EIS Flare Study Option 1: FLR001
This study will be the initial core flare study used by the EIS team during rise of activity in solar cycle 24. Results should allow us to refine future flare studies and to develop strategies for the eventual use of the EIS internal flare trigger.
It includes a fast raster study designed to diagnose flaring plasma through measurement of line intensities, shifts, and widths over a range of high temperatures, as well as electron densities using the Fe XIV line ratio.
The parameters of the initial version are as follows:
Slit size: 2"
Exposure time: 5s
Raster cadence: 5 minutes
The raster comprises 4 spectral windows, each of which are in the LW detector to avoid pointing ambiguities:
Window 1: 254.70 - 255.39. 32 pixels containing Fe XVII (254.87), Fe XXIV (255.11) and Fe X (255.39), with enough room for large blueshifts in Fe XVII.
Window 2: 256.26 - 256.95. 32 pixels containing He II (256.32) and S XIII (256.68).
Window 3: 264.60 - 264.94. 16 pixels centered on density sensitive Fe XIV (264.78).
Window 4: 274.02 - 274.35. 16 pixels centered on density sensitive Fe XIV (274.20).
The study consists of 12 repeats of the raster which will take approximately 1 hour. A single raster has a data volume of 3012.55 kBits after compression, which equals 36.25 MBits per hour. Given the daily telemetry volume for EIS of ~600 MBits per day, this study should be run continuously on a target active region for at least 16 hours per day or longer if possible, adjusting for solar rotation. The flare trigger will not be used at least initially.
EIS Flare Study Option 2: HH_Flare_180x160_1
This study is used to hunt for various flow structures in solar
flares. It can also be used for studies of the active regions. This is a sparse raster study for continuous running at 700 Mbit/day. It uses the 2” slit; 180” X 160” FoV with 8s exposure and 5m cadence for two interleaved rasters. This provides 40% coverage. Three different line lists with 11 or 12 lines each are chosen.
Target: Active region
Type: scanning raster
Field of view: 180"x160"
Exposure time: 8s
step size: 5"
Raster Duration: 6m 13s
Data Volume: 4 Mbits
O VI: detection of TR response at the impulsive phase
Fe X: hunting of reconnection inflow
Fe XII: hunting of reconnection inflow
Fe XIV: study for normal coronal loops with density sensitive pairs
Fe XV : study of flare loops in a cooling phase
Fe XVI: study of flare loops in a cooling phase
Fe XVII: study of flare-loop heating and reconnection outflow
Fe XXIII: study of loop-top hot region and reconnection outflow
Fe XXIV: study of loop-top hot region and reconnection outflow
The non-thermal velocity component in solar flares is
studied by combinations of Fe XXIII and Fe XXIV.
Active region including those with the potential for flaring
Instruction to planners:
1) Centre the raster on an active region
2) When flare hunting, adjust the raster repeat for a maximum run-time
possible, accounting for the TM constraint.
Raster repeat: 160
Run time: 16h 30m
Data volume: 782 Mbits (JPEG85)
Data Volume: 635 Mbits (JPEG75)
Note: When the telemetry is limited, change the compression parameter
from JPEG85 to JPEG75. If in doubt, consult:
Do not adjust the data compression below JPEG75