University of Cambridge > Talks.cam > DAMTP Astro Lunch > Modelling Ion Populations in Plasmas: the Solar Transition Region

Modelling Ion Populations in Plasmas: the Solar Transition Region

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If you have a question about this talk, please contact Dr William B├ęthune.

Ion abundances for each element in a plasma depend on the interplay of atomic transitions that can take place both within an ion and between neighbouring ions. Knowledge of the ion populations present is fundamental for extracting key plasma parameters, such as temperature, density and elemental abundances, from lines observed in plasma spectra. In high temperature, medium density plasmas, such as the solar corona, modelling can be greatly simplified owing to the plasma conditions present, and predicted ion populations agree well with observations. Further down in the solar atmosphere, in the transition region, higher densities, lower temperatures and the dynamic nature of the plasma mean the simplifications used in the modelling no longer apply. Predicted intensities for some ions can be up to a factor of ten different from observations. Improvements being made to the modelling, using carbon as a test case, will be presented, including new atomic calculations. Predictions made by the new modelling for ion populations will be compared to the existing model, and a preliminary comparison with observations given.

This talk is part of the DAMTP Astro Lunch series.

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