Funding from: BOF, Odysseus & GOA (KU Leuven), EC-FP7 (Soteria, www.soteria-space.eu)
Giovanni Lapenta, Lapo BettariniCentrum voor Plasma-Astrofysica - Katholieke Universiteit Leuven (Belgium)
with help from Tibor Torok
SOTERIA Initiation Challenge
Report Deliverable 3.3
Report Deliverable 3.3
We propose for us and to the community a CME/flare initiation challenge and benchmark
How different physics and resolution affects the evolution
Steps taken for starting the challenge
CME/Flare start model
Compare different models:
•Ideal MHD•Resistive MHD•Different resitivities•Zero beta MHD•Two fluid and kinetic
Useful benchmark for different codes now and in the future
Where and how reconnection develops
How fast does the prominence raise
Tajima, Shibata, Plasma Astrophysics
Goals of the challenge
FLIP3D-MHD AMR-VAC PLUTO ECHO
90’s - now 90’s - now 2005 - now 2005 - now
Brackbill - Lapenta
Toth - Keppens
University of Turin
University of Florence
Fluid Physics Simulations
Two suggestions for the challenge
Fan & GibsonApJ 609, 1123, 2004
Birn et alApJ 645, 732, 2006
10:09:30 AM
CHALLENGE 1Modified from
Fan & Gibson, ApJ 609, 1123, 2004
We start from the flux rope already emerged, avoiding difficulties with emergence
Not in equilibrium
Expansion against the overarlying arcade
Specific choice of arcade and of rope
Approach from Fan&Gibson, ApJ 609, 1123, 2004
is the distance from the rope (poloidal radius, if ropes is a torus)
Model: equations
10:09:30 AM
Typical evolution (FLIP3D-MHD)
10:09:30 AM
CHALLENGE 2Modified from
Birn et al, ApJ 645, 732, 2006
Twisted flux ropes embedded in a helmet streamer type
configuration
Connected to the photosphere and anchored to the corona by an
overlying arcade
Approximate equilibrium
Specific choice of the degree of twist and amount of plasma
pressure
Approach from Birn et al, ApJ 645, 732, 2006
Model: equations
• f = 0.2 nearly force-free flux rope with a strong shear field B
• ε = 1 the initial states are not exactly force-balanced. The maximum forces in the vertical direction were found to be approximately 0.1 (normalized by characteristic values of current density and magnetic field)
Model: features
Typical evolution (PLUTO)
2 oral sessions
1 poster session
Session at AGU Meeting in San Francisco
10:09:30 AM
http://exascience.com/
Several positions available
INTEL ExaScience Lab in Leuven
June 8, 2010New Lab to Develop Solar Flare
Prediction as Driver for Intel’s Future Exascale
Supercomputers
(Intel, imec and Five Flemish Universities)
Task 4: Space weather model validation and forcasting (Hvar, ROB, KFKI, UOulu, KUL, DTU)
Based on the results of Tasks 1-3 we will improve existing capability and develop new methods for space weather forcasting, including:
•Prediction of arrival time of interplanetary CMEs at the Earth (Hvar)
•Prediction of geomagnetic disturbances associated with high-speed streams from coronal holes (Hvar)
•Validation of the Solar Particle Engineering Code (SOLPENCO) for extreme events (KFKI)
•Model validation and prediction of near-Earth solar wind disturbances associated with ICMEs and high speed solar wind streams (KUL, Hvar) and their geo-effectiveness (DTU, UOulu, KFKI, ROB)
•Short-term prediction of the magnetic storms and the time development of the improved Dst (UOulu, ROB)
•Long-term forcasting of coronal hole and solar activity centre occurrence (UOulu)
•Prediction of scintillations (IEEA)
Deliverable 4.5 (next year)
New FP7 project on space weather modelling: SWIFF
