2014/08/07

Dust production in a variety oftypes of supernovae
Takaya Nozawa(NAOJ, Division of theoretical astronomy)

Main collaborators:
Keiichi Maeda (Kyoto University)
Masaomi Tanaka (NAOJ)
Takashi Kozasa, Asao Habe (Hokkaido University)
Hideyuki Umeda (University of Tokyo)
Ken’ichi Nomoto (Kavli IPMU)

0-1. Introduction
Supernovae (SNe) are major sources of dust?
‐huge amounts of dust grains (>108 Msun) are detected in hostgalaxies of quasars at redshift z > 5 (the cosmic age < 1 Gyr)➔ core-collapse SNe (CCSNe) generating from short-lived
massive stars must predominantly supply dust to the ISM‐contribution of dust mass from AGB stars and CCSNe in the MWn(CCSNe) / n(AGB stars) ~ 0.05-0.1 (Salpeter IMF)
Mdust = 0.01-0.05 Msun per AGB star (Zhukovska & Gail 2008)
Mdust = 0.1-1.0 Msun per SN (e.g., Nozawa et al. 2003, 2007)➜ contribution of interstellar dust from CCSNe is comparablewith that from AGB stars
what composition, size, and mass of dust are ejected by CCSNe?

0-2. Classification of core-collapse SNe
SN IInSmith+11© Swinburne Univ. of Tech.

- Type II SNe (SNe II-P) ➜ massive hydrogen envelope- Type IIb/Ib SNe (SNe IIb/Ib) ➜ very little/no hydrogen envelope- Type Ic SNe (SNe Ic) ➜ no helium and hydrogen envelope- Type IIn SNe ➜ dense (massive) circumstellar medium

1. Observations of dust formationin SNe (and SNRs)

1-1. Summary of observed dust mass in CCSNe

missing cold dust?

young SNRs

Matsuura+2011

Type II-P SNeBalow+2010

Gomez+2012

swept-up IS dust?

Far-IR to sub-mm observations are essential for revealing
the mass of dust grains produced in the ejecta of SNe

1-1. Summary of observed dust mass in CCSNe

missing cold dust?

young SNRs

Type II-P SNe

swept-up IS dust?

Far-IR to sub-mm observations are essential for revealing
the mass of dust grains produced in the ejecta of SNe

1-2. Herschel detects cool dust in SN 1987A~180K~10-5 Msun
~20K~0.5 Msun
Matsuura+2011

on 4 Oct 2003
Gemini T-ReCS(λ = 10.36 μm)
2 pixels : 0.18”(Bouchet+04)

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

1-3. ALMA reveals dust formed in SN 1987A
ALMA, 1.4 mm

ALMA, 870 µm

ALMA, 450 µm

HST optical (HI)Chandra, X-ray

SED of 25-years old SN 1987A

Indebetouw+2014
blue: Hαgreen: 1.6 µm
red: CO(2-1)➜ >0.1 Msunof CO

ALMA spatially resolves cool(~20K) dust of ~0.5 Msun formedin the ejecta of SN 1987A➔ SNe could be production
factories of dust grains

1-4. Possible target: SNR 1E0102-72.3 in SMC
Are there any other candidates of SNe/SNRs in which
massive cool dust grains can be detected with ALMA?
➜ extragalactic SNe are too far (D > 1 Mpc) to detect the thermal
emission from cool dust in SNe even with ALMA
➜ young Galactic SNRs are too extended (θ > 1 arcmin) for thegood spatial resolution of ALMA (~0.1 arcsec)

young (compact) SNRs in LMC/SMC !!

・ SNR 1E0102-72.3

24 μm

X-ray, radio- O-rich (Type Ib?)
- age : ~1000 yr- Mwarm ~ 10-3 Msun
- Mcool ~ ???
Stanimirovic+05

Gaetz+00

1-5. SNR 1E0102-72.3 is too extended!

even the youngest SNR 1E0102-72.3 is too extended !!
40 times more extended➜ surface brightness is 1x103 times lower for the same massand temperature of dust

SN 1987A is the unique but the only target to detect
continuum emission from cool dust in SNe!!
SN 1987A

40 arcsec

1-6. Summary of observations of SN dust
‐ALMA confirmed the presence of a large amount of
newly formed dust in the ejecta of SN 1987A➜ heavy elements (Si, Mg, Fe, C) are locked up in dust grains➜ CCSNe are efficient production factories of interstellar dust

‐It seems too hard to detect thermal emission fromcool dust in any SNe/SNRs other than SN 1987A➜ even the youngest SNR in LMC/SMC are too extended‐A part of dust grains formed in the SN ejecta will be
destroyed by the reverse shocks
what fraction of dust grains can survive to be injected?
➜ destruction efficiency depends on dust composition and size
➜ infrared to submm observations have few information on thethe composition and size distribution of dust

2. Size and mass of dust ejectedby core-collapse SNe2-1. Dust mass and size ejected from SNe IINozawa+07, ApJ, 666, 955

SNe II

total mass of dust surviving thedestruction in Type II SNRs;
0.07-0.8 Msun (nH,0 = 0.1-1 cm-3)
size distribution of dust after theshock-destruction is domimatedby large grains (> 0.1 μm)

2-2. 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- M(56Ni) = 0.07 Msun

2-3. Dependence of grain radii on SN typeSN IIb

SN II-P

0.01 μm- condensation time of dust
300-700 days after explosion- the radius of dust formed in
H-stripped SNe is small- total mass of dust formed
・ 0.167 Msun in SN IIb
・ 0.1-1 Msun in SN II-P・ SN IIb without massive H-env➔ adust < 0.01 μm

Nozawa+10, ApJ, 713, 356

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

2-4. Destruction of dust in Type IIb SNR
homogeneous CSM (ρISM = const)

stellar-wind CSM (ρCSM ∝ 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 the hot gas
that was swept up by the reverse shocks➔ small radius of newly formed grains➔ early arrival of reverse shock at dust-forming region
Nozawa+10, ApJ, 713, 356

2-5. IR emission from dust in Cas A SNRAKARI 90 μm image (color)・ 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, 356AKARI 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)

2-6. Scaling relation of average grain radius
Nozawa & Kozasa (2013)

CMgSiO3

Λon > 30

Λon > 30

Λon = τsat/τcoll : ratio of supersaturation timescale to gas
collision timescale at the onset time (ton) of dust formation

Λon = τsat/τcoll ∝ τcool ngas
・ fcon,∞ and aave,∞ are uniquely determined by Λon・ steady-state nucleation rate is applicable for Λon > 30

2-7. Summary of dust formation in SNe II-P/IIb‐Size of newly formed dust depends on types of SNe

・ H-retaining SNe (Type II-P) : aave > 0.01 μm➜ a significant fraction of newly formed dust can survive➜ H-retaining SNe can be major sources of interstellar dust

・ H-stripped SNe (Type IIb/Ib/Ic) : aave < 0.01 μm➔ dust is almost completely destroyed by the reverse shocks➔ H-stripped SNe may be poor sources of interstellar dust‐Our model treating dust formation and evolution selfconsistently can reproduce IR emission from Cas A‐Condensation efficiency and average radius of dust
are uniquely determined by Λon = τsat / τcoll at the onset
time (ton) of dust formation

3. Dust formation in a cool denseshell (CDS) behind the SN shock3-1. Origin of IR emission from SNe
Dust formation in the ejecta

Dust formation in dense shellIR echo by CS dust

Shock heating of CS dust

3-2. Evidence for dust formation in SN 2006jc
Tominaga+08
optical・ brightening of IR・ rapid decline of optical light・ blueshift of emission lines
formation of CO/SiO molecules(more robust if SiO are depleted)

NIR

ejecta case

X-ray

dust formation in cool
dense shells (CDSs)
explains extinctionof zero-v component

Smith+08

CDS case

3-3. Dust formation in Type IIn SN 2010jl

carbonT = 1300 K

silicate
T = 1450 K

3-4. Dust properties in Type IIn SN 2010jl
opticallight curve

Dust in SN 2010jl
・ carbon grains
・ dust mass: ~10-3 Msun・ grain radius: <0.1μm(possibly <0.01 µm)
Maeda, TN, et al. (2013)

3-5. Dust formation in Type IIn SN 2010jl

Power-law size
distribution
・ α : ~3.5・ maximum radius :~3-4 µm (>0.5 μm)

Gall+2014, Nature3-6. Caveats on Gall et al. (2014) paper
Gall+2014, Nature
Dust formed incool dense shell

Dust formed in
the ejecta
Pre-existing
circumstellar dust

The mass of newly formed
dust increases with time?

We should not discuss
the mass of newly formed
grains by integrating theformation of dust in theejecta and CDS

3-7. Summary of dust formation in CDSs
‐Dust formation in cool dense shells (CDSs) is anotherformation path of dust in SNe➜ seems common for Type IIn SNe surrounded by dense gas‐The wavelength-dependence of extinction of emission
lines is a powerful tool to derive the size of dust
for Type IIn SN 2010jl
aave < 0.1 μm (Maeda+2013)aave > 0.5 μm (Gall+2014)‐We should distinguish between dust
formation in the ejecta and in CDSs
➜ Properties of dust formed in the CDSs
should not be adopted universally as theproperties of dust formed in CCSNe
Smith+2011