Dust Enrichment bySupernova Explosions
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 (Univ. of Tokyo)
2011/08/10

How does the cosmic dust evolve
throughout the cosmic age?
When and how did the universe
begin to be enriched with dust?

1-1. Discovery of huge amounts of dust at z > 5
There has been clear evidence for the presence of a large
amount of dust (>108 Msun) in quasars at z > 5 (t < 1.2 Gyr)SED of QSO at z=6.4

What is the origin of massive dust?
・ core-collapse SNe (Type II SNe)
➔ ~0.1-1 Msun per SN is needed(Maiolino+’06; Dwek+’07; Gall+’11)

・ AGB stars + SNe(Valiante+’09; Dwek & Cherchneff’11)➔ 0.01-0.05 Msun per AGB stars
LIR = 10^13 Lsun

Leipski+’10, A&A, 518, L34

・ Grain growth in ISM + AGB stars + SNe(Draine’09; Michalowski+’10; Pipino+’11;
Asano-san’ talk)1-2. Dust formation and destruction in SNe
Supernovae may be sources of the first dust・ 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)
its presence has not been proved observationally

He coreFSRS
CD・ a part of dust grains formed in SNeare destroyed due to sputtering in
the hot gas swept up by the shocks(Bianchi & Schneider’07; Nozawa+’07, ’10)

➔ the destruction efficiency of dust
depends on the size distribution1-3. Mass and size of dust ejected from SN II-P
Nozawa+2007, ApJ, 666, 955

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)

at time of dust formation

after destruction of dust
by reverse shock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-P

0.01 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
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!!

4-1. 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

4-2. 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 poor sourcesof interstellar 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