2012/12/12

Dust in supernovae
Takaya Nozawa
Kavli IPMU (Kavli Institute for the Physics andMathematics of the Universe)

Collaborators:
T. Kozasa, A. Habe (Hokkaido University)
K. Maeda, K. Nomoto (K-IPMU)
H. Umeda (U.T.), N. Tominaga (Konan Univ.)

1-1. Introduction
・ SNe are important sources of interstellar dust?
－ huge amounts of dust grains (>108 Msun) are detectedin host galaxies of quasars at redshift z > 5➔ 0.1 Msun of dust per SN is needed to be ejected toexplain such massive dust at high-z (Dwek et al. 2007)－ contribution of dust mass from AGB stars and SNen(AGB stars) / n(SNe) ~ 10-20
Mdust = 0.01-0.05 Msun per AGB (Zhukovska & Gail 2008)
Mdust = 0.1-1.0 Msun per SN (Nozawa et al. 2003; 2007)

What composition, size, and mass of dust
can be formed in SNe?

1-2. Summary of observed dust mass in CCSNe
SN1987A
CrabtheoryCas A
missing cold dust?

young SNRs

swept-up IS dust?
young SNeby courtesy of M. Tanaka

FIR to sub-mm observations have revealed the presenceof massive (>0.1 Msun) dust grains in the ejecta of CCSNe

1-2. Summary of observed dust mass in CCSNe
SN1987A
CrabtheoryCas A
missing cold dust?

young SNRs

swept-up IS dust?

FIR to sub-mm observations
have revealed the presence
young SNeof massive (>0.1 Msun) dust grains in the ejecta of CCSNe
by courtesy of M. Tanaka

What mass of the newly formed grains can survive to be
injected into the interstellar space?

1-3. Emission and absorption efficiency of dust
○ Thermal radiation from dust grainsFλ ∝ 4πa2 Qemis(a,λ) πBλ(Tdust) # Qemis = Qabs
carbonsilicate(Qemis/a) is independent of aFλ ∝ 4πa3 (Qemis[a,λ]/a) πBλ(Tdust)∝ 4 Mdust κemis(λ) πBλ(Tdust)➔ IR emission is derived given Mdust, κabs, and Tdust1-4. Composition of dust formed in SNe
IS dust : carbonaceous grain andsilicate (MgSiO3, MgFeSiO4, …)
SN 2004et

SN 2006jc

silicate➔ 1750 K

silicate

carbon

SN 2004et, Kotak+09

carbon➔ 1660 K

SN 2006jc, Smith+08
SN 2010jl, Keiichi’s talk2. Formation and evolution of dustin supernovae

He coreFSRSCD2-1. Dust formed in Type II-P SNeaverage radius
0.01 μm

Umeda & Nomoto+02

Condensation time

－ various dust species form
according to compositionof gas in each layer－ condensation time:
300-600d after explosion－ average radii: >~0.01 μm
Nozawa+03, ApJ, 598, 785

2-2. Evolution of dust in SNRs
Nozawa+07, ApJ, 666, 955

Model : Type II-P
Mpr= 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

2-3. 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 dustby reverse shock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－ M(56Ni) = 0.07 Msun

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

0.01 μm－ the radius of dust formedin H-stripped SNe is small－ condensation time of dust
300-700d after explosion

・ SN IIb without massive
H-env ➔ adust < 0.01 μm－ total mass of dust formed
・ 0.167 Msun in SN IIb
・ 0.1-1 Msun in SN II-P・ SN II-P with massive
H-env ➔ adust > 0.01 μm

Nozawa+10, ApJ, 713, 356

3-3. Evolution of dust in Type IIb SNRTime evolution of dust mass

predicted IR SED at 330 yr

330 yrAlmost all newly formed
grains are destroyed inshocked gas in the SNR
Herschelobservation
due to small
radius ofMd,cool= 0.075
Msun
newlyformed
dust
Tdust ~ 35 K
(Barlow+10)
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

4-1. 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

4-2. Dust formation and evolution in SNe Ia
average radius

Nozawa+11, 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

4-3. Carbon dust and outermost layer
・ There has been no evidence for dust formation in SNe Ia➔ Formation of massive carbon dust does not matchthe observations－ C dust mass: ~0.001 Msun
－ massive unburned carbon(~0.05 Msun) in deflagration

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

Observational data: SN 2005df at
day 200 and 400 (Gerardy+07)

The presence of unburned
carbon-rich layer always
involve formation of C dust

4-4. Dust formation in super-Chandra SNe?
－ super-Chandra SNe :Meje ~ 2.0 Msun

SN 2009dc, Tarbenberger+10

detection of CII line
➔ presence of massive
unburned carbon
SN 2006gz, Maeda+09

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

5. Summary of this talk・ SNe II-P can inject a large amount of dust (>0.1 Msun)－ almost all Mg, SI, and Fe atoms are trapped in dust
－ FIR observations of SNe support massive dust・ 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 selfconsistently can reproduce IR emission from Cas A・ Formation of C dust in SNe Ia may give some hints onthe composition of outermost layers