1. Spectroscopic Observations with SolarB-EIS Helen E. Mason DAMTP, Centre for Mathematical Sciences Giulio Del Zanna, MSSL

2. Solar-B Spacecraft EIS - MSSL/NRL EUV Imaging Spectrometer SOT - ISAS/NAOJ Solar Optical Telescope XRT - SAO/ISAS X-ray Telescope FPP - Lockheed/NAOJ Focal Plane Package

3. Mission Characteristics Launch date: September 2006 Launch vehicle: ISAS MV Mission lifetime: 3 years Orbit: Polar, sun synchronous Inclination: 97.9 degrees Altitude: 600 km. Mass: 900 kg

4. EIS Design The EIS telescope is an off-axis paraboloid design, with focal length 1.9m and mirror diameter 150mm. EIS has a total length of 3m. Multilayer toroidal gratings disperse the spectrum onto 2 detectors covering 40A each - 170-210A, 240-290 A Angular resolution: 2". Four slit/slot positions are available - 1", 2", 40“, 266". Spectral/Velocity resolution: 3km/s for Doppler velocities, 20km/s for line widths Temporal resolution: In spectrosocopy mode: < 1s in dynamic events ~ 10s in active regions

5. Slit Exchange Mechanism Primary Mirror Entrance Filter Concave Grating Filter CCDs Shutter 1939 mm 1440 mm 1000 mm EIS Optical Diagram Grating Front Baffle Entrance Filter Primary Mirror CCD Camera

6. EIS Field-of-View (FOV) 360  512  EIS Slit Maximum FOV for raster observation 512  900  Raster-scan range Shift of FOV center with coarse-mirror motion 250  slot 40  slot 512 

7. Four slit/slot selections available EUV line spectroscopy - Slits - 1 arcsec  512 arcsec slit - best spectral resolution - 2 arcsec  512 arcsec slit - higher throughput EUV Imaging – Slots –Overlappogram; velocity information overlapped –40 arcsec  512 arcsec slot - imaging with little overlap –250 arcsec  512 arcsec slot - detecting transient events Slit and Slot Interchange

8. Observables 1 Observation of single lines –Line intensity and profile –Line shift (  ) → Doppler motion –Line width (  w) and temperature → Nonthermal motion  ww

9. CDS observations of a spray ejecta from an X2 flare – Pike and Mason, 2002, Sol.Phys., 206, 359 Outward speed 700km/s Rotational vel +/-350km/s

10. Source Regions of the High Speed Solar Wind Hassler, Mason et al (1999) Science SUMER spectroscopic observations in a coronal hole in Ne VIII 770Å (650 000 K) Shows outflows (blue shifts) in coronal hole as compared to red shifts in quiet Sun Largest outflows occur along the boundaries and the intersections of the chromospheric network (superimposed dark lanes) –“solar wind breaking through network like grass around the edges of paving stones in a patio” Observations with SUMER (UV Spectrometer) Dopplergram showing the up- and downflows

11. CDS – FeXIX line,10MK

13. Blue shifted SiXII (74km/s) and FeXIX (140km/s) emission

14. Non-Gaussian profiles Two component emission line profiles:  HRTS: Dere & Mason (1993)

15. EIS - expected Accuracy of Velocity Doppler velocity Line width Bright AR line Flare line Photons (1  1  area) -1 sec -1 Photons (1  1  area) -1 (10sec) -1 Number of detected photons

16. Observables 2 Observation of line pair ratios –Temperature –Density – for example –Fe XIII 203.8/202.0 diagnostic

17. CDS - Electron Density and Temperature Structure of a limb active region - Mason et al, 1999, Sol.Phys., 189, 129

18. Observables 3 Observation of multiple lines –Differential emission measure

19. Joint CDS and TRACE Data for 2 nd May 1998

27. EIS Sensitivity IonWavelength (A) logTN photons ARM2-Flare Fe X184.546.001536 Fe XII186.85 / 186.886.1113/21105/130 Fe XXI187.897.00-346 Fe XI188.23 / 188.306.1141 / 15110/47 Fe XXIV192.047.30- 4.0  10 4 Fe XII192.396.1146120 Ca XVII192.826.7031 1.8  10 3 Fe XII193.526.11135305 Fe XII195.12 / 195.136.11241/16538/133 Fe XIII200.026.2020113 Fe XIII202.046.203582 Fe XIII203.80 / 203.836.207/2038/114 Detected photons per 1  1  area of the sun per 1 sec exposure. IonWavelength (A) logTN photons ARM2-Flare Fe XVI251.076.40-108 Fe XXII253.167.11-71 Fe XVII254.876.60-109 Fe XXVI255.107.30- 3.3  10 3 He II256.324.7016 3.6  10 3 Si X258.376.111462 Fe XVI262.986.4015437 Fe XXIII263.767.20- 1.2  10 3 Fe XIV264.786.3020217 Fe XIV270.516.3017104 Fe XIV274.206.301476 Fe XV284.166.35111 1.5  10 3 AR: active region

28. EIS – Electron Density Sensitive Line Ratios (Del Zanna and Mason, 2005)

29. EIS Initial Science Plan Core line list, to be: HeII 256, FeXII 195, CaXVII 193 Quiet Sun brightenings Active region heating Flare trigger/dynamics Coronal Mass Ejection Onset Coronal Hole Boundaries

30. EIS Processed Science Data Products Intensity Maps (T e, n e ):Intensity Maps (T e, n e ): – images of region being rastered from the zeroth moments of strongest spectral lines Doppler Shift Maps (Bulk Velocity):Doppler Shift Maps (Bulk Velocity): – images of region being rastered from first moments of the strongest spectral lines Line Width Maps (NT Velocity):Line Width Maps (NT Velocity): – images of region being rastered from second moments of the strongest spectral lines Norikura coronagraph observations of all three of these parameters

31. XRT on Solar-B

32. The End