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Disentangling the role ofsupernovae, stellar winds and
ionising radiation on thestructure of galactic discs
Frantisek Dinnbier
(University of Cologne)
SILCC collaboration: Stefanie Walch (PH1 Cologne), P. Clark (CardiffUniversity), D. Derigs (PH1 Cologne), P. Girichidis (AIP Potsdam),
S. Glover (ITA Heidelberg), S. Haid (PH1 Cologne), R. Klessen(ITA Heidelberg), T. Naab (MPA Garching), D. Seifried (PH1 Cologne),
R. Wunsch (AsU Prague)
6th September 2018
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The energy budget
ionising radiation and winds(early feedback), sharp dropafter t ∼ 5− 10Myr
SNe starting after ' 3Myr;they have approximatelyconstant rate
ionising radiation hassmaller coupling efficiency(by factor of ∼ 0.1− 0.01than winds or SNe)
Frantisek Dinnbier SNe, winds and ionising radiation in galactic discs
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The initial conditions
box of side lengths 500pc× 500pc× 10000pccentered at the galactic disc
resolution 4 pc
surface density of gas Σ = 10M� pc−2
self-consistent modelling of sink particleformation (star clusters) and their feedback
star clusters populated by a realistic IMF, oneSN per 120M� of the stellar population
gravitational acceleration due to gas, sinkparticles, background stellar potential coupledto mixed BCs
chemistry H, H+, H2, CO, C+
no magnetic field for now; spatially constantG0; no galactic shear
Frantisek Dinnbier SNe, winds and ionising radiation in galactic discs
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Modelling stellar feedback
SNe for ρ > 10−24 g.cm−3 →momentum injection
SNe for ρ < 10−24 g.cm−3 → thermalenergy injection
SNe have always fixed radius
Wind feedback by momentum injection
Ionising radiation traced by TreeRay
three thresholds for sink particleformation (implicit parameter;nonuniform SFR):ρ = 2.0× 10−22 g.cm−3,ρ = 2.0× 10−21 g.cm−3,ρ = 2.0× 10−20 g.cm−3 → 24simulations
Frantisek Dinnbier SNe, winds and ionising radiation in galactic discs
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Modelling stellar feedback
SNe for ρ > 10−24 g.cm−3 →momentum injection
SNe for ρ < 10−24 g.cm−3 → thermalenergy injection
Sne have always fixed radius
Wind feedback by momentum injection
Ionising radiation traced by TreeRay
three thresholds for sink particleformation (implicit parameter;nonuniform SFR):ρ = 2.0× 10−22 g.cm−3,ρ = 2.0× 10−21 g.cm−3,ρ = 2.0× 10−20 g.cm−3 → 24simulations
Frantisek Dinnbier SNe, winds and ionising radiation in galactic discs
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Modelling stellar feedback
SNe for ρ > 10−24 g.cm−3 →momentum injection
SNe for ρ < 10−24 g.cm−3 → thermalenergy injection
Sne have always fixed radius
Wind feedback by momentum injection
Ionising radiation traced by TreeRay
three thresholds for sink particleformation (implicit parameter;nonuniform SFR):ρ = 2.0× 10−22 g.cm−3,ρ = 2.0× 10−21 g.cm−3,ρ = 2.0× 10−20 g.cm−3 → 24simulations
Frantisek Dinnbier SNe, winds and ionising radiation in galactic discs
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Modelling stellar feedback
SNe for ρ > 10−24 g.cm−3 →momentum injection
SNe for ρ < 10−24 g.cm−3 → thermalenergy injection
Sne have always fixed radius
Wind feedback by momentum injection
Ionising radiation traced by TreeRay
three thresholds for sink particleformation (implicit parameter;nonuniform SFR):ρ = 2.0× 10−22 g.cm−3,ρ = 2.0× 10−21 g.cm−3,ρ = 2.0× 10−20 g.cm−3 → 24simulations
Frantisek Dinnbier SNe, winds and ionising radiation in galactic discs
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Overview of the SFR
For 30M�/ kpc2/Myr (Tammann+ 1994) → ∼ 750 SNe per
100Myr in the box
nsink[cm-3]
103
102
101
NoFB
Massinmassivestarsatt=100Myr
Dinnbieretal.,inprep.
NumberofSinksatt=100Myr
HighSFRLowSFR
Kennicu,-Schmidtvalue
Frantisek Dinnbier SNe, winds and ionising radiation in galactic discs
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Overview of the SFR
For 30M�/ kpc2/Myr (Tammann+ 1994) → ∼ 750 SNe per
100Myr in the box
Frantisek Dinnbier SNe, winds and ionising radiation in galactic discs
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SNe feedback only
Frantisek Dinnbier SNe, winds and ionising radiation in galactic discs
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SNe and wind feedback
Frantisek Dinnbier SNe, winds and ionising radiation in galactic discs
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Ionising radiation only
Frantisek Dinnbier SNe, winds and ionising radiation in galactic discs
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SNe, wind and ionising radiation
Frantisek Dinnbier SNe, winds and ionising radiation in galactic discs
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Volume filling fraction of the warm medium(300K < T < 1.0× 104 K)
Frantisek Dinnbier SNe, winds and ionising radiation in galactic discs
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Volume filling fraction of the warm-hot medium(1.0× 104 K < T < 3.0× 105 K)
Frantisek Dinnbier SNe, winds and ionising radiation in galactic discs
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Volume filling fraction of the hot medium(3.0× 105 K < T )
Frantisek Dinnbier SNe, winds and ionising radiation in galactic discs
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The mass loading factor
SNe drive outflows
winds are unable to drivestrong outflows
when acting together withSNe, ionising radiationtends to decrease massloading
Frantisek Dinnbier SNe, winds and ionising radiation in galactic discs
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Conclusions
Ionising radiation increases the volume filling factor of the warmphase and decreases the volume filling factor of the hot phase.
When the ionising radiation is included, the values for the VFFare closer to the observed values than with SNe only → ionisingradiation is likely to be important to properly model galacticdiscs.
When included in self-consistent model of star formation,ionising radiation decreases the SFR substantially more thanstellar winds.
The role of stellar winds is subordinate to ionising radiation insetting the phases of the ISM, and regulating star formation.
Frantisek Dinnbier SNe, winds and ionising radiation in galactic discs
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Thank you for your attention
Frantisek Dinnbier SNe, winds and ionising radiation in galactic discs