University of Cambridge > > DAMTP Astrophysics Seminars > Understanding Solar Coronal EUV and X-Ray Emission: Comparing MHD

Understanding Solar Coronal EUV and X-Ray Emission: Comparing MHD

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If you have a question about this talk, please contact Laurène Jouve.

Observations of the solar corona have come a long way in the last couple of decades: emission images of the EUV and X-ray corona are now routinely available (e.g., from Hinode EIS and XRT , STEREO/EUVI, SOHO / EIT , Yohkoh SXT ). At the same time, magnetohydrodynamic (MHD) computations of the corona have advanced considerably: it is now possible to simulate emission in the global corona and active regions. This confluence provides unique opportunities to test models versus observations, to achieve a deeper understanding of the properties of the corona, and in particular, to constrain the largely unknown mechanism of coronal heating. We will describe how we compare an MHD model with observations, the limitations of the approach, and what future prospects exist.

This talk is part of the DAMTP Astrophysics Seminars series.

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