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SUMMARY:Heating and cooling of multistranded solar coronal loops - Stépha
 ne Régnier (University of Central Lancashire)
DTSTART:20120529T120000Z
DTEND:20120529T130000Z
UID:TALK37624@talks.cam.ac.uk
CONTACT:Jérôme Guilet
DESCRIPTION:One big puzzle in Solar Physics is why coronal loops tracing t
 he magnetic field lines are observed in EUV emission? In other words\, wha
 t is the thermodynamic\nevolution of coronal loops? To tackle this issue\,
  we use a 1D hydrodynamic model describing a loop as an amalgamation of st
 rands evolving independently.\nThe energy input is prescribed by the Parke
 r model of nanoflare heating: discrete distribution of short bursts releas
 ing energy (about 10^24 erg) along\nthe loop. We first show that the model
  can reproduce the main observed features\, especially focusing on the ubi
 quitous existence of blue-shifts in spectral\nobservations. The modelled D
 oppler-shifts are a consequence of condensation at the foot-points of the 
 loop inducing cool plasma moving downwards\, and of\nevaporation generatin
 g outflows of hot material. The second step is to study the cooling of a p
 reviously heated loop\, and to answer the following questions: what is the
  characteristic time-scale of cooling? what are the signatures of cooling 
 in different pass-bands?
LOCATION:MR14\,  Centre for Mathematical Sciences\, Wilberforce Road\, Cam
 bridge
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