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MHD modeling of coronal disturbances related to CME lift-off J. Pomoell 1, R. Vainio 1, S. Pohjolainen 2 1 Department of Physics, University of Helsinki.

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Presentation on theme: "MHD modeling of coronal disturbances related to CME lift-off J. Pomoell 1, R. Vainio 1, S. Pohjolainen 2 1 Department of Physics, University of Helsinki."— Presentation transcript:

1 MHD modeling of coronal disturbances related to CME lift-off J. Pomoell 1, R. Vainio 1, S. Pohjolainen 2 1 Department of Physics, University of Helsinki 2 Tuorla Observatory, University of Turku

2 Introduction Solar flares and coronal mass ejections (CMEs) capable of launching global large-amplitude coronal disturbances and shocks Observed directly in Hα (Moreton waves), EUV (EIT waves), soft X-rays, He I and radio Play a role in the acceleration of electrons and ions to high energies, exact mechanisms unclear Observed in-situ and as various EM signatures STEREO AHEAD EUVI 195 Å May 19, 2007

3 Type II radio bursts Plasma emission (F+H) caused by shock-accelerated e -, knowing gives

4 Questions & Aims Current consensus: Interplanetary type IIs generated by CME driven shocks. But what about coronal type IIs, generated by blast waves (flares) or driven waves (CMEs)? What about high-frequency type IIs? (Pohjolainen, Pomoell, Vainio: A&A 490, 2008) We address such issues by performing MHD simulations of CME lift-off Look for features that might be of importance when interpreting observations or ?

5 MHD Model 2D model, gravitationally stratified corona including a dense loop Superimpose flux rope structure with higher density Alfvén speed increases in the higher corona, low in the loop

6 Eruption dynamics When the flux rope starts to rise, a perturbation is formed around the flux rope, and steepens to a shock Below the loop, the shock remains weak, but strengthens and slows down quickly when entering the loop As the flux rope decelerates, the displaced loop and shock escape from the driver The shock escapes quickly after exiting the loop Density Speed

7 Dynamic spectrum Assuming radio type II emission is produced at the leading edge of the shock, we plot frequency vs. time Qualitative similarities

8 Driven or blast wave? In a simulation without dense loops, the shock also escapes from the flux rope The skirt of the shock sweeps the solar surface followed by another wave EIT waves? Density Temperature

9 Summary of results Depending on the variations of the Alfvén speed in the low corona, the erupting CME can at times acts as the driver of the shock, while at other times the shock may propagate freely Difficult to determine whether coronal waves caused by flare or CME, low-cadence observations may be misleading Correlation between speed and location of type II bursts and ejecta can be very complex Possible that fragmented, high-frequency type IIs due to CME driven shocks propagating through dense coronal loops

10 Conclusion By performing numerical simulations side by side with analysis of observations, the physics involved in the coronal phenomena can more readily be extracted than by solely analyzing the observational data All approaches needed in order to understand these dynamical processes


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