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SUMMARY:Global MHD simulations of ejections of magnetic flux ropes - Dr. P
 aolo Pagano
DTSTART:20151102T160000Z
DTEND:20151102T170000Z
UID:TALK61830@talks.cam.ac.uk
CONTACT:Andrew Hillier
DESCRIPTION:Magnetic flux ropes ejections are considered a progenitor of C
 oronal Mass Ejections (CMEs) from the Solar Corona and their occurrence us
 ually follows a long lasting equilibrium in the solar corona. Magnetic flu
 x ropes form in the solar corona due to the evolution the coronal magnetic
  field driven by photospheric motions and flux emergence events and when m
 agnetic flux ropes become unstable their ejection may turn into a CME rele
 asing plasma and magnetic flux into the interplanetary space. Although sta
 te of the art simulations can explain flux rope ejections\, to perform the
 se studies from realistic configurations merged into the global corona is 
 key to shed light on still standing questions: what is the impact of a flu
 x rope ejection on the global configuration of the corona? Can a single ej
 ection accelerate or trigger ejections in different locations?\nHowever th
 e size of the full coronal domain and the different time scales involved p
 ose considerable challenges. To this end we couple the Global Non-Linear F
 orce-Free Field (GNLFFF) model applied to observed magnetograms to 3D MHD 
 simulations of the global corona. The GNLFFF is tailored to describe the s
 low magnetic evolution of the corona that leads to a flux rope formation\,
  while the MPI-AMRVAC software is a numerical MHD model that keeps a gener
 al approach and can effectively model a fast flux rope ejection. We will p
 resent our model and its potential in the Space Weather forecast context.
LOCATION:MR14\,  Centre for Mathematical Sciences\, Wilberforce Road\, Cam
 bridge
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