Are supernovae main sources ofinterstellar dust?
（超新星爆発は星間ダストの主要な供給源か？）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.)
2011/07/07

Outline
1. Introduction
2. Formation and evolution of dust in Type IIb SNewith application to Cassiopeia A SNR

3. Missing-dust problem in core-collapse SNe
4. Formation of dust in the ejecta of SNe Ia
5. Summary1. Introduction

1-1. Discovery of massive dust at z > 5 quasars
・ 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*Herschel・ PACS :70 μm
100 μm160 μm－ age : ~900 Myr (z=6.42)－ 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

・ SPIRE :250 μm350 μm500 μmLeipski+’10, A&A, 518, L34

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

➔ ~0.1 Msun per SN is sufficient (Maiolino+’06; Li+’08)➔ > 1.0 Msun per SN (Dwek+’07)
・ AGB stars + SNe(Valiante+’09; Dwek & Cherchneff’11)➔ 0.01-0.05 Msun per AGB (Zhukovska & Gail ’08)
➔ 0.01-1.0 Msun per SN・ Grain growth in dense clouds + AGB stars + SNe(Draine’09; Michalowski+’10; Pipino+’11; Mattsson’11,Gall+’10, ’11; Valiante+’11)

・ Quasar outflows (Elvis+’02)

1-3. Dust formation in primordial supernovae
Supernovae are important sources of dust?
・ Evolution of dust throughout the cosmic age－ A large amount of dust (> 108 Msun) in z > 5 quasars➔ 0.1-1.0 Msun of dust per SN must be ejected－ Inventory of interstellar dust in our Galaxy
・ Theoretical studies on dust formation in the SN ejecta(Todini & Ferrara’01; Nozawa+’03; Schneider+’04;
Bianchi & Schneider+’07; Cherchneff & Dwek’09, ’10)

－ Mdust=0.1-1 Msun in (primordial) Type II-P SNe (SNe II-P)－ Mdust=1.0-60 Msun in pair-instability SNe (PISNe)
its presence has not been proved observationally!!

1-4. 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

1-5. Mass and size of dust ejected from SN II-PPISNe
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+2007, ApJ, 666, 955
at time of dust formation

after destruction of dust
by reverse shock2. Formation and evolution of dustin SNe IIb: Application to Cas A2-1. 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

2-2. Dependence of dust radii on SN type
SN IIbSN II-P0.01 μm

SN Ib (SN 2006jc)－ condensation
time of dust(Nozawa+2008)
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 et al. 2010, 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

2-3. 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 et al. 2010, ApJ, 713, 356

2-4. 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 et al. 2010, 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)

3. Missing-dust problem in CCSNe

3-1. Difference in estimate of dust mass in SNe
・ Theoretical studies－ at time of dust formation : Mdust=0.1-1 Msun in CCSNe(Nozawa+’03; Todini & Ferrara’01; Cherchneff & Dwek’10)－ after destruction of dust by reverse shock (SNe II-P) :Msurv~0.01-0.8 Msun (Nozawa+’07; Bianchi & Schneider’07)

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

3-2. Missing-dust problem in CCSNe
Tanaka, TN, et al. 2011, submitted

theoryhigh optical depth
or cold dust ??

grain growth orformation in CDS??
confusion
with IS dust??

Middle-aged SNe with ages of 10-100 yrs are goodtargets to measure the mass of dust formed in SNe!!

3-3. Search for dust in middle-aged CCSNe－ silicate－ dust temperture ~ 230 K－ dust mass ~ 10-3 Msun

SN 1978K : Type IIn SNe
X-ray bright, massive CSM➔ the dust is likely to beof circumstellar origin

3-4. Estimate of dust mass in middle-aged SNe
Tanaka, TN, et al. 2011, submitted

What is temperature of newly formed but unshocked dust?

Massive dust can behidden if Tdust < 100 K

3-5. Temp. of cool dust and its detectability
Tanaka, TN, et al. 2011, submitted

0.1 Msunheating sources of dust
・ 44Ti ➔ ~1036 erg/s
・ X-ray emission➔ < ~1037 erg/s

LIR < Ltot < 1037 erg/s➔ Tdust < 45 K for 0.1 Msun
Tdust < 90 K for 10-3 Msun

・ Possible targets
SN 1978K, 93J, 04dj, 04et

3-6. Herschel detects massive dust in SN 1987A
Matsuura, ..., TN, et al. 2011 to be appeared in Science
cool dust in SN1987A
theoryhigh optical depth
or cold dust ??

grain growth orformation in CDS??
confusion
with IS dust??

Herschel detects cool (~20K) dust of 0.4-0.7 Msun toward
SN 1987A!

4. Formation of dust in SNe Ia

4-1. Introduction〇 Type Ia supernovae (SNe Ia)－ thermonuclear explosions of C+O white dwarfs withthe mass close to Chandrasekhar limit (~1.4 Msun)・ deflagration (Nomoto+76, 84)➔ subsonic wave, unburned C in the outer layer・ (delayed) detonation (Khokhlov91a, 91b)
➔ supersonic wave, burning almost all C－ synthesize a significant amount of Fe-peak andintermediate-mass elements such as Si, Mg, and Ca➔ play a critical role in the chemical evolution➔ possible sources of interstellar dust?

4-2. Type Ia SNe are sources of dust?
〇 Suggestions on dust formation in SNe Ia－ SNe Ia may be producers of Fe grains(Tielens98; Dwek98)－ the isotopic signature of presolar type X SiC grains
can be explained if produced in SNe Ia (Clayton+’97)〇 Observations of normal SNe Ia－ no increase of IR dust continuum (and no CO emission)－ no rapid decrease of the optical light curve－ no blueshift of atomic line emissions➔ these signatures have been reported for CCSNe－ no evidence for ejecta-dust in Tycho SNR (Douvion+’01)

4-3. 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

4-4. Dust formation and evolution in SNe Ia
average radius

Nozawa et al. 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 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

4-5. 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= 22
τsilicate = 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

4-6. Infrared thermal emission from dust
Observational data : SN 2005bf
at day 200 and 400 (Gerardy+’07)

black solid lines :SEDs including
emission from C grains➔ much higher than theobservational results

red solid lines :SEDs not including
emission from C grains➔ not contradict with theobservational results
0.03 Msun of silicate canbe allowed as dust mass

4-7. Carbon dust and outermost layer of SNe Ia〇 Formation of massive carbon dust
－ high sticking probability of α = 0.1-1➔ if α < ~0.01, any dust grain cannot condense－ dust formation around 100 days, M(56Ni) ~ 0.6 Msun
➔ dust formation can be destroyed by energetic
photons and electrons prevailing in the ejecta－ massive unburned carbon (~0.05 Msun) in deflagration➔ change of WD composition by the He-shell flash➔ burning of carbon by a delayed detonation wave

observationally estimated carbon mass in SNe Ia :Mc < 0.01 Msun (Marion+06; Tanaka+08)

4-8. Dust formation in super-Chandra SNe?
－ super-Chandra SNe :M(56Ni) ~ 1.0 Msun

SN 2009dc, Tarbenberger+’10detection of CII line
➔ presence of massive
unburned carbon

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

5. Summary of this talk・ Size of newly formed dust depends on types of SNe－ H-retaining SNe (Type II-P) : aave > 0.01 μm－ H-stripped SNe (Type IIb/Ib/Ic and Ia) : aave < 0.01 μm➔ dust is almost completely destroyed in the SNRs
➔ H-stripped SNe may be poor producers of dust
・ Our model treating dust formation and evolution self-consistently
can reproduce IR emission from Cas A・ Middle-aged SNe with the ages of 10-100 yr are good targets tomeasure the mass of dust formed in SNe－ We detect emission from SN 1978K, which is likely from shocked
circumstellar silicate dust with 1.3x10-3 Msun
－ The non-detection of the other 6 objects seems to be natural
because our present search is sensitive only to Ltot >1038 erg/s・ Mass of dust in young SNRs may be dominated by cool dust
➔ FIR and submm observations of SNRs are essential➔ Herschel detects massive cool dust toward SN 1987A