1 / 15

Shocks!

Shocks!. David Burgess Astronomy Unit Queen Mary, University of London. This presentation was given at: Workshop on Solar Kinetics and MHD, 25-27 Feb 2008, RAL Cosener's House, Abingdon, UK. This is not a comprehensive tutorial about collisionless shocks in the solar context.

mason-carney
Download Presentation

Shocks!

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. Shocks! David BurgessAstronomy UnitQueen Mary, University of London

  2. This presentation was given at: Workshop on Solar Kinetics and MHD, 25-27 Feb 2008, RAL Cosener's House, Abingdon, UK. This is not a comprehensive tutorial about collisionless shocks in the solar context. The aim is only to give an indication of some current areas of interest in shock research, and in particular to draw attention to some areas and questions that could be interesting to pursue further in the context of the solar atmosphere and corona.

  3. Shocks: • Converting flow to thermal energy Without collisions … • All the important physics is kinetic • Particle reflection • Instabilities • Particle acceleration

  4. What parameters are important? • Shock normal angle : quasi-parallel versus quasi-perpendicular • Mach Number • Plasma beta • Simulation method (hybrid, PIC, etc) • Mass ratio • Dimensionality

  5. Some Topics … • Electron acceleration • Nonstationarity • Turbulence

  6. Electron Acceleration at Qperp • Fast Fermi by mirror reflection • Highest energies (but lowest efficiency) at close to perpendicular

  7. Effect of including structure • Test particle electrons in fields from 2D hybrid simulation • Structure: power law energy spectra up and downstream

  8. Nonstationarity at Qperp Shocks • Hybrid: nonstationary at low enough  • PIC: overturning via over-reflection of ions • Effect controlled by  and mass ratio used in simulations …

  9. Nonstationarity at Qperp Shocks • With realistic mass ratio foot dynamics controlled by electromagnetic two stream instability • With implications for (eg) shock surfing acceleration

  10. Nonstationarity at Oblique Shocks • PIC simulations • Away from perpendicular, standing whistler can dominate structure • Nonstationarity via competition of different mechanisms

  11. Kinetic Effects in Turbulence • Kinetics and the “dissipation” scale • What is the “energy cascade” at kinetic scales? • What happens with multiple kinetic scales? • Control of temperature and temperature anisotropy with linear instabilities

  12. Shocks in the Corona Flares …

  13. Solar shocks continued … CME

  14. More solar shocks?

  15. Dynamic Fibrils - Simulations

More Related