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