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BEGIN:VEVENT
DTSTAMP:20260308T073033Z
DTSTART;VALUE=DATE-TIME:20250108T150000
DTEND;VALUE=DATE-TIME:20250108T160000
SUMMARY:Andrew Hillier (Exeter): Turbulent mixing layers and cooling the 
 solar corona
TZID:Europe/London
UID:20250108-8ac672c692f555ff01930cbb9a2a5bb1@warwick.ac.uk
CREATED:20241220T135937Z
DESCRIPTION:Abstract: In many astrophysical systems mixing between cool a
 nd hot temperature gas/plasma through Kelvin-Helmholtz instability-drive
 n 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 interacti
 on between either prominence or spicule material and coronal material al
 lowing the development of intermediate temperature material with enhance
 d radiative losses. In this talk\, I will present a set of equations to 
 model the evolution of such a mixing layer based on the self-similar evo
 lution of a turbulent layer and use this to make predictions for the mix
 ing-driven cooling rate and the rate at which mixing can lead to the con
 densation of coronal material. These theoretical predictions are benchma
 rked against 2.5D and 3D MHD simulations (the latter showing the additio
 nal development of the thermal instability). Applying the theoretical mo
 del to prominence threads or fading spicules we found that the mixing wo
 uld lead to the creation of transition region material with a cooling ti
 me of ~100s\, explaining the warm emission observed as prominence thread
 s or spicules fade in cool spectral lines without the requirement for an
 y heating. In fact\, our results imply that the observations of the sola
 r atmosphere that appear to show cool prominence or spicule material bec
 oming warm are likely to be a sign of cooling of the corona and not heat
 ing.
LOCATION:PS1.28
CATEGORIES:CFSA Seminar
LAST-MODIFIED:20241220T135937Z
ORGANIZER;CN=Anne-Marie Broomhall:
END:VEVENT
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