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SUMMARY:Testing the Physics of Solar Flares with NASA’s Solar Dynamics O
 bservatory and Radiative MHD Simulations - Mark Cheung ( Lockheed Martin S
 olar &amp\; Astrophysics Laboratory &amp\; Stanford University)
DTSTART:20180416T130000Z
DTEND:20180416T140000Z
UID:TALK102784@talks.cam.ac.uk
CONTACT:Dr. Yufeng Lin
DESCRIPTION:In part one of this talk\, we show how extreme UV images of th
 e solar corona taken by NASA’s Solar Dynamics Observatory can be used to
  quantify the thermal structure and evolution of magnetically active regio
 ns on the Sun. The thermal structures inferred from extreme UV observation
 s are consistent with their soft X-ray counterparts. Lessons learned from 
 such studies guide the development of models of solar flares and eruptions
 . In the second part of this talk\, we present radiative MHD simulations o
 f flares and eruptions with sufficient realism for the synthesis of remote
  sensing measurements at visible\, UV and X-ray wavelengths. These models 
 allow us to explain a number of well-known observational features\, includ
 ing the time profile of the X-ray flux\, chromospheric evaporation and con
 densation\, the sweeping of flare ribbons in the lower atmosphere\, global
  coronal waves\, and the non-thermal spectral shape of coronal X-ray sourc
 es. Implications for how we interpret X-ray spectra from other astrophysic
 al sources will be discussed.
LOCATION:MR14\,  Centre for Mathematical Sciences\, Wilberforce Road\, Cam
 bridge
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