1. Overview of CMSO Center for Magnetic Self-Organization in Laboratory and Astrophysical Plasmas
S. Prager
May, 2006

2. Outline Physics topics Participants Physics goals and highlights
Educational outreach
Management structure
Funding

3. Magnetic self-organization

4. The nonlinear plasma physics

5. Magnetic self-organization in the lab
magnetic fluctuations
(reconnection)
toroidal magnetic flux
dynamo
heat flux
(MW/m2)
energy transport
rotation
(km/s)
momentum transport
ion temperature
(keV)
ion heating
time (ms)

6. CMSO goal: understand plasma physics needed to solve key laboratory and astrophysical problems
linking laboratory and astrophysical scientists
linking experiment, theory, computation

7. Original Institutional Members
Princeton University
The University of Chicago
The University of Wisconsin
Science Applications International Corp
Swarthmore College
Lawrence Livermore National Laboratory
~25 investigators,
~similar number of postdocs and students
~ equal number of lab and astrophysicists

8. With New Funded Members
Princeton University
The University of Chicago
The University of Wisconsin
Science Applications International Corp
Swarthmore College
Lawrence Livermore National Laboratory
Los Alamos National Laboratory (05)
University of New Hampshire (05)
~30 investigators,
~similar number of postdocs and students
~ equal number of lab and astrophysicists

9. Cooperative Agreements (International)
Ruhr University/Julich Center, Germany(04)
Torino Jet Consortium, Italy (05)

10. Experimental facilities
yields range of topologies and critical parameters
Joint experiments and shared diagnostics

11. MST: Madison SymmetricTorus (Wisconsin)
MRX: Magnetic Reconnection
Experiment (Princeton)
SSX: Swarthmore Spheromak
Experiment
MST: Madison SymmetricTorus (Wisconsin)
SSPX: Sustained Spheromak Physics
Experiment (LLNL)

12. MRX SSX Inductively produced plasmas, Spheromak or annular plasmas
Locailzed reconnection at merger
SSX
Electrostatically - produced spheromaks (by plasma guns)
Two spheromaks reconnect and merge

13. SSPX
Electrostatically - produced spheromak
MST
Reversed field pinch

14. Liquid gallium MRI experiment (Princeton)
To study the magnetorotational instability

15. Major Computational Tools
Not an exhaustive list
Codes built largely outside of CMSO
Complemented by equal amount of analytic theory

16. Sample Physics Highlights
New or emerging results
Mostly where center approach is critical
We are pursuing much of the original plans,
but new investigations have also arisen
(plans for next 2 years discussed later)

17. Reconnection Two-fluid Hall effects Reconnection with line tying
Effects of coupled reconnection sites
Effects of lower hybrid turbulence
not foreseen in proposal

18. Hall effects on reconnection
Identified on 3 CMSO experiments
(MRX, SSX, MST)
Performed quasilinear theory
Will study via two-fluid codes (NIMROD, UNH) and possibly via LANL PIC code

19. Observation of Hall effects
Observed quadrupole B component,
MRX SSX
radius
also observed in magnetosphere

20. Reconnection with line-tying
Studied analytically (UW, LANL) and computationally(UW)
Compare to non-CMSO linear experiments
Features of periodic systems survive
(e.g.,large, localized currents)

21. v radius Linear theory for mode resonance in cylinder periodic
line-tied
radius
radius

22. Effects of multiple, coupled reconnections
Many self-organizing effects in MST occur ONLY with
multiple reconnections

23. Effects of multiple, coupled reconnections
Many self-organizing effects in MST occur ONLY with
multiple reconnections
core reconnection only
multiple reconnections
core
core reconnection
edge
edge reconnection

24. Applies to magnetic energy release, dynamo, momentum
transport, ion heating
Related to nonlinear mode coupling
Might be important in astrophysics where multiple
reconnections may occur
(e.g., solar flare simulations of Kusano)

25. Lower hybrid turbulence
Detected in MRX
Magnetic fluctuations
f(MHz)
Reconnection rate  turbulence amplitude;
Instability theory developed,
May explain anomalous resistivity

26. Lower hybrid turbulence
Detected in MRX
Similar to turbulence in magnetosphere (Cluster)
Magnetic fluctuations E B
f(MHz)
Reconnection rate ~ turbulence amplitude;
Instability theory developed,
May explain anomalous resistivity

27. Momentum Transport radial transport of toroidal momentum
In accretion disks, solar interior, jets, lab experiments, classical viscosity fails to explain momentum transport

28. Leading explanation in astrophysics
MHD instability
Flow-driven (magnetorotational instability)
momentum transported by j x b and v.v
Leading explanation in lab plasma
resistive MHD instability
current-driven (tearing instability)
momentum transported by j x b and v.v

29. Momentum Transport Highlights
MRI in Gallium: experiment and theory
MRI in disk corona: computation
Momentum transport from current-driven reconnection

30. MRI in Gallium Experiment (Princeton) hydrodynamically stable, Vvq r
--- Couette flow
+ diff. endcaps
+ end caps rotate
with outer cyl.
Couette flow
Experiment (Princeton)
hydrodynamically stable,
ready for gallium V
experiment
radius
Simulation (Chicago)
underway

31. Combines idea from Princeton, code from SAIC
MRI in disk corona
Investigate effects of disk corona on momentum transport; possible strong effect
Combines idea from Princeton, code from SAIC
initial state: flux dipole
...after a few rotations

32. Momentum transport from current-driven reconnection
experiment
Requires multiple tearing modes (nonlinear coupling)

33. Theory and computation of Maxwell stress in MHD
resonant
surface
quasilinear theory for one tearing mode
computation for multiple, interacting modes
An effect in astrophysical plasmas?
reconnection and flow is ubiquitous
raises some important theoretical questions
(e.g., effect of nonlinear coupling on spatial structure)

34. Ion Heating

35. Ion heating in solar wind
thermal speed km/s
r/Rsun
Strong perpendicular heating of high mass ions

36. Ion heating in lab plasma
Observed during reconnection in all CMSO experiments
Ti (eV)
MST
t = ms
t = ms
radius

37. Conversion of magnetic energy to ion thermal energy
~ 10 MW flows into the ions

38. change in ion thermal energy (J)
MRX
reconnected magnetic field energy (J)

39. Magnetic energy can be converted to Alfvenic jets
SSX
Energetic ion flux
time (s)

40. Ions heated only with core and edge reconnection
MST
core reconnection
core
edge
edge reconnection
Ti (eV)
time (ms)

41. What is mechanism for ion heating?
Still a puzzle
Theory of viscous damping of magnetic fluctuations has been developed

42. Magnetic chaos and transport
Magnetic turbulence
Transport in chaotic magnetic field

43. Magnetic chaos and transport
Magnetic turbulence
Star formation
Heating via cascades
Scattering of radiation
Underlies other CMSO topics
Transport in chaotic magnetic field
Heat conduction in galaxy clusters (condensation)
Cosmic ray scattering

44. Magnetic turbulence Properties of Alfvenic turbulence
Intermittency in magnetic turbulence
Comparisons with turbulence in experiments
Sample results:
Intermittency explains pulsar pulse width broadening,
Observed in kinetic Alfven wave turbulence
computation
Measurements underway in experiment for comparison

45. Transport in chaotic field
Experiment
measure transport vs gyroradius in chaotic field

46. Transport in chaotic field
Experiment
measure transport vs gyroradius in chaotic field
Result
Small gyroradius (electrons): large transport
Large gyroradius (energetic ions): small transport
Ion orbits well-ordered
Transport measured via neutron emission from energetic ions produced by neutral beam injection
Possible implications for relativistic cosmic ray ions

47. The Dynamo

48. Why is the universe magnetized?
Growth of magnetic field from a seed
Sustainment of magnetic field
Redistribution of magnetic field

49. Why is the universe magnetized?
Growth of magnetic field from a seed
primordial plasma
Sustainment of magnetic field
e.g., in solar interior
in accretion disk
Redistribution of magnetic field
e.g., solar coronal field
extra-galactic jets

50. The disk-jet system Field produced from transport
Field sustained (the engine)

51. CMSO Activity Theoretical work on all problems
the role of turbulence on the dynamo,
flux conversion in jets,
Lab plasma dynamo effect:
field transport,
with physics connections to growth and sustainment

52. Abstract dynamo theory
Small-scale field generation (via turbulence)
Computation: dynamo absent at low /
Theory: dynamo present at high Rm
Magnetic field fluctuations generated by turbulent convection
Large-scale field generation
No dynamo via homogeneous turbulence,
Large-scale flows sustains field
Dynamo action driven by shear and magnetic buoyancy instabilities.

53. MHD computation of Jet production
Magnetically formed jet
|J| contours

54. MHD computation of Jet evolution
Magnetically formed jet
|J| contours
helical fields
develop in jet
When kink unstable, flux conversion B -> Bz
Similarities to experimental fields

55. Dynamo Effect in the Lab
in experiment
E||
j||
radius
additional current drive mechanism (dynamo)

56. Hall dynamo is significant
(theory significant)

57. Hall dynamo is significant
experiment:
Laser Faraday rotation

58. Questions for the lab plasma, relevant to astrophysics
At what conditions (and locations) do two-fluid and MHD dynamos dominate?
Is the final plasma state determined by MHD, with mechanism of arrival influenced by two-fluid effects?
Is the lab alpha effect, based on quasi-laminar flows, a basis for field sustainment
(possibly similar to conclusion from computation for astrophysics)

59. CMSO Educational Outreach
Highlight is Wonders of Physics program
Supported by CMSO and DOE (50/50)
Established before CMSO,
expanded in quantity and quality

60. ~ 150 traveling shows/yr
all 72 Wisconsin counties,
plus selected other states
~ 6 campus shows

61. Center Organization

62. Topical Coordinators each pair = 1 lab, 1 astro person
Reconnection Yamada, Zweibel
Momentum transport Craig, Li
Dynamo Cattaneo, Prager
Ion Heating Fiksel, Schnack
Chaos and transport Malyshkin, Terry
Helicity Ji, Kulsrud
Educational outreach Reardon, Sprott

63. CMSO Steering Committee
F. Cattaneo
H. Ji
S. Prager
D. Schnack
C. Sprott
P. Terry
M. Yamada
E. Zweibel
meets weekly by teleconference

64. CMSO Program Advisory Committee
S. Cowley (Chair) UCLA
P. Drake University of Michigan
W. Gekelman UCLA
R. Lin UC - Berkeley
G. Navratil Columbia University
E. Parker University of Chicago
A. Pouquet NCAR, Boulder, CO
D. Ryutov Lawrence Livermore National Lab

65. CMSO International Liaison Committee
M. Berger University College, London, UK
A. Burkert The University of Munich, Germany
K. Kusano Hiroshima University, Japan
P. Martin Consorzio RFX, Padua, Italy
Y. Ono Tokyo University, Japan
M. Velli Universita di Firenze, Italy
N. Weiss Cambridge University, UK

66. CMSO Meetings Sept, 03 Ion heating/chaos (Chicago)
Sept, 03 Reconnection/momentum (Princeton)
Oct, 03 Dynamo (Chicago)
Nov, 03 General meeting (Chicago)
June,04 Hall dynamo and relaxation (Princeton)
Aug, 04 General meeting (Madison)
Sept, 04 PAC meeting (Madison)
Oct, 04 Reconnection (Princeton)
Jan, 05 Video conference of task leaders
March, 05 General meeting (San Diego)
April, 05 Dynamo/helicity meeting (Princeton)
June, 05 Intermittency and turbulence (Madison)
June, 05 Experimental meeting (Madison)
Oct, 05 General meeting (Princeton)
Nov, 05 PAC meeting (Madison)
Jan, 06 Winter school on reconnection (Los Angeles, w/CMPD)
March, 06 Line-tied reconnection (Los Alamos)
June, 06 Workshop on MSO (Aspen, with CMPD))
Aug, 06 General meeting (Chicago)

67. Budget CMSO is a partnership between NSF and DOE
NSF $2.25M/yr for five years
DOE ~$0.4M to PPPL ~$0.1M to LLNL
~$0.15M to UNH
all facility and base program support
LANL ~$0.34M
CMSO is a partnership between NSF and DOE

68. Summary CMSO has enabled many new, cross-disciplinary
physics activities (and been a learning experience)
New linkages have been established
(lab/astro, expt/theory, expt/expt)
Many physics investigations completed, many new starts
The linkages are strong, but still increasing,
the full potential is a longer-term process than 2.5 years