SN 2006jc)－ condensation
timedust(Nozawaet al.of2008)
300-700 d after explosion－ total mass of dust formed
・ 0.167 Msun in SN IIb
・ 0.1-1 Msun in SN II-P
Nozawa+’10, ApJ, 713, 356－ 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
homogeneous CSM (ρ = const)

stellar-wind CSM (ρ ∝ r-2)
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 reverse shock at dust-forming region
Nozawa+’10, ApJ, 713, 356

3-4. IR emission from dust in Cas A SNRAKARI corrected 90 μm image

・ 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
Nozawa+’10, ApJ, 713, 356

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)

4-1. Missing-dust problem in CCSNe
Matsuura,
Tanaka,...,TN,TN,etetal.al.2011,2011,submitted
Sciencecool dust in SN1987A
theorycold dust ??

young SNRs

Herschel detects cool (20K) dustof 0.4-0.7 Msun toward SN 1987A!
young SNe

There is a big difference in the mass of dust between
observational estimates and theoretical predictions!!

4-2. Resolving cold dust in SN87A with ALMA
ALMA Cycle 0 Proposal‘Detecting cool dust in SN1987A’（PI：Nozawa）

Band 7 (850 μm)

Band 9 (450 μm)

0.1 Msun of silicate ➔ 5σ detection

This proposal is ranked in thehighest priority to be observed !

4. Formation of dust in SNe Ia

4-1. Dust formation in Type Ia SNe○ Type Ia SN modelW7 model (C-deflagration) (Nomoto+’84; Thielemann+’86)－ Meje = 1.38 Msun

－ E51 = 1.3－ M(56Ni) = 0.6 Msun

0.1 Msun of C and O
remains unburnedin the outermost layer
with MC/MO ~ 14-2. Dust formation and evolution in SNe Ia
average radius

Nozawa+2011, ApJ, 736, 45

dust 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

4-3. Optical depths by newly formed dust
V band (0.55 μm) opacity at 300 days for γ = 1
MC= 0.006 Msun
Msilicate = 0.030 Msun
MFeS = 0.018 Msun
MSi= 0.063 Msun

τC= 22τsilicate = 0.01
τFeS = 14
τSi= 78

Mtotalτtotal

= 0.116 Msun

= 114

V band (0.55 μm) opacity at 300 days for γ = 0.1
Mtotal~ 3x10-4 Msun

τtotal=1

Formation of dust grains (C, Si, and Fe) should be
suppressed to be consistent with the observations

4-4. Carbon dust and outermost layer of SNe Ia
・ There has been no evidence for dust formation in SNe Ia➔ Formation of massive carbon dust does not matchthe observationsObservational data : SN 2005df at
day 200 and 400 (Gerardy+’07)－ massive unburned carbon(~0.05 Msun) in deflagration➔ change of compositionof WD by He-shell flash➔ burning of carbon by adelayed detonation

observationally estimatedcarbon mass in SNe Ia :Mc < 0.01 Msun
Nozawa+2011, ApJ, 736, 45(Marion+’06; Tanaka+’08)

4-5. Dust formation in super-Chandra SNe?
－ super-Chandra SNe :M(56Ni) ~ 1.0 Msun

SN 2009dc, Tarbenberger+’10

detection of CII line
➔ presence of massive
unburned carbon

enhanced fading at ~200 day➔ formation of carbon dust?

5. Summary of this talk・ Type II SNe with massive H envelopes－ radius of dust formed : aave > 0.01 μm➔ H-retaining SNe may be important sources of dust,
supplying 0.1-1.0 Msun of dust to the ISM
・ Type IIb/Ib/Ia SNe without massive H envelopes－ grain radius formed : aave < 0.01 μm➔ dust is almost completely destroyed in the SNRs
➔ H-stripped SNe are not likely to be sources of dust
＊ Our model treating dust formation and evolution self-consistently
can reproduce the IR emission from Cas A SNR

・ Mass of dust in young SNRs are dominated by cool dust
－ FIR and submm observations of SNRs are essential➔ Herschel detected massive cool dust in SN 1987A

5-1. Implication on evolution history of dust
〇 metal-poor (high-z or starbust) galaxies
・ massive stars (SNe) are likely to be dominant・ mass loss of massive stars would be less efficient➔ Type II-P SNe might be major sources of dust
necessary for serving the seeds for grain growth in the ISM－ dust mass per SN II-P after the RS destruction
Mdust = 0.1-0.8 Msun for nH,0 = 0.1-1 cm-3
－ average radius of dust is quite large (> 0.01 μm)
・ grain growth in the ISM makes grain size larger➔ dust extinction curve in the early universe might begray (wavelength-independent) if SNe II-P (and graingrowth) are main sources of dust at high redshift5-2. Implication on evolution history of dust
〇 metal-rich (low-z or Milky Way) galaxies
・ low-mass stars are dominant・ mass loss of massive stars would be more efficient➔ SNe (IIb, Ib/c, Ia) might be minor sources of dust

－ dust is almost completely destroyed in the SNRs
since size of newly formed dust is small (< 0.01 μm)
Dust size distribution at t=5 Myr (nH=1 /cc)

・ How are small dust grains produced?

－ size of dust from AGB stars is unknown
relatively large (0.01-0.1 μm)?? (Yasuda & Kozasa 2011)－ shattering due to grain-grain collisions
Hirashita, TN, +’10, MNRAS, 404, 1437