Lorem Ipsum Dolor Svitlana Zhukovska · Lorem Ipsum Dolor Lifecycle of dust in local galaxies...

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?


1. Grain cycle in multiphase ISM

Milky Way

Peters, SZ et. 2017

SImulating LifeCycle of Molecular Clouds


❖ 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


Milky Way

SImulating LifeCycle of Molecular Clouds

Cum

ulat

ive

distr

ibut

ion

Peters, SZ et. 2017



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)


cold, T<300K warm, 300K<T<105K hot, T>105K


Dwarf galaxy


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


Density when part enters a phase

Dwarf galaxy


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


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


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


Solar neighbourhood

Dwarf galaxy

.


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!



Hu, SZ et al. 2019

Dependence on pre-shock gas density

Chia-Yu Hu’s talk


Fraction of grains destroyed for vshock=100km/s, nH~0.3cm-3


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


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


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


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


4. Dust balance - Milky Way

SZ et al. 2017, 2018

3D models of dust evolution - silicate

Gas density Msunpc-2



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



[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



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?


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



SZ 2008, SZ and Gail 2009

Dust-to-gas and dust-to-metal profiles in Milky Way



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



❖ 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!

Lorem Ipsum Dolor Svitlana Zhukovska · Lorem Ipsum Dolor Lifecycle of dust in local galaxies...

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