EIS Core Science Programme

• Active Regions:
  
  1. connect the photospheric velocity field to signatures of coronal heating observed in the corona. This will be carried out on other coronal brightenings, such as bright points.
  2. search for evidence of waves and loop oscillations in loops. Use EIS observations for coronal seismology.
  3. study dynamic phenomena within active region loops. Discriminate between siphon flows, bi-directional flows and turbulence.


• Quiet Sun:
  
  1. link quiet Sun brightenings and explosive events to the magnetic field changes in the network and inter-network to understand the origin of these events. We will search for responses to small changes in the photospheric magnetic and velocity fields.
  2. determine the variation of explosive events and blinkers with temperature.
  3. search for evidence of reconnection and flows at junctions between open and closed magnetic field at coronal hole boundaries.
  4. determine the impact of quiet Sun events on larger scale structures within the corona.
  5. determine physical size scales with generally diffuse quiet Sun coronal plasmas using densiyt diagnostics.


• Solar flares:
  
  1. determine the source and location of flaring and identify the source of energy for flares. EIS will measure the velocity fields and observe coronal structures with temperature information. This information will help us address the flare trigger mechanism.
  2. detection of reconnection inflows, outflows and the associated turbulence which play the pivotal role in flare particle acceleration.


• Coronal Mass Ejections:
  
  1. determine the location of dimming (and the subsequent velocities) in various magnetic configurations. We will determine the magnetic environment that leads to a coronal mass ejection and measure the low altitude component of the coronal mass ejection mass budget.
  2. The situations to be studied include filaments, flaring active regions and trans-equatorial loops.


• Large Scale Structures:
  
  1. determine the temperature and velocity structure in a coronal streamer.
  2. determine the velocity field and temperature change of a trans-equatorial loop, and search for evidence of large-scale reconnection.
  3. using a low latitude coronal hole, search for the source of the fast solar wind.

Last Revised: Monday, 24-Jul-2006

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