Blob resolution test
Blob resolution test Decoupled winds
Analytic Winds ¤ SPH Particle = collection of Nc cold clouds (flotsam) ¤ Pressure equil w/ambient gas
Ambient gas (kernel-smoothed)
Parameters: Mass of clouds, Mc, temperature Tc=104K
Analytic Winds: Forces ¤ Gravity + Ram pressure:
ρa Rc
vr
Analytic Winds: Heating ¤ Ram pressure: dE/dt = Framv ¤ Spitzer conduction: dE/dt ~ 4πRc2 Nc Ta5/2 (Ta-Tc)/Rc Ta
Tc=104K
Analytic Winds: Mixing ¤ Kelvin-Hemholtz τcc = (ρc/ρa)1/2 Rc/vr ¤ Conductive evaporation τevap ¤ Mix particle’s kT & Z with neighbors τmix = (τcc-1+τevap-1)-1
τmix
Analytic Winds: Evolution ¤ Assume pressure equilibrium: Rc evolves (on sound crossing timescale)
¤ Conserve momentum by recoiling neighbors. ¤ Conserve energy & metals during mixing. ¤ Within ISM: Assume ρa~10-2, Ta~106 like coronal gas ¤ Rejoin when |Tc-Ta| < εTTa AND |vc-va| < εvcs.
Test case ¤ nambient = 10-3 ¤ Mc = 103 M¤. ¤ Tc = 104K.
Analytic Winds: Metal mixing
Analytic Winds: Temperature
Galaxy properties gas metallicity (solar)
10.0
10-2 10-3 10-4 10-5 9
standard interactive winds 10 11 Stellar mass
100.00
1.0
standard interactive winds 0.1 9
12 1000.00
SFR
stel. mass func.
10-1
standard interactive winds
10 11 Stellar mass
12
10.00 1.00 0.10 0.01 9
10 11 Stellar mass
12
Gabor+in prep
Wind propagation & mixing ¤ No code follows kinetic ejection correctly, while superheating requires high resolution and results in mostly warm/hot outflow. How do we get the dynamic range we want with proper hydro? ¤ Mixing is too strong within mesh cells, too weak among SPH particles. What is the right balance? ¤ How do mixing and ejection differ in hot halos vs cool halos? How much hot gas makes a hot halo? ¤ Can we develop a set of post-Agertzian tests to quantify mixing & propagation in cold vs hot halos? ¤ What observations can shed light on this? (Cloud properties in outflows? Halo hot gas content?)
Analytic Winds ¤ SPH Particle = collection of Nc cold clouds (flotsam) ¤ Pressure equil w/ambient gas
Ambient gas (kernel-smoothed)
Parameters: Mass of clouds, Mc, temperature Tc=104K
Analytic Winds: Forces ¤ Gravity + Ram pressure:
ρa Rc
vr
Analytic Winds: Heating ¤ Ram pressure: dE/dt = Framv ¤ Spitzer conduction: dE/dt ~ 4πRc2 Nc Ta5/2 (Ta-Tc)/Rc Ta
Tc=104K
Analytic Winds: Mixing ¤ Kelvin-Hemholtz τcc = (ρc/ρa)1/2 Rc/vr ¤ Conductive evaporation τevap ¤ Mix particle’s kT & Z with neighbors τmix = (τcc-1+τevap-1)-1
τmix
Analytic Winds: Evolution ¤ Assume pressure equilibrium: Rc evolves (on sound crossing timescale)
¤ Conserve momentum by recoiling neighbors. ¤ Conserve energy & metals during mixing. ¤ Within ISM: Assume ρa~10-2, Ta~106 like coronal gas ¤ Rejoin when |Tc-Ta| < εTTa AND |vc-va| < εvcs.
Test case ¤ nambient = 10-3 ¤ Mc = 103 M¤. ¤ Tc = 104K.
Analytic Winds: Metal mixing
Analytic Winds: Temperature
Galaxy properties gas metallicity (solar)
10.0
10-2 10-3 10-4 10-5 9
standard interactive winds 10 11 Stellar mass
100.00
1.0
standard interactive winds 0.1 9
12 1000.00
SFR
stel. mass func.
10-1
standard interactive winds
10 11 Stellar mass
12
10.00 1.00 0.10 0.01 9
10 11 Stellar mass
12
Gabor+in prep
Wind propagation & mixing ¤ No code follows kinetic ejection correctly, while superheating requires high resolution and results in mostly warm/hot outflow. How do we get the dynamic range we want with proper hydro? ¤ Mixing is too strong within mesh cells, too weak among SPH particles. What is the right balance? ¤ How do mixing and ejection differ in hot halos vs cool halos? How much hot gas makes a hot halo? ¤ Can we develop a set of post-Agertzian tests to quantify mixing & propagation in cold vs hot halos? ¤ What observations can shed light on this? (Cloud properties in outflows? Halo hot gas content?)
