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[Possible EIS Core Team Studies (2009-Dec-01)|http://docs.google.com/Doc?docid=0AdazsPAS3_6xZGNzZHFiOWhfMTY2ZjQ3cG1oZGQ&hl=en&invite=CIDL2K4H]\\
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Available EIS Core Team Studies /%
!!!Quiet Sun\\
!1. Evolution of X-ray bright point – Kamio ([kamio@linmpi.mpg.de|mailto:kamio@linmpi.mpg.de])
%%roundedCorners-yyyy--CDFFAA-88D84F
* point to a quiet region with an X-ray bright point near disk centre
* run IUU_SLOT_136x400_Q65 (ID # 292) for context \\
__{{
- data volume: 12.1 Mbit; duration: 15m 41s\\
- run SK_QS_34x168c (ID # 295) for BP study; data volume: 2.1 Mbit; dur: 3m 49s\\
- run for 3 hours or longer \\
- SOT: support with magnetograms (3 min cadence) and Ca II H filtergrams to track evolution of magnetic fields in the photosphere\\
}}__
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__2. Coronal/TR Doppler & photosphere transverse magnetic features and cancellation events – Yokoyama ([yokoyama.t@eps.s.u-tokyo.ac.jp|mailto:yokoyama.t@eps.s.u-tokyo.ac.jp])__\\
- QS near the disk centre, if possible, include an XBP in FOV for alignment\\
- observation structure similar to the Muglach programme\\
- 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; volume: 1.4Mbits, \\
- duration: 1.5min, rate:16.4kbps\\
- three images should be taken before and after program b)\\
- b) Study: sta_loop_context_lo (#278); vol: 23.3Mbits, dur: 34min, rate: 34kbps\\
- repeat n times to fit into available data volume\\
- EXPOSURE: 30s, RASTER: 60 steps, SLIT: 2", STEP: 2" FOV: 120"x248"\\
__SOT __support: FG/NFI: NaI/IV 2-wavelength filter (mandatory)\\
- 1st priority on the high cadence (at least < 60sec).\\
- 2nd priority on the longer coverage (>2-3hrs continuous coverage; \\
- Interuptions by SAAs and S/C nights are OK.)\\
- 3rd priority on the FOV (at least, larger than 100arcsec^2)\\
- SP: fast mapping, FOV: same as FG/NFI (mandatory)\\
- FG/BFI: CaII/G-band (lowest priority, can be omitted)\\
__XRT __support: FOV: cover the same FOV as SOT Filters: low-temperature filter-pair; Cadence: <5min\\
!3. QS Brightenings – Bewsher ([d.bewsher@rl.ac.uk|mailto:d.bewsher@rl.ac.uk]), Young \\
EIS to point at quiet Sun region near disk centre \\
run following studies:\\
PRY_slot_context_v3 (dur: 3min; vol: 3 Mbit) once at start of observation\\
tr_bright_lo (dur: 6min; vol: 1.5 Mbit) repeatedly to fill available time slot\\
PRY_slot_context_v3 again, once at end of observation\\
run tr_bright_lo for minimum of 4h; longer if possible\\
request SOT and XRT to observe EIS FoV: 20” x 144”\\
SOHO/CDS involvement desirable; __advise schedule to Bewsher__\\
!4. Search for Evidence of Wave Activity in the Solar Corona - Bewsher ([dbewsher@uclan.ac.uk|mailto:dbewsher@uclan.ac.uk]), Harrison ([richard.harrison@stfc.ac.uk|mailto:richard.harrison@stfc.ac.uk])\\
run__ __rah_line_narrow; duration: 1 h 5 m 20 s; data volume: 24 Mbits\\
run for 6 hour min (~ 144Mbits); longer if possible; repeat to fill time slot\\
point to the off limb ‘quiet’ solar corona above the equator; solar y = 0; limb should be in the fov; planner should maximise the altitude observable\\
request SOT and XRT to observe EIS fov (238 x 256”)\\
__CDS involvement essential,__ __advise schedule to Bewsher – note email change__\\
\\
__5. X-ray Bright Points Onset – Brown __([dsbrown@uclan.ac.uk|mailto:dsbrown@uclan.ac.uk])__, Bewsher ([dbewsher@uclan.ac.uk|mailto: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|mailto: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|mailto: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 HPW019AR__1x400_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|mailto: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|mailto: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|mailto:hwarren@nrl.navy.mil]) Ko ([yko@ssd5.nrl.navy.mil|mailto: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|mailto:yko@ssd5.nrl.navy.mil]) to agree final pointing\\
__see Core HOP 146; use these original studies for on-disc CHs only__\\
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__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)\\
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!12. Filament Evolution – Green ([lmg@mssl.ucl.ac.uk|mailto: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|mailto:db2@mssl.ucl.ac.uk]), Van Driel ([lidia.vandriel@obspm.fr|mailto: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|mailto:alan.gabriel@ias.u-psud.fr]), Harra ([lkh@mssl.ucl.ac.uk|mailto:lkh@mssl.ucl.ac.uk])__\\
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__EIS CORE HOP 130: Multi-temperature Full Disk Slot Scans - Ugarte-Urra ([iugarte@ssd5.nrl.navy.mil|mailto:iugarte@ssd5.nrl.navy.mil]), Brooks ([dhbrooks@ssd5.nrl.navy.mil|mailto:dhbrooks@ssd5.nrl.navy.mil]) __\\
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__EIS CORE HOP 146: Solar Wind Source Regions During Solar Minimum Conditions – Kuen Ko ([yko@ssd5.nrl.navy.mil|mailto:yko@ssd5.nrl.navy.mil]), Mariska ([mariska@nrl.navy.mil|mailto:mariska@nrl.navy.mil])__\\
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__EIS CORE HOP 137: Evolution of Network Boundary Elements: Possible Connections to the Corona – Warren ([hwarren@nrl.navy.mil|mailto: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|mailto: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_context__LITE__ (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|mailto:hwarren@nrl.navy.mil]),__ Ugarte-Urra ([iugarte@ssd5.nrl.navy.mil|mailto: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|mailto:ineke@mcs.st-and.ac.uk]), Bewsher ([d.bewsher@rl.ac.uk|mailto: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|mailto: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|mailto:jlc@mssl.ucl.ac.uk]), Harra ([lkh@mssl.ucl.ac.uk|mailto: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|mailto: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|mailto: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 \\
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__9. CME onsets - Bewsher ([danielle.bewsher@stfc.ac.uk|mailto: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|mailto: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|mailto: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|mailto: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.\\
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