Stochastic Reconnection in Partially Ionized Gas:Progress Report
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Stochastic Reconnection in Partially Ionized
Gas:Progress Report
Stochastic Reconnection in Partially Ionized
Gas:Progress Report
A. Lazarian (UW-Madison)Collaboration with
J. Cho (UW-Madison and CITA)
A.Esquivel (UW-Madison)
H. Yan (UW-Madison)
E. Vishniac (Johns Hopkins)
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Questions to address?Questions to address?
• How does turbulence affect reconnection?
• What are the properties of turbulence in partially ionized gas?
• How does partial ionization change the expected reconnection rate?
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Motivation: Interstellar Fields• Turbulent: Re ~VL/ ~1010 >> 1
~ rLvth, vth < V, rL<< L
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Armstrong & Spangler (1995)Armstrong & Spangler (1995)
Lazarian& Pogosyan (00) &Starnimirovic & Lazarian (01) showed Kolmogorov velocityspectrum of HI here.
Slope ~ -5/3
Ele
ctro
n d
en
s ity
sp
ect
r um
AUpc
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What is the effect of Interstellar Tubrulence?
What is the effect of Interstellar Tubrulence?
• Makes boundary conditions difficult to control.
• X point reconnection is not feasible unless large scale field reconfigure themselves over hundreds of parsec scales.
• Fast local (e.g. X point) reconnection does not guarantee fast reconnection if the global outflow regions are narrow.
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Relation to Center ActivitiesRelation to Center Activities
• Properties of turbulence: related to “Magnetic Chaos and Transport”
• Reconnection and properties of turbulence are related to “Ion Heating”.
• Reconnection is an essential part of the picture of “Dynamo” and “Angular Momentum Transport”
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What is Stochastic Reconnection?What is Stochastic Reconnection?
• Stochastic reconnection:• The natural state of fluids
is turbulence.
• Presence of an stochastic component of the B field.
• Magnetic field lines dissipate not on their entire scale length (L), but on a smaller scale (||) determined by turbulence statistics.
• Many simultaneous S-P reconnections.
Lazarian & Vishniac (1999)
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Properties of Stochastic Reconnection
Properties of Stochastic Reconnection
• Can be both fast and slow (depending on the level of turbulence) (B!)
• Allows flares of reconnection.
• Depends of the properties of turbulence
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Partially ionzed gas:possible effects
Partially ionzed gas:possible effects
• Free diffusion of neutrals out of the current sheet. Probably not so important (Vishniac & Lazarian 1998, Heitsch & Zweibel 2003).
• Turbulence is affected by damping caused by neutrals. Is it fatal?
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Turbulence in partially ionized gas:Theoretical expectations
(from Lazarian, Vishniac & Cho 2004)
Turbulence in partially ionized gas:Theoretical expectations
(from Lazarian, Vishniac & Cho 2004)
• In partially ionized gas MHD turbulence does not vanish at the viscous damping scale.
• Magnetic intermittency increases with decrease of the scale.
• Turbulence gets resurrected at ion decoupling scale.
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B
Viscous magnetized fluid
Viscosity is important while resistivity is not.
~0.3pc in WNM
Does viscous damping scale
is the scale at which MHD
turbulence ends?
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Viscosity Damped Turbulence: New Regime of MHD Turbulence
Cho, Lazarian & Vishniac 2002b
E(k)~k-1intermittent
Numerical testing confirms that
magnetic turbulence does not die!!!
Expected: k-1 for magnetic field k-4 for kinetic energy
Scale dependent intermittency
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Viscosity damped turbulence protrudes up to the scales at which neutrals decouple from ions. After that the normal MHD turbulence in ionic fluid is restored.
Lazarian, Vishniac & Cho (2003)
Yet to be tested with two fluid code
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Results: Expected Reconnection Rates for Phases of ISM(from Lazarian, Vishniac & Cho 2004)
Results: Expected Reconnection Rates for Phases of ISM(from Lazarian, Vishniac & Cho 2004)
• Molecular cloud: 0.1 VA (L30/l303/2)
• Dark cloud: 0.1 VT MA1/2L30/l30
1/4)
• Cold Neutral Medium:
0.08 VTM2(L30/l303/2)
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Some Astrophysical Implications
Some Astrophysical Implications
• Removal of magnetic field during star formation
• Solar flares and particle acceleration
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Numerical TestingsNumerical Testings
• Numerical testing of the stochastic reconnection idea
• Further testing of the divergence of the field lines in the new regime of turbulence.
• Numerical testing of the resurrection of turbulence prediction (using two fluid code).
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SummarySummary
• Interstellar reconnection happens in turbulent medium and on very large scales.
• Turbulence and external forcing makes large scale X point not probable.
• Stochastic reconnection is fast, but it may also be slow.
• The research requires interaction with other directions of the Center.
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Compressible MHD Turbulence: Stimulating Prior Work
Compressible MHD Turbulence: Stimulating Prior Work
Higdon 1984 (anisotropy in compressible
MHD turbulence)
Goldreich & Shridhar 1995 (incompressible
MHD theory, hints about compressibility)
Lithwick & Goldreich 2001 (effects of compressibility)
Choice is biased by author’s preferences.
Longer list is in Cho, Lazarian & Vishniac 2003.
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Implication 1: CR transportS
catt
erin
g ef
fici
e ncy
(Kolmogorov)
Fast modes
Alfven modes are inefficient. Fast modes are efficient in spite of damping
Big difference!!!
From Yan & Lazarian 2002
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What are the scattering rates for different ISM phases?
Solid line is analytical resultsSymbols are numerical results
(a) gyroresonance is dominant; (b) the scattering in partially ionized media is not important.
From Yan & Lazarian 2004
GyroresonanceTTD
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Implication 2: Dust DynamicsImplication 2: Dust Dynamics
• Gyroresonace with fast modes is most efficient
• Grains get supersonic• Grains may get
aligned
From Yan & Lazarian 2003
Grain size
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Cascade time follows Kolmogorov scaling
tcas~k-2/3
Cho, Lazarian, & Vishniac 2002a
Implication 3: Decay of MHD turbulence
Implication 3: Decay of MHD turbulence
• Fast decay of MHD turbulence reported earlier is not due to coupling of compressible and incopressible motions!
Incompressible MHD turbulence
decays fast.
Inportant for star formation.
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Large scales
Normal MHD Turbulence
Viscosity damped regime
Large Scales
(Small k only)
Small Scales
(Large k only)
Magnetic
structures
perpendicular
to mean B. Intermittency is prominent
for new regime at small
scales.
Intermittent structures
Smaller and smaller
structures forming
at scales smaller
than the damping
scale.From Cho, Lazarian & Vishniac 2003
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Ordinary MHD New regime
Viscosity damped turbulence exhibits scale-dependent intermittency!
Cho, Lazarian & Vishniac 2003
Corresponds to prediction in Lazarian, Vishniac & Cho 2003
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Viscosity damped MHD turbulence results in a shallow
spectrum of density fluctuations. Could there be a relation
to tiny scale structures observed in the ISM?
From Cho & Lazarian 2003
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Why E(k)~k-1?
• Magnetic fluctuations evolve due to shear at the damping scale. => Cascade of magnetic energy with the fixed rate:
Expect to see a lot of magnetic structure belowthe viscous damping scale (e.g. below 0.3pc for WNM)
Bl2
diss
= const => Bl2 ~ const, or E(k)~k-1
kE(k)~Bl
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Genus analysis (cont.)Genus analysis (cont.)
• A shift from the mean can reveal “meatball” or “Swiss cheese” topology.
• Genus curve of the HI in the SMC and from compressible MHD simulations.
• The SMC show a evident “Swiss cheese” topology, the simulations are more or less symmetric.
• Genus are a quantitative measure of the topology, allows to test simulations & observations.
SMC
MHD