Transcript Giovanni Lapenta, L. Bettarini, M. Skender Centrum voor

SOTERIA Initiation
Challenge
Giovanni Lapenta, Lapo Bettarini
Centrum voor Plasma-Astrofysica - Katholieke Universiteit Leuven (Belgium)
with help from Tibor Torok
Funding from: BOF, Odysseus & GOA (KU Leuven), EC-FP7 (Soteria, www.soteria-space.eu)
Report Deliverable 3.3
Report Deliverable 3.3
Steps taken for starting the challenge
We propose for us and to the community a CME/flare initiation
challenge and benchmark
How different physics and resolution affects the evolution
CME/Flare start model
Goals of the challenge
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
Fluid Physics Simulations
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
Two suggestions for the challenge
Fan & Gibson
ApJ 609, 1123, 2004
Birn et al
ApJ 645, 732, 2006
10:09:30 AM
CHALLENGE 1
Modified from
Fan & Gibson, ApJ 609, 1123, 2004
Approach from Fan&Gibson, ApJ 609, 1123, 2004
We start from the flux rope already emerged,
avoiding difficulties with emergence
Specific choice of arcade and of rope
Expansion against the overarlying arcade
Not in equilibrium
Model: equations
is the distance from the rope (poloidal radius, if ropes is a torus)
Typical evolution (FLIP3D-MHD)
10:09:30 AM
10:09:30 AM
CHALLENGE 2
Modified from
Birn et al, ApJ 645, 732, 2006
Approach 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
Specific choice of the degree of twist and
amount of plasma pressure
Approximate equilibrium
Model: equations
Model: features
•
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)
Typical evolution (PLUTO)
Session at AGU Meeting in San Francisco
2 oral
sessions
1 poster
session
INTEL ExaScience Lab in Leuven
10:09:30 AM
June 8, 2010
New Lab to Develop Solar Flare
Prediction as Driver for Intel’s Future
Exascale Supercomputers
(Intel, imec and Five Flemish Universities)
http://exascience.com/
Several positions available
Deliverable 4.5 (next year)
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)
New FP7 project on space weather modelling: SWIFF