EIS Science Goals: The First Three Months….

1. EIS Science Goals: The First Three Months…. Louise Harra Mullard Space Science Laboratory University College London

2. SCIENCE GOALS • Coronal heating - to determine the physical mechanisms responsible for coronal heating in the quiet Sun and active regions (e.g. detect magnetic reconnection, wave heating). • Transient Phenomena - to determine the physical mechanisms responsible for transient phenomena, such as solar flares, coronal mass ejections, jets, network brightenings (e.g. determine energy transport and mass motions during transient events). • Energy Transfer from the photosphere to the corona -to investigate the causal relationship between dynamics in the photosphere and coronal phenomena.

3. Extreme-Ultraviolet Imaging Spectrometer (EIS) • EIS Records Solar Extreme-Ultraviolet (EUV) Spectra That Contain Information on the Dynamics, Velocity, Temperature, and Density of the Emitting Plasma • Spectra Are Obtained With High Spatial Resolution • Spectra at Many Locations Within an Entire Solar Structure Can Be Recorded • Spectra Are Obtained With Sufficient Time Resolution to Determine the Dynamics As a Function of Position Within Solar Flare and Active Region Loops • EIS Is the First EUV Solar Spectrometer Capable of Obtaining High Spectral Resolution Data With Both High Spatial and Temporal Resolution

4. EIS Science Planning Guide • We are developing this on our web site www.mssl.ucl.ac.uk/espg.html • Includes an EIS study form in order to ‘play’ with your own personal observing plans. • Includes a list of EIS studies produced by the EIS team • Includes line lists and intensities in different regions of activity • Includes a set of science data products • Includes an initial science plan for the first 3 months

5. The first 3 months…. • Flare trigger and dynamics: the first spatial determination of evaporation and turbulence in a flare • Active region heating:the first spatial determination of the velocity field in active region loops • Coronal Mass Ejection Onset:first spatial velocity and dimming measurement at high temporal resolution • Coronal Hole Boundaries:the first measurement of intensity and velocity field at the coronal hole boundary • Quiet Sun Brightenings:first determination of the relationship between different categories of quiet Sun events.

6. Flare Trigger/Dynamics Evaporation - We know it’s happening, but where from and what size?

7. Flare Trigger/Dynamics Inflow: we’ve seen it once! But is it happening all the time?

8. Flare Trigger/Dynamics What causes a flare? We have many tantalizing hints - EIS will provide spatial resolved preflare Vnt & flow measurements. TRACE 1600+ CDS OV TRACE 195 + RHESSI 6-12keV

9. Active Region Heating What causes loop heating and dynamics? Accurate line width and Doppler velocity measurements over a range of velocities will provide critical information.

10. Coronal Mass Ejection Onset We need to know the velocity and dimming profiles over a range of temperatures to begin to understand the CME onset (see Harra & Sterling, 2001)

11. Coronal Mass Ejection Onset Coronal waves are often seen related to CMEs - what are the physical characteristics of these waves? CDS data is showing some tantalizing hints…. See Harra & Sterling 2003

12. Coronal Hole Boundaries The CH boundaries are not well understood - we will be able to determine the velocity field at this important region.

13. Quiet Sun Events Are explosive events and blinkers the same phenomena? We will be able to measure velocities at good spatial resolution…. OV 45,000km 7,500 km

14. Conclusions • I have concentrated on what EIS can do for us in the first few months - combining these observations with SOT and XRT will provide new and exciting science. • We intend to track targets for long periods of time (at least a day on each target). • If there is an active region we will track it. If not we will carry out the CME onset on filaments, QS and CH studies.