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Lorem Ipsum Dolor
Lifecycle of dust in local galaxies
Svitlana Zhukovska Exeter University
Dusting the Universe - Tucson - 4-8 March 2019
Thorsten Naab (MPA), Chia-Yu Hu (CCA) Clare Dobbs (Exeter University)
Dmitry Semenov & Thomas Henning (MPIA)
Svitlana Zhukovska Life cycle of grains in local galaxies 4/3/2019
Outline
COLD CLOUDS DIFFUSE MEDIUM
AGB stars
SN II
Young stars
Dust shattering, disruption by SNe
Dust growth by accretion
New grains
SN Ia
1. Cycling of grains through ISM phases
2. Destruction of grains in ISM3. Grain growth
4. Where is dust balance in local galaxies?
Svitlana Zhukovska Life cycle of grains in local galaxies 4/3/2019
1. Grain cycle in multiphase ISM
Milky Way
Peters, SZ et. 2017
SImulating LifeCycle of Molecular Clouds
Svitlana Zhukovska Life cycle of grains in local galaxies 4/3/2019
❖ Longer residence times in H2 than molecular phase
❖ Broad distribution of tres
❖ Mean values residence time tres:
18 Myr , 8 Myr, 36 Myr, 9 Myr
1. Grain cycle in multiphase ISM
Milky Way
SImulating LifeCycle of Molecular Clouds
Cum
ulat
ive
distr
ibut
ion
Peters, SZ et. 2017
Svitlana Zhukovska Life cycle of grains in local galaxies 4/3/2019
1. Grain cycle in multiphase ISM
Dwarf galaxy
Hu, Naab, Glover et al. 2017
❖ GADGET-3 with SPH implementation (SPHGal):
❖ self-gravity
❖ non-equilibrium cooling and chemistry
❖ interstellar radiation fields (ISRF)
❖ shielding
❖ star formation
❖ stellar feedback (photoionisation, SNe)
Svitlana Zhukovska Life cycle of grains in local galaxies 4/3/2019
cold, T<300K warm, 300K<T<105K hot, T>105K
1. Grain cycle in multiphase ISM
Dwarf galaxy
Svitlana Zhukovska Life cycle of grains in local galaxies 4/3/2019
hot
cold
warm
SZ et al. in prep.
l
og n
gas [
cm-3
]
log
nga
s [cm
-3]
l
og n
gas [
cm-3
]
log
nga
s [cm
-3]
tres [Gyr]
hot
cold
warm
Maximum density in a phase
1. Grain cycle in multiphase ISM
Density when part enters a phase
Dwarf galaxy
Svitlana Zhukovska Life cycle of grains in local galaxies 4/3/2019
Mean: 18 Myr, 8 Myr, 36 Myr, 9 MyrMedian: 15 Myr, 5 Myr, 44 Myr, 2 Myr
Mean: 28 Myr, 191 Myr, 3 MyrMedian: 13 Myr, 63 Myr, 1 Myr
1. Grain cycle in multiphase ISM
Dwarf galaxy Solar neighbourhood
Cum
ulat
ive
distr
ibut
ion
0
0.2
0.4
0.6
0.8
1
10 20 30 40 50 60 70 80
Cum
ulat
ive
distr
ibut
ions
tres [Myr]
coldwarm
hot
Svitlana Zhukovska Life cycle of grains in local galaxies 4/3/2019
cold hotwarm
0.9
0.9 0.3
0.3
Peters, SZ et al. 2017SZ et al. in prep
Mass exchange rates M/M in Gyr-1
1. Grain cycle in multiphase ISM
Solar neighbourhood
Dwarf galaxy
.
Svitlana Zhukovska Life cycle of grains in local galaxies 4/3/2019
2. Dust destruction - theory
❖ Main mechanisms of destruction in shocks❖ thermal sputtering T>105K❖ inertial sputtering of atoms at shock v> 100 km/s❖ evaporation in high-velocity grain-grain collisions
❖ PAHs do not survive in shocks with v > 150 km/s
vshock=100 km/s
Bocchio et al. 2014
—— silicate—— carbonaceous (a-C:H)
before shock
after shock
McKee 1989, Tielens+1994, Jones +1994, 1996, Dwek+1996, Bocchio+2014, Slavin+2015
Small grains destroyed by shocks -shattering is important to recover
small grain population!
Svitlana Zhukovska Life cycle of grains in local galaxies 4/3/2019
2. Dust destruction - theory
Hu, SZ et al. 2019
Dependence on pre-shock gas density
Chia-Yu Hu’s talk
Svitlana Zhukovska Life cycle of grains in local galaxies 4/3/2019
Fraction of grains destroyed for vshock=100km/s, nH~0.3cm-3
2. Dust destruction - theory
silicates carbonaceous
Draine&Salpeter (1979), Seab&Shull (1983), McKee et al. (1987), Jones et al. (1994, 1996), Serra Diaz-Cano&Jones (2008), Bocchio et al. (2014), Slavin et al. (2015), Hu et al. (2019)
0
20
40
60
80
100
1975 1980 1985 1990 1995 2000 2005 2010 2015 2020
Frac
tion
dest
roye
d, %
graphitea-C:H
silicate
Svitlana Zhukovska Life cycle of grains in local galaxies 4/3/2019
2. Dust destruction - SNR observations
❖ Blair et al. 2008 Kepler SNR 75%❖ Arendt et al. 2010 Puppis A SNR 25%
❖ Williams et al. 2006, Borkowski et al. 2006
4 SNRs of CC SNe4 SNRs of SN Ia
90% of grains with a<40nm 30-40% for larger grains
❖ Sankrit et al. 2014 Cygnius Loop 40-50%
❖ Dopita et al. 2016 N49 30-40%
Milky Way
LMC
LMC SMC
❖ Temim et al. 2016 7.7 ± 3.3 3.3 ± 1.8
❖ Lacievic et al. 2015 1.2 -11.2
Dust mass destroyed, M⊙
Dust fraction destroyed
LMC SMC
Svitlana Zhukovska Life cycle of grains in local galaxies 4/3/2019
2. Dust destruction - lifetimes of grains
Barlow (1978), Jones et al. (1994, 1996), Serra Diaz-Cano&Jones (2008), Micelotta et al. (2010), Bocchio et al. (2014), Jones and Nuth (2011), Slavin et al. (2015), Zhukovska et al. (2016), Hu et al. (2019)
0
0.5
1
1.5
2
2.5
3
3.5
1975 1980 1985 1990 1995 2000 2005 2010 2015 2020
Du
st lif
eti
mes
[Gyr]
Publication year
graphitesilicate
a-C:HPAH
Milky Way
Svitlana Zhukovska Life cycle of grains in local galaxies 4/3/2019
3. Dust production
AGB stars: Ferrarotti&Gail 2006, Zhukovska+2008, Ventura+2012a,b, Nanni+2013, 2014, Di Criscienzo+2013
SNe: Marassi et al. 2019, Matsuura+2017, Sarangi+2018, Micelotta+2018, Jeonghee Rho’s talk
Stellar dust inputStar formation history Gas enrichment history
ISM dust growthISM evolution
dynamicschemistry
Dust, gas enrichment history
Grain sizescomposition
amount
Stellar yields
Svitlana Zhukovska Life cycle of grains in local galaxies 4/3/2019
4. Dust balance - Milky Way
SZ et al. 2017, 2018
3D models of dust evolution - silicate
Gas density Msunpc-2
Svitlana Zhukovska Life cycle of grains in local galaxies 4/3/2019
4. Dust balance - Milky Way
SZ et al. 2017, 2018
❖ Growth in ISM is limited to Tgas<300K and enhanced due to grain charges ❖ Silicates grains with sizes 4 - 250 nm❖ Double-slope relation explained by dust growth
-2
-1.5
-1
-0.5
0
1018 1019 1020 1021 1022
[Si/H
] gas
NH [cm-2]
3D models of dust evolution - silicate
Voshchinnikov & Henning (2010)
no grain charges
[Si g
as/H
]log n(H) [cm-3]
CMRN4nmECMRN4nm
-2.5
-2
-1.5
-1
-0.5
0
-2 -1 0 1 2 3
Observations
Svitlana Zhukovska Life cycle of grains in local galaxies 4/3/2019
4. Dust balance - Milky Way
[Fe g
as/H
]
log n(H) [cm-3]
CMRN1nmECMRN1nm
-3
-2.5
-2
-1.5
-1
-0.5
0
-2 -1 0 1 2 3-3
-2.5
-2
-1.5
-1
-0.5
0
1018 1019 1020 1021 1022
Fe
[Fe/
H] g
as
NH [cm-2]
ECMRN1nmno grain charges
SZ et al. 2018
❖ Small iron grains with sizes 1 - 10 nm - large surface area!❖ A fraction solid iron is protected in silicate grains from destruction?
Dwarf irregulars and DLAs also need iron nano-grains to explain depletions (Gioannini et al. 2018)
3D models of dust evolution - iron
Svitlana Zhukovska Life cycle of grains in local galaxies 4/3/2019
4. Dust balance - Milky Way
Zhukovska et al. 2018
10-10
10-5
100
105
1010
0 50 100 150 200 250 300
τ sca
, τde
s [s
]
Td [K]
τdesτsca, a=3 nmτsca, a=1 nm
Dust temperature
Timescales of scanning, desorption
Td maxTd max100
101
102
103
104
105
106
107
100 101 102 103 104 105 106τ r
ad [s
]E/hc [cm-1]
iron, a=3 nmiron, a=1 nmsilicate, a=3 nmsilicate, a=1 nm
Timescales of radiative cooling
Photon energy
How frequent are UV photon absorptions?For 3 nm sized iron particle: the mean time between two UV
absorptions 1.2d and total number of absorptions in CNM 3 × 109
How do grains grow?
Svitlana Zhukovska Life cycle of grains in local galaxies 4/3/2019
4. Dust balance in local galaxies
Chiang et al. 2018
Dus
t-to-
met
al ra
tio
Dus
t-to-
gas
ratio
Spatially resolved dust and metal in M101
❖ Negative dust-to-metal gradient❖ Decreasing DTM in regions dominated by atomic H
Svitlana Zhukovska Life cycle of grains in local galaxies 4/3/2019
4. Dust balance in local galaxies
SZ 2008, SZ and Gail 2009
Dust-to-gas and dust-to-metal profiles in Milky Way
Svitlana Zhukovska Life cycle of grains in local galaxies 4/3/2019
4. Dust balance in local galaxies
Mattsson et al. 2014
Observed negative dust-to-metal gradients support dominance of dust growth over destruction
log
Dus
t-to-
met
al ra
tio
log
Dus
t-to-
met
al ra
tio
Des
truct
ion
para
met
er
Gro
wth
par
amet
er
Only destruction, no growth, no stars Only growth, no destruction, no stars
Svitlana Zhukovska Life cycle of grains in local galaxies 4/3/2019
4. Dust balance in local galaxies
❖ Dust-to-gas—metallicity relation is best reproduced with low efficiencies of dust condensation in SNe
❖ Dust growth in ISM becomes important with increase of metallicity
Remy-Ruyer…, SZ et al. 2014, Zhukovska 2014
Dwarf galaxies
-7
-6
-5
-4
-3
-2
-1
6.5 7 7.5 8 8.5 9 9.5
log
Dus
t-to-
gas
ratio
12 + log(O/H)
Model 1Model 2Model 5Model 6Model 7
DGS, Madden+2012KINGFISH, Kennicutt+2011Supernovae
AGB stars
ISM-growth
Svitlana Zhukovska Dust growth in the ISM: clues from depletions 05/06/2018
Thanks for your attention!