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SUMMARY:The magnetic Kelvin-Helmholtz instability\, radiative mixing layer
 s and the cooling of the solar corona - Prof. Andrew Hillier\, University 
 of Exeter
DTSTART:20221017T130000Z
DTEND:20221017T140000Z
UID:TALK182465@talks.cam.ac.uk
CONTACT:Dr Yamini K Rao
DESCRIPTION:In many astrophysical systems mixing between cool and hot temp
 erature gas/plasma through Kelvin-Helmholtz-instability-driven turbulence 
 leads to the formation of an intermediate temperature phase with increased
  radiative losses that drive efficient cooling. The solar atmosphere is a 
 potential site for this process to occur with interaction between either p
 rominence or spicule material and coronal material allowing the developmen
 t of intermediate temperature material with enhanced radiative losses. In 
 this talk\, I will present a set of equations to model the evolution of su
 ch a mixing layer based on the self-similar evolution of a turbulent layer
  and use this to make predictions for the mixing-driven cooling rate and t
 he rate at which mixing can lead to the condensation of coronal material. 
 These theoretical predictions are benchmarked against 2.5D MHD simulations
 . Applying the theoretical model to prominence threads or fading spicules 
 we found that the mixing would lead to the creation of transition region m
 aterial with a cooling time of ∼100s\, explaining the warm emission obse
 rved as prominence threads or spicules fade in cool spectral lines without
  the requirement for any heating. In fact\, our results imply that the obs
 ervations of the solar atmosphere that appear to show cool prominence or s
 picule material becoming warm are likely to be a sign of cooling of the co
 rona and not heating.
LOCATION:In Person MR14
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