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EIS - MSSL/NRL EUV Imaging Spectrometer SOT - ISAS/NAOJ Solar Optical Telescope PowerPoint Presentation
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EIS - MSSL/NRL EUV Imaging Spectrometer SOT - ISAS/NAOJ Solar Optical Telescope XRT - SAO/ISAS X-ray Telescope FPP - Lockheed/NAOJ Focal Plane Package. Mission Characteristics. Launch date: August 2006 Launch vehicle: ISAS MV Mission lifetime: 3 years. Orbit: Polar, sun synchronous

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Presentation Transcript
slide1

EIS - MSSL/NRL EUV Imaging Spectrometer

SOT - ISAS/NAOJ Solar Optical Telescope

XRT - SAO/ISAS X-ray Telescope

FPP - Lockheed/NAOJ Focal Plane Package

mission characteristics
Mission Characteristics
  • Launch date: August 2006
  • Launch vehicle: ISAS MV
  • Mission lifetime: 3 years
  • Orbit: Polar, sun synchronous
  • Inclination: 97.9 degrees
  • Altitude: 600 km.
  • Mass: 900 kg
slide3

EIS - Instrument Features

  • Large Effective Area in two EUV bands: 170-210 Å and 250-290 Å
    • Multi-layer Mirror (15 cm dia ) and Grating; both with optimised Mo/Si Coatings
    • CCD camera; Two 2048 x 1024 high QE back illuminated CCDs
  • Spatial resolution: 1 arcsec pixels/2 arcsec resolution
  • Line spectroscopy with ~ 25 km/s pixel sampling
  • Field of View:
    • Raster: 6 arcmin×8.5 arcmin;
    • FOV centre moveable E – W by ± 15 arcmin
  • Wide temperature coverage: log T = 4.7, 5.4, 6.0 - 7.3 K
  • Simultaneous observation of up to 25 lines
slide4

EIS Optical Diagram

Primary Mirror

1939 mm

Slit Exchange Mechanism

Shutter

Entrance Filter

CCDs

Filter

1000 mm

1440 mm

Concave Grating

Primary Mirror

Entrance Filter

CCD Camera

Front Baffle

Grating

slide5

Dual CCD Camera

Grating

Primary Mirror

EIS Instrument Completed

Filter Holder Installed

Entrance Filter Holder

Installation of Key Subsystems in Structure

observables



w

Observables
  • Observation of single lines
    • Line intensity and profile
    • Line shift () → Doppler motion
    • Line width (w) and temperature

→ Nonthermal motion

  • Observation of line pair ratios
    • Temperature
    • Density
  • Observation of multiple lines
    • Differential emission measure
slide8

Slit and Slot Interchange

  • 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
eis field of view fov

Shift of FOV center with coarse-mirror motion

Maximum FOV for raster observation

360 

900 

900 

512 

512 

512 

Raster-scan range

250 

slot

40 

slot

EIS Slit

EIS Field-of-View (FOV)
expected accuracy of velocity
Expected Accuracy of Velocity

Flare line

Bright AR line

Photons (11 area)-1 sec-1

Photons (11 area)-1 (10sec)-1

Doppler velocity

Line width

Number of detected photons

processed science data products

Norikura coronagraph observations

of all three of these parameters

Processed Science Data Products
  • Intensity Maps (Te, ne):

– images of region being rastered

from the zeroth moments of

strongest spectral lines

  • Doppler Shift Maps (Bulk Velocity):

– images of region being rastered from

first moments of the strongest

spectral lines

  • Line Width Maps (NT Velocity):

– images of region being rastered from

second moments of the strongest

spectral lines

the first 3 months
The first 3 months….
  • Flare trigger and dynamics:Spatial determination of evaporation and turbulence in a flare
  • Active region heating:Spatial determination of the velocity field in active region loops
  • Coronal Hole Boundaries:Measurement of intensity and velocity field at a coronal hole boundary
  • Quiet Sun Brightenings:Determination of the relationship between different categories of quiet Sun events.
active regions
Active Regions
  • connect the photospheric velocity field to the signatures of coronal heating. This will allow us to determine the dominant heating mechanism in active regions, and will be extended to other coronal brightenings.
  • search for evidence of waves in loops and make use of observations for coronal seismology
  • study dynamic phenomena within active region loops.
quiet sun
Quiet Sun
  • 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.
  • determine the variation of explosive events and blinkers with temperature.
  • Search for evidence of reconnection and flows at junctions between open and closed magnetic field at coronal hole boundaries.
  • Determine the impact of quiet Sun events on larger scale structures within the corona.
  • Determine physical size scales using density diagnostics.
solar flares
Solar Flares
  • 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. Hence will allow us to address the trigger mechanism.
  • detection of reconnection inflows, outflows and the associated turbulence which play the pivotal role in flare particle acceleration.
coronal mass ejections
Coronal Mass Ejections
  • determine the location of dimming (and the subsequent velocities) in various magnetic configurations allowing us to determine the magnetic environment that leads to a coronal mass ejection.
  • The situations to be studied include filaments, flaring active regions and trans-equatorial loops.
large scale structures
Large Scale Structures
  • determine the temperature and velocity structure in a coronal streamer
  • determine the velocity field and temperature change of a trans-equatorial loop, and search for evidence of large-scale reconnection.
  • Using a low-latitude coronal hole, search for evidence of the fast solar wind.
slide19

Information is maintained on our website;

http://www.mssl.ucl.ac.uk/www_solar/solarB/

The EIS science planning guide shows details of the 3 month plan studies including line choices, which slit/slot, FOV etc.

The planning software will be released into SSW in the autumn. Quicklook software etc. is already in SSW. Details are on the website.

The next solar-B science meeting will be in Kyoto in November.