Dynamics of Multi-Phase Interstellar Medium Shu-ichiro Inutsuka (Nagoya Univ) Thanks to Hiroshi...
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![Page 1: Dynamics of Multi-Phase Interstellar Medium Shu-ichiro Inutsuka (Nagoya Univ) Thanks to Hiroshi Koyama (Univ. Maryland) Tsuyoshi Inoue (Kyoto Univ.) Patrick.](https://reader030.fdocuments.net/reader030/viewer/2022033105/56649e0e5503460f94af8b51/html5/thumbnails/1.jpg)
Dynamics of Multi-Phase Interstellar Medium
Shu-ichiro Inutsuka (Nagoya Univ)
Thanks to Hiroshi Koyama (Univ. Maryland)Tsuyoshi Inoue (Kyoto Univ.)Patrick Hennebelle (Paris Obs. & ENS)Masahiro Nagashima (Nagasaki Univ.)
Keywords:radiative cooling/heating, thermal instability,MHD, ambipolar diffusion, etc.
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Polarization Map of Synchrotron Rad
Depolarized region looks likeCanal!
No good theory yet!
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n vs Height from Galactic Midplane
Ferrière 2001, Rev.Mod.Phys. 73, 1031H2 gas
ionized gas
HI gas
average number density n cm-3
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Vertical (Quasi-)Hydrostatic Equilibrium?
PCR > Pmag > Pgas Parker Instability?
Pgas
Ferrière 2001, Rev.Mod.Phys. 73, 1031
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Various Components (Radial)
NGC6946
MRI does not explain this!
equipartition assumed
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M51 Synchrotron
Polarization(Fletcher & Beck 2005)
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Dynamical Timescale of ISM
Dynamical Three Phase Medium– McKee & Ostriker 1977
SN Explosion Rate in Galaxy… 1/(100yr) Expansion Time…1Myr Expansion Radius… 100pc
( 10-2 yr-1 )( 106 yr )( 100pc ) 3 = 1010 pc3 VGal.Disk
Dynamical Timescale of ISM 1Myr
« Timescale of Galactic Density Wave 100Myr
(10kpc)2
100pc
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CGPS data in W5 HII region
21cm continuum (HII gas) Tb=5K (bright) → 12.5K (dark)
Image : 60m dust emissionContour : 12CO(1-0) @ vLSR=-39.8 km/s
Ionized gas is surrounded with the dust shell. Distribution of CO molecules show poor correlation with the dust shell.
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CGPS data in W5 HII regionHI 21cm emission @ vLSR=-39.8 km/s
: Tb=45K (bright) → 110K (dark)
Shell-like HI Self-Absorption feature is found around W5. HISA feature overlaps with the dust shell.
Hosokawa & SI 2007, ApJ 664, 363
See also recent Planck paper (arXiv1101.2029) on “Dark Gas”
contour : 60μm dust emission
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Radiative Equilibrium
WNM(Warm Medium)
CNM(Cold Medium)
Solid: NH=1019cm-2, Dashed: 1020cm-2
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Radiative Cooling & HeatingSolid: Cooling, Dashed: Heating
Koyama & Inutsuka (2000) ApJ 532, 980 , based on Wolfire et al. 1995
grains
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2D Evolution from Unstable Equilibrium
Periodic Box Evolution without Shock Driving
With Cooling/Heating and Thermal Conduction
Without Physical Viscosity Pr = 0
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1D Shock Propagation into WNM
Density-Pressure Diagram
Density-Temperature Diagram– through unstable region
unstable
Koyama & SI 2000, ApJ 532, 980
See also Hennebelle & Pérault 1999
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20 p
c104*104 pixels
10,0002
Hennebelle & Audit 07
Audit & Hennebelle 20073D simulations12003
Heitsch et al. 40962
2D
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Property of "Turbulence"
v < CS,WNM Kolmogorov-like SpectrumHennebelle & Audit 2007
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Property of "Turbulence"
v < CS,WNM Kolmogorov-like
Spectrum
Hennebelle & Audit 2007
Armstrong, Rickett, & Spangler 1995
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Evaporation of Spherical CNM in WNM
Smaller CNM cloud evaporates:R~0.01pc clouds evaporate in ~Myr
condensationevaporation
Analytic Formula
Nagashima, Koyama, Inutsuka & 2005, MNRAS 361, L25Nagashima, Inutsuka, & Koyama 2006, ApJL 652, L41
Evaporation Timescale
Size of CNM cloud
CNM
WNM
Rc
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Evaporation of Spherical CNM in WNM
If the ambient pressure is larger, the critical size of the stable cloud is smaller.
"Tiny Scale Atomic Structure"? Braun & Kanekar 2005
Nagashima, Inutsuka, & Koyama 2006, ApJL 652, L41
Ambient Pressure
Critical
Radius
CNM
WNM
Rc
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Summary• Shock waves in ISM create
Turbulent CNM embedded in WNM.• In Turbulent Multi-Phase ISM
– Thermal Instability, Magnetic Field, Ambipolar Diffusion, etc.
What nextTurbulent Diffusion of Magnetic FieldParticle AccelerationOverall Modeling of Gaseous Galactic Halo
Good Information from CMB observations