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SUMMARY:Cooling the solar atmosphere with shocks - Ben Snow (Exeter)
DTSTART:20260302T160000Z
DTEND:20260302T170000Z
UID:TALK242473@talks.cam.ac.uk
CONTACT:Roger Dufresne
DESCRIPTION:Whilst the solar surface is a few thousand degrees\, the solar
  corona (~2Mm further out than the surface) is roughly a million degrees. 
 This has formed one of the greatest challenges in the solar physics\, usua
 lly referred to as the coronal heating problem: how is the million-degree 
 corona obtained and maintained against radiation. The last 70 years of sol
 ar research has focussed heavily on understanding heating mechanisms in an
  effort to solve the coronal heating problem. However\, my research has sh
 own that mechanisms often studied in the context of heating\, such as shoc
 ks\, may actually be cooling the solar plasma. Here I present results on r
 adiative shocks and present analytical and numerical evidence of temperatu
 re-reducing shocks occurring under coronal conditions. The turbulent numer
 ical simulation allows statistics of shocks to extracted\, with roughly 40
 % of shocks having a net reduction in temperature. As such\, the role of s
 hocks in heating/cooling the solar atmosphere is an open question.
LOCATION:MR14 DAMTP and online
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