imprs lindau, 6.2.2003 space weather and plasma simulation jörg büchner, mpae lindau...
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IMPRS Lindau, 6.2.2003
Space weather and plasma Space weather and plasma simulationsimulation
Jörg Büchner, MPAe LindauJörg Büchner, MPAe Lindau
Collaborators: Collaborators:
B. Nikutowski and I.Silin, LindauB. Nikutowski and I.Silin, Lindau
A. Otto, FairbanksA. Otto, Fairbanks
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IMPRS Lindau, 6.2.2003
OutlineOutline What is „Space Weather“: Manifestation, What is „Space Weather“: Manifestation,
consequences, action at Earth and in spaceconsequences, action at Earth and in space How does it work ? - Main scenarios of plasma How does it work ? - Main scenarios of plasma
heating and particle acceleration by artists‘s moviesheating and particle acceleration by artists‘s movies MODELING AND SIMULATION APPROACHESMODELING AND SIMULATION APPROACHES:: Force free magnetic fields -> lowest order solar Force free magnetic fields -> lowest order solar
fieldsfields Ideal MHD -> large scale motion in the coronaIdeal MHD -> large scale motion in the corona Resistive MHD -> reconnection in the transition Resistive MHD -> reconnection in the transition
regionregion Kinetic simulation -> dissipation, structure Kinetic simulation -> dissipation, structure
formationformation State of the art global simulation and outlookState of the art global simulation and outlook
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IMPRS Lindau, 6.2.2003
Manifestation: Aurora Manifestation: Aurora
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IMPRS Lindau, 6.2.2003
Action in SpaceAction in Space
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IMPRS Lindau, 6.2.2003
Space Weather: consequencesSpace Weather: consequences
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IMPRS Lindau, 6.2.2003
How does it work? How does it work? Solar Wind and Magnetic Solar Wind and Magnetic
Substorms Substorms
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IMPRS Lindau, 6.2.2003
Source: motion of solar Source: motion of solar plasmasplasmas
Solar plasma Solar plasma convection:convection:
Dynamo effect -> magnetic fields Dynamo effect -> magnetic fields Flows -> upward Poynting flux Flows -> upward Poynting flux
Estimated energy fluxes:Estimated energy fluxes:Active regions (0.5 -1) 104 W m-2Active regions (0.5 -1) 104 W m-2 Quiet regions 300 W mQuiet regions 300 W m-2-2
Coronal holes 800 W mCoronal holes 800 W m-2-2
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IMPRS Lindau, 6.2.2003
Typical dimensionless Typical dimensionless parametersparameters
If: L – Geometrical scale, n – Number density; If: L – Geometrical scale, n – Number density; Tj – Temperature and B – Magnetic field,
then:Tj – Temperature and B – Magnetic field, then:Ion-gyro radius:Ion-gyro radius:
Mean-free path:Mean-free path:
Dreicer-fieldDreicer-field
If EA > ED collisions don‘t prevent runaway: collisionless!If EA > ED collisions don‘t prevent runaway: collisionless!
<<
Magnetic Reynolds numberMagnetic Reynolds number
E = v B ~E = v B ~
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IMPRS Lindau, 6.2.2003
Typical valuesTypical values
Rm > 1 >> 1 >>>1Rm > 1 >> 1 >>>1
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IMPRS Lindau, 6.2.2003
Force-free approximationForce-free approximation
04:20 04:20 18.10.96 18.10.96 04:4004:40
i.e. Currents flow only parallel to the magnetic field ->
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IMPRS Lindau, 6.2.2003
Ideal MHD Ideal MHD (magnetohydrodynamics) (magnetohydrodynamics)
E + v x B=0 -> „ideal“ magnetohydrodynamics, i.e.E + v x B=0 -> „ideal“ magnetohydrodynamics, i.e.magnetic flux and plasma move togethermagnetic flux and plasma move together
SOHO-MDI photospheric B fields on 17./18.10.1996 60“, 23MmSOHO-MDI photospheric B fields on 17./18.10.1996 60“, 23Mm
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IMPRS Lindau, 6.2.2003
MHD Simulation mit MHD Simulation mit Dissipation und Dissipation und
Neutralgas-StößenNeutralgas-Stößen
Non-ideal MHD Non-ideal MHD simulationssimulations
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IMPRS Lindau, 6.2.2003
MHD Simulation mit MHD Simulation mit Dissipation und Dissipation und
Neutralgas-StößenNeutralgas-Stößen
Non-ideal MHD Non-ideal MHD simulationssimulations
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IMPRS Lindau, 6.2.2003
MHD - simulations: MHD - simulations: exampleexample
Eruptive Eruptive magneticmagneticReconnection Reconnection directly in the directly in the transition regiontransition region
The question remains The question remains open: what is the nature open: what is the nature of dissipation?of dissipation?-> plasmakinetic -> plasmakinetic investigation necessaryinvestigation necessary
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IMPRS Lindau, 6.2.2003
Next order - smaller - scalesNext order - smaller - scalesElectron equation of motion (Electron equation of motion (“Ohm’s law”“Ohm’s law”):):
• Below c/pi electrons and ions decouple, i.e. electrons are magnetized, ions not -> Plasma- Hall- Effect• Below c/pe : Electrons demagnetized as well
c/pic/pee <- Scales
Jpne1
BJnec1
Bvc1
EdtJd4
ei2pe
Electroninertia
Whistlerwaves
kinetic Alfvenwaves
<- Effects<- Effects
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IMPRS Lindau, 6.2.2003
Crucial point: current sheets
Lznn /cosh 20
yx j
cz
B 4
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IMPRS Lindau, 6.2.2003
Hall currents in current Hall currents in current sheets sheets
(Thin current sheet with io ~> L)
(Thin current sheet with io ~> L)
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IMPRS Lindau, 6.2.2003
Vlasov-code kinetic Simulation
0)(1 ,
,
,,,
v
fBv
cE
m
e
r
fv
t
f ei
ei
eieiei
vdfvej
vdfe
ei
Veijei
V
eieij
ei
3,
,,
3,
,,
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IMPRS Lindau, 6.2.2003
From microscopic fluctuations and From microscopic fluctuations and turbulence to a global instability: turbulence to a global instability:
TIMETIME
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IMPRS Lindau, 6.2.2003
From microscopic fluctuations and From microscopic fluctuations and turbulence to global instability: turbulence to global instability: SPACE
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IMPRS Lindau, 6.2.2003
Current sheet Current sheet decaydecay: from : from microscopic fluctuations to global microscopic fluctuations to global
instabilityinstability
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IMPRS Lindau, 6.2.2003
Microscopic dissipationIonen distribution in the
current directionElectron distribution in the
current direction
Ions drive waves → plateau - formation → electron-heating
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IMPRS Lindau, 6.2.2003
Current reduction -> disspation
Ion distribution function
Electron distribution function
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IMPRS Lindau, 6.2.2003
3D current instability3D current instability
Plasma density wave Plasma density wave
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IMPRS Lindau, 6.2.2003
Transition to reconnectionTransition to reconnection
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IMPRS Lindau, 6.2.2003
3D magnetic reconnection3D magnetic reconnection
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IMPRS Lindau, 6.2.2003
State of the art: global MHD State of the art: global MHD modelsmodels
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IMPRS Lindau, 6.2.2003
Multiscale processes in complex Multiscale processes in complex system system -> plasma simulations necessary-> plasma simulations necessary
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IMPRS Lindau, 6.2.2003
Comparison with Comparison with observationsobservations
IInternational program „nternational program „LLiving iving WWith a ith a SStar“ tar“ (ILWS)(ILWS) Missions 2006-08: SUNRISE, STEREO, MMS, SDO ...Missions 2006-08: SUNRISE, STEREO, MMS, SDO ...
South Pole Sitter
L2