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Title: Combining observations and 3D numerical simulations for solar
flare modelling<br>
Speaker: Miho Janvier (Institut d'Astrophysique Spatiale, Paris)<br>
<br>
Friday 27th of October from 10:30 to 11:30 at FC61.<br>
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Abstract:<br>
<div style="margin: 0px; line-height: normal;" class="">Solar flares
are the most energetic events taking place in our solar system.
They result from the conversion of magnetic energy stored in the
Sun’s atmosphere into energetic particles, heat, and in some cases
into the launch of solar storms (or Coronal Mass Ejections - CMEs)
in interplanetary space. Solar flares and CMEs are at the origin
of space weather events: on Earth, they lead to geomagnetic storms
and can be responsible for disruptions of satellite systems, as
well as electricity transport on large-scale national power grids.
Auroras, atmospheric ion losses, and other effects of space
weather also take place on other planets in the solar system.
Therefore, <span style="font-kerning: none" class="">understanding
the underlying mechanisms of solar flares is of primary
importance to better predict their evolution and influence on
nearby planets.</span></div>
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class=""></span><br class="">
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<div style="margin: 0px; line-height: normal;" class=""><span
style="font-kerning: none" class="">Increased temporal and
spatial resolutions of ground and space observatories have
allowed us to refine a standard model for eruptive flares, which
can explain their generic features (the presence of flare
ribbons, flare loops and a twisted erupting magnetic structure).
In particular, 3D MHD modelling has provided us with some
predictions on the magnetic field behaviour during the eruption,
such as the evolution of regions where the magnetic field energy
is converted. These predictions are nowadays well documented
with the help of observations with, e.g., the AIA and HMI
instruments aboard the NASA mission Solar Dynamics Observatory.</span></div>
<div style="margin: 0px; line-height: normal; min-height: 14px;"
class=""><span style="font-kerning: none" class=""></span><br
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<div style="margin: 0px; line-height: normal;" class=""><span
style="font-kerning: none" class="">We will look at how these
predictions can be validated with a careful study of the active
region configuration with different techniques, whether with
dynamic (MHD) or static (also known as magnetic field
extrapolations) numerical models. This will show how approaches
combining different modelling techniques and observations
provide a major step in extending and completing the standard
model for eruptive flares in its 3D version.</span></div>
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