Tentative program
Week 1: 2529 July
Monday, 25 July
9:0012:00 Registration, computer setup
14:0016:00 Discussion of the program agenda
and presentation plan
16:0017:00 Welcome reception
Tuesday, 2629 July
Program Topic: "Numerical simulations and meanfield theory"
 Recent results of numerical dynamo simulations
 Effects of magnetic helicity and crosshelicity
 Models of turbulent diffusivity and magnetic pumping
 Progress in meanfield dynamo models
 Links between numerical simulations and meanfields models
Tuesday, July 26, 9:30  12:00 (coffee break 10:3011:00)
 Effects of magnetic helicity and crosshelicity
A. Brandenburg, V. Pipin, D. Sokoloff, K. Kuzanyan, N. Yokoi
Wednesday, July 27, 9:30  12:00 (coffee break 10:3011:00)
 Crosshelicity, models of turbulent diffusivity and magnetic pumping
N.Yokoi, Crosshelicity modeling (cont.)
I. Rogachevskii, Models of turbulent pumping
N. Kleeorin, Compressibility effects in turbulent pumping and diffusivity
Thursday, July 28, 9:30  12:00 (coffee break 10:3011:00)
 Meanfield dynamo models
V. Pipin, Surfaceshear dynamo model
G. Guerrero, Fluxtransport solar dynamo models, advantages and issues
Friday, July 29, 9:30  12:00 (coffee break 10:3011:00)
 Meanfield dynamo theory and observations
K. Kuzanyan, Review of observations of crosshelicity
A. Bonanno, Dynamo model with meridional flow with deep stagnation point
Week 2: 15 August
"Advances in dynamo theory"
Monday, August 1
 Turbulence models in dynamo theory
A. Brandenburg, Introduction to tauapproximation
K.H. Raedler, Comments on tau and smoothing approximations
I. Rogachevskii, Comparison of tau approximation with others analytical approaches
Tuesday, August 2
 Dynamical models and dynamo
M.Reshetnyak, Break of symmetry in Parker's dynamo
N. Kleeorin, How to calculate the integral of motion, and Kolmogorov theory in the contents of dynamo theory
Wednesday, August 3
 Recent results of numerical dynamo simulations
R. Simitev, Convectivedriven dynamo and applications to the Sun
F. Busse, Applications of thinshell models to the Sun
P. Kapyla, Stratified convective dynamos in a spherical shell
A. Brandenburg, Low Prandtl number simulations
Thursday, August 4
 Oscillatory and chaotic regimes
D. Mitra, Kinematic dynamos with shear and fluctuating alpha effect
Xing Wei, Kinematic dynamo action in spherical Couette flow
Friday, August 5
 Subgrid scale models
N. Mansour, SGS MHD LES models
N.Yokoi, Incorporation of helicity effects in subgrid scale models
Week 3: 812 August
Program Topic: "Astrophysical Dynamos"
Monday, August 8
Individual project and collaborations
Tuesday, August 9
A. Bobrick, Mass transfer in white dwarfcompact object binaries
R. Arlt, Angularmomentum removal through stellar radiation zones
Wednesday, August 10
D. Sokoloff, Simple model for geodynamo reversals
M.Reshetnyak, Compressibility and Kinetic Helicity Generation in Geodynamo
Thursday, August 11
K. Kuzanyan, Observable statistical properties of current helicity distribution in
solar active regions as manifestation of multiscale nature of solar
turbulence
D. Sokoloff, Cluster analysis of the butterfly diagram
Friday, August 12
A. Bonanno, Stellar dynamo
D. Sokoloff, Polar branches of stellar activity waves: dynamo models
Sharanya Sur, Galactic dynamo
Week 4: 1518 August
Program Topic: "Dynamo, Magnetic SelfOrganization and Links to Observations"
Monday, 15 August
Joern Warnecke, Coronal mass ejections driven by dynamo action underneath the solar surface
Fabio Del Sordo, The generation of vorticity through irrotational forcing
Tuesday, 16 August
Elisabete M. de Gouveia Dal Pino, Magnetic Flux Transport in turbulent Astrophysical environments: the role of Magnetic Reconnection
Phil Goode, Strange solar cycles
11:00 Nordita seminar: Irina Kitiashvili, Multiscale dynamics of the Sun
Wednesday, 17 August
Jan Stenflo, Bipolar magnetic regions on the Sun: Global analysis of the SOHO/MDI data set
Alexander Kosovichev, Helioseismology and magnetic field observations from SDO
Maarit Mantere, New interpretation of starspots
1:30pm Seminar: Irina Kitiashvili, Realistic simulations of solar magnetoconvection
3:30pm GĂ¶ran Scharmer, Observations of the Evershed effects
Thursday, 18 August
Phil Goode, New solar observational results that support local dynamos
Jan Stenflo, Collapsed, uncollapsed, and hidden magnetic flux on the quiet Sun
Vincent Duez, Relaxation in rotating stellar radiation zones
Simon Candelaresi, Magnetic helicity, topological interpretation, relaxation and transport
3:30pm  Jan Snellman, 1D models of Boussinesq convection
Afternoon tea topics:
Nobumitsu Yokoi, Comments on solar wind turbulence
Nobumitsu Yokoi, Magnetic reconnection
Axel Brandenburg, Solar winds results
19 August
9:00  12:00 Final reports by participants
 Concluding remarks, future plans
Understanding the origin of solar and stellar magnetic field is one
of the central problems of physics and astrophysics, and a key to
understanding the cosmic magnetism, in general. There are two main
difficulties in studying this problem: 1) magnetic fields are generated
by turbulent dynamos in convection zones below the visible surface,
not accessible by direct observations; 2) solar and stellar magnetic
activity is a multiscale phenomenon, involving physical processes on
very small scales, probably, below the current observational limit,
and at the same time showing remarkable largescale spatial and temporal
organizations over a whole star. The prime target of our investigation
is the Sun, which serves as the Rosetta Stone in this field and holds
the key to unlocking the secrets of magnetic field generation in the
Universe. The most detailed observational data and theoretical models
have been obtained for the Sun, but also a very significant progress
has been in observations and theories of magnetism on other stars.
Observationally, most efforts for solving the problem of solar and stellar
magnetism are focused on developing helio and asteroseismology for
probing the structure and dynamics inside the Sun and stars and detecting
changes associated with magnetic fields, on highresolution observations
for probing smallscale and even unresolved magnetic structures and
their organization and evolution, and on studying largescale patterns
of sunspots and starspots and magnetic activity cycles.
Theoretically, this problem is addressed by developing physical models
at three different levels of the spatial and temporal domain: 1) direct
3D MHD simulations of small volumes of the convection zone with the
highest possible resolution (local dynamo); 2) 2D and, more recently,
3D meanfield theories of the global dynamo on the scale of the activity
cycle, based on turbulent sources and transport models; 3) simple 1D
nonlinear dynamical models to investigate longterm evolution of the
dynamo. These approaches have been developed independently and quite
successfully by different groups.
Registration deadline: 20 June 2011
Deadline for accommodation: 20 May 2011
