Testing the Physics of Solar Flares with NASA’s Solar Dynamics Observatory and Radiative MHD Simulations

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• Mark Cheung ( Lockheed Martin Solar & Astrophysics Laboratory & Stanford University)
• Monday 16 April 2018, 14:00-15:00
• MR14, Centre for Mathematical Sciences, Wilberforce Road, Cambridge.

If you have a question about this talk, please contact Dr. Yufeng Lin.

In part one of this talk, we show how extreme UV images of the solar corona taken by NASA ’s Solar Dynamics Observatory can be used to quantify the thermal structure and evolution of magnetically active regions on the Sun. The thermal structures inferred from extreme UV observations 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 of 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, including the time profile of the X-ray flux, chromospheric evaporation and condensation, the sweeping of flare ribbons in the lower atmosphere, global coronal waves, and the non-thermal spectral shape of coronal X-ray sources. Implications for how we interpret X-ray spectra from other astrophysical sources will be discussed.

This talk is part of the DAMTP Astrophysics Seminars series.

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