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Possible EIS Core Team Studies (2009-Dec-01)

Quiet Sun
#

1. Evolution of X-ray bright point – Kamio (kamio@linmpi.mpg.de)
#

2. Coronal/TR Doppler & photosphere transverse magnetic features and cancellation events – Yokoyama (yokoyama.t@eps.s.u-tokyo.ac.jp)
#

3. QS Brightenings – Bewsher (d.bewsher@rl.ac.uk), Young
#

4. Search for Evidence of Wave Activity in the Solar Corona - Bewsher (dbewsher@uclan.ac.uk), Harrison (richard.harrison@stfc.ac.uk)
#

5. X-ray Bright Points Onset – Brown (dsbrown@uclan.ac.uk), Bewsher (dbewsher@uclan.ac.uk)
EIS to point at quiet Sun region near disk centre
target QS magnetic fragments as seen by SOT with little/no emission in the corona
run the following studies:
PRY_slot_context_v2 (dur 3 min; vol 3 Mbit) once at start of observation
dob_bp_slit_raster (dur 33m 50s; vol 7 Mbit) or dob_bp_slot_raster (dur 2m 13s; vol 7 Mbit); repeat to fill available time slot
PRY_slot_context_v2 at end of observations
run dob_bp_****_raster for minimum 4h; run both studies on different days
request SOT and XRT to observe EIS FoV: 120x160" (dob_bp_slit_raster) or 160x160" (dob_bp_slot_raster)
TRACE/CDS involvement desirable; advise schedule to Brown and Bewsher

6. Coronal Jets – Warren (hwarren@nrl.navy.mil), Ugarte-Urra
#

measure DEM in jet reconnection region
run slot_context_lite_v1 before/after IUU_SCAN_STEPS_002 in N- polar CH
place raster (slit: 368") so that part covers adjacent Quiet Sun
run for as long as possible outside of eclipse

7. Quiet Sun diagnostics/evolution - Ugarte-Urra (iugarte@ssd5.nrl.navy.mil)
#

point to a generic quiet Sun region (solar tracking). Two study sequences:
a) run NRL_QSCH_30X400_90s2 multiple times (3 at least)
b) run IUU_SLOT_488x512 as context
run HPW019AR1x400_45s (sit-and-stare) for 2 hours
run IUU_SLOT_488X512 as context
Note: ideally run sequences one after the other on the same pointing.
sequences can run independently of each other if needed.
SOT magnetograms and XRT C_poly or Al_poly observations desirable,
matching EIS cadence (1-2 min) in sequence b)

8. Coronal Hole Density Measurement – Young (peter.young.ctr.uk@nrl.navy.mil)
#

polar or equatorial CH
select pointing based on EIT 195 images; choose darkest part of CH
accurate warm pixel removal essential for CH data
run REGCAL071 and REGCAL072 on the same day; also context study
study sequence is: REGCAL071; REGCAL072; PRY_slot_context_v2 ;
PRY_CH_density
run on mid-latitude extension to N-polar CH
Note 1: repeat PRY_CH_density to fill time slot; vol: 20 Mbit; data rate: 5.2 kbps
Note 2: for large dark CH areas, stitch two or more repeats of PRY_CH_density

9. Eclipse Spectral Atlas - Young (pyoung@ssd5.nrl.navy.mil)
#

obtain reference spectra for general science during Hinode eclipse season
run PRY_slot_context_v3 (5 Mbits) and Eclipse_raster_v2 (99 Mbits)
observe any target
run PRY_slot_context_v3 once
follow by one run of Eclipse_raster_v2 (total duration: 54mins)
start PRY_slot_context_v3 10 mins after end of Hinode orbital night
repeat for consecutive day-time periods depending on available data volume

10. Properties in Solar Wind Source Regions – Warren (hwarren@nrl.navy.mil) Ko (yko@ssd5.nrl.navy.mil)
#

target: equatorial or low-latitude coronal hole within ± 400 latitude; Polar CH extensions also possible if within ± 400; observe with CH at central meridian
run a) YKK_EqCH_02n around the centre of the coronal hole
run b) YKK_EqCH_02n between the centre and East CH boundary
run c) YKK_EqCH_02w at E CH boundary partly covering the 'visible' CH, partly covering adjacent AR or QS to the East
run context raster slot_context_q50 covering FOV of the a, b and c rasters
default pointing: Sun center X=0", Y=0"; slit field-of-view to cover the solar equator; if CH does not reach latitude zero cover lowest latitude reached
if all three studies not possible in time available, run b) followed by c)
contact Yuan-Kuen Ko (yko@ssd5.nrl.navy.mil) to agree final pointing
see Core HOP 146; use these original studies for on-disc CHs only

11. Quiet sun dynamics study – Muglach
- run studies in the order: three times (a) - n times (b) – three times (a)
- a) Study: quiet_sun_slot (#210); 40x512 slot image as context
- three images should be taken before and after program b)
- b) Study: KM-qs-study-low (#315)
- run in areas of quiet Sun, also plage or moderately active regions possible
- slit should at least be partially on the disk
- avoid large, well developed ARs and coronal holes
- study for small-scale short-term variation of QS structures in cool EIS lines.
- repeat n times to fit into available data volume; at least for 30 min
- EXPOSURE: 20s, RASTER: Scanning, 4 steps, SLIT: 2", STEP: 2"
FOV: 10"x464"
- if n = 30 for (b), data volume is 70 Mbits; run (b) for longer if volume available
Co-observing: - SOT:
1) magnetograms in either Fe I or Na I, in 60s cadence (or less if telemetry allows).
SOT to run > 15 min before EIS start and at least 15 min after EIS end.
2) SP scans of the target regions valuable additions but lower priority than 1.
3) BFI images in G-Band can be added; lower priority than 1 and 2.
4) XRT: filtergrams in the thinnest filter(s)

12. Filament Evolution – Green (lmg@mssl.ucl.ac.uk)
#

- Observe an on-disc filament
- Run
- cme_slot_red_lkh for approx 30 min; data vol: 18 Mbit; context
- cme_slit_red_lkh to fill available time; 34 min has data vol: 31 Mbit
- cme_slot_red_lkh for approx 30 min; data vol: 18 Mbit; context
- Run if suitable quiescent filament is available on disc

13. Interchange Reconnection at CH Boundaries – Baker (db2@mssl.ucl.ac.uk), Van Driel (lidia.vandriel@obspm.fr) search for closed/open field interactions at CH boundaries with adjacent activity
#

run dhb_polar_scan_Q90 (ID #294);
check with proposers for pointing details
run for small closed structures at CH boundaries or inside on-disc CHs
------------------------------------------------------------------------------------------------------EIS CORE HOP 80: Polar Coronal Hole Observation – Gabriel (alan.gabriel@ias.u-psud.fr), Harra (lkh@mssl.ucl.ac.uk)

EIS CORE HOP 130: Multi-temperature Full Disk Slot Scans - Ugarte-Urra (iugarte@ssd5.nrl.navy.mil), Brooks (dhbrooks@ssd5.nrl.navy.mil)

EIS CORE HOP 146: Solar Wind Source Regions During Solar Minimum Conditions – Kuen Ko (yko@ssd5.nrl.navy.mil), Mariska (mariska@nrl.navy.mil)

EIS CORE HOP 137: Evolution of Network Boundary Elements: Possible Connections to the Corona – Warren (hwarren@nrl.navy.mil)
------------------------------------------------------------------------------------------------------B. Active Region, Flare, CME
Useful AR context studies for before/after main AR observation are:
PRY_slot_context_v3 or PRY_slot_contextLITE

1. Active Region Studies – Warren (hwarren@nrl.navy.mil), Mariska
Studies HPW017AR_30x400_30s2, HPW018AR300x400_30s2 and
HPW019AR_1x400_45s2
select as appropriate for AR ToO
use PRY_slot_context_v3 or PRY_slot_context LITE before/after selected HPW
check with Harry Warren re ASRC for raster expansion

2. AR dynamics and CME watch – Young, Ugarte-Urra
#

40” slot for large FoV, high cadence AR images in a wide Te range to i) examine loop morphology ii) detect CME initiation.
run either i) PRY_slot_context_v3 (AR dynamics, includes diagnostics) or ii) PRY_slot_contextLITE (488”x488”; 3.5min); (CME watch, low TLM, extended hours)
repeat to fill available time slot
- run for 3 hours, preferably longer

3. Active Region Studies – Warren

(hwarren@nrl.navy.mil), Ugarte-Urra (iugarte@ssd5.nrl.navy.mil)
# - observe the large dispersing AR near CM
- run a large raster with HPW018
- run a fast scan with IUU_SCAN_STEPS_002 for several hours

4. Loop morphology and oscillations - de Moortel (ineke@mcs.st-and.ac.uk), Bewsher (d.bewsher@rl.ac.uk), Young
relatively quiescent (non-flaring) coronal loop system either on disk or limb.
point to loops in the active region.
run PRY_footpoints_lite (dur: 28min; vol: 55 Mbit), sta_loop_slot_lo (dur: 39min; vol: 22 Mbit).
- study sequence is:
- PRY_footpoints_lite once at beginning of a period
- sta_loop_slot_lo at the same pointing
- repeat sta_loop_slot_lo to fill available time slot.
run on any quiescent AR; advise schedule to de Moortel

5. Pre-flare activity monitoring - Wallace (ajw2@mssl.ucl.ac.uk)
#

point to a flaring AR to search for features that precede flares
run Flare0_slit_AJW; (dur: 50m 34s; vol: 2.9 Mbits; size: 180” x 320”)
scanning raster; slit: 2”; step:2”; exposure: 30s; 89 steps.
run repeatedly on a flaring AR to fill available time allocation.

6. Search for Active Region outflows – Culhane (jlc@mssl.ucl.ac.uk), Harra (lkh@mssl.ucl.ac.uk)
#

- observe AR outflows at opposite boundaries of the large dispersing AR near CM
- run HPW015_DETAILED_MAP_1_45s_200x360 twice; two separate pointings
- total data volume: 662 Mbits; duration: 2 x 2h 44 m or 5h 28 m total
- check pointing positions with proposers

7. AR Temperature Diagnostic – Mason (hm11@damtp.cam.ac.uk)
#

run cam_ar_temp_lite_v2
target: temperature structure of active regions on the limb
centre raster at the active region core.
exposure time: 30s; raster: scanning; slit: 2"; step Size: 2", FOV: 360"X400";
raster duration: 1h40m46s

8. High cadence observations of AR transient brightenings and microflares - Mason (hm11@damtp.cam.ac.uk)
#

run cam_artb_lite_v2
run on AR to study transient brightenings and microflares at very high cadence
raster centre should be at polarity inversion line.
raster: scanning; slit: 2", step size: 2"; FOV: 40"X120"
raster duration: 4m32 seconds
run as many times as possible and at least for 3-4 hours continuous


9. CME onsets - Bewsher (danielle.bewsher@stfc.ac.uk), Harrison
algorithm to detect CME-related dimming
point above limb at AR if it develops with part of limb in FoV
if AR present, centre raster y-direction on the AR; null evaluation in AR absence
run cmeo_slit_lo; minimum 5 rasters; Duration: 4.2 h; Volume: 13 Mbit or
run cmeo_slot_lo; min duration: 5 h; Volume: 10 Mbit
algorithm uses difference imaging so minimum durations must be available

10. CORE EIS Flare Study – Milligan (ryan.o.milligan@nasa.gov)
#

run FLR001_flare_study;
exposure: 5s; raster: scanning; slit: 2”; step: 2”; FoV: 80” x 120”; raster time: 5m
run for 2 hr; data volume: 36 Mbit
target: any AR with significant flare probability

C. Test and Calibration Studies
#

1. EIS slit calibration – Young (pyoung@ssd5.nrl.navy.mil)
- Obtain co-spatial data in the 1", 2" and 40" slits for various calibration tests (slit
widths, tilt, intensity calibration)
- run CALIB_slit_slot_v1
- study includes three separate rasters; each must be individually pointed
- point off-limb above the quiet Sun at the equator (either limb)
- make two separate adjacent entries of calib_slit_slot_v1 on the timeline
- select Solar-X position 50-60” above limb; same for each of the rasters in both
study entries
- select Y position with the YIP input rather than the solar-Y position
- set the YIP entry to 511 for each of the three rasters in first study entry
- for the second study entry, set YIP to 1 for each of the three rasters
- data volume: 54 Mbits.

2. EIS velocity calibration – Kamio (kamio@linmpi.mpg.de)
- Determine the slit tilt and curvature in full Y height for velocity calibration
- execute raster scans at three positions with 1" and 2" slits
- run ID 375 SK_DEEP_5x512_SLIT1 – the 1" slit study, with Y initial positions
#1 YIP=1; #2 YIP=256; #3 YIP=512
- run ID 376 SK_DEEP_10x512_SLIT2 – the 2" slit study, with Y initial positions
#4 YIP=1; #5 YIP=256; #6 YIP=512
- six consecutive rasters require total time 60min and data volume 45Mbits
- target: quiet region near disk center (0", 0"); shift EIS FOV ±200" in E-W
direction to avoid ARs; do not run if ARs in target area;
- keep the same mirror initial position (MIP) for all rasters.