JSPWiki: EisCoreStudy

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!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])\\

!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])\\

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!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\\

!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\\

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!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])\\

!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])\\

!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])\\

!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])\\

!EIS CORE HOP 137: \\Evolution of Network Boundary Elements: Possible Connections to the Corona – Warren ([hwarren@nrl.navy.mil|mailto:hwarren@nrl.navy.mil])\\

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{{Useful AR context studies for before/after main AR observation are: PRY_slot_context_v3 or PRY_slot_contextLITE}}

Useful AR context studies for before/after main AR observation are: PRY_slot_context_v3 or PRY_slot_contextLITE

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[{ALLOW view jsun,eiscorestudy}]

[{ALLOW edit jsun}]

[Possible EIS Core Team Studies (2009-Dec-01)|http://docs.google.com/Doc?docid=0AdazsPAS3_6xZGNzZHFiOWhfMTY2ZjQ3cG1oZGQ&hl=en&invite=CIDL2K4H]\\

%%(text-align:center;font-size:25px;bold;)

Available EIS Core Team Studies

!!!Quiet Sun\\

!1. Evolution of X-ray bright point – Kamio ([kamio@linmpi.mpg.de|mailto:kamio@linmpi.mpg.de])\\

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-- 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\\

}}

!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])\\

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{{

-- 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) \u2013 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 \\

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{{

-- 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__\\

}}

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{{

-- 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])\\

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{{

-- 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 \\

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{{

-- 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]) \\

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{{

-- 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]) \\

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{{

-- 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])\\

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{{

-- 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]) \\

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{{

-- target: equatorial or low-latitude coronal hole within ± 40%%sup 0%% latitude; Polar CH extensions also possible if within ± 40%%sup 0%%; 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__\\

}}

!11. Quiet sun dynamics study – Muglach __\\

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{{

-- 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|mailto:lmg@mssl.ucl.ac.uk])\\

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{{

-- 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__\\

}}

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{{

-- 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])\\

!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\\

%%information

{{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\\

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{{

-- Studies HPW017AR_30x400_30s2, HPW018AR300x400_30s2 and \\

-- HPW019AR_1x400_45s2\\

-- select as appropriate for AR ToO\\

-- use PRY_slot_context_v3 or PRY_slot_contextLITE before/after selected HPW\\

-- check with Harry Warren re ASRC for raster expansion\\

}}

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

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{{

-- 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|mailto:hwarren@nrl.navy.mil]), Ugarte-Urra ([iugarte@ssd5.nrl.navy.mil|mailto:iugarte@ssd5.nrl.navy.mil]) \\

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{{

-- 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\\

}}

!14/12/09: Active Region Abundance Variations - Ko ([yko@ssd5.nrl.navy.mil|mailto:yko@ssd5.nrl.navy.mil])

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{{

-- target: young AR of less than 3 days; search for any abundance evolution\\

-- FoV to cover centre of the AR\\

-- run study twice a day; separate runs by ~ 12 hours; run for 7 consecutive days until AR west limb passage or decay - subject to TLM limitations\\

-- run YKK_ARabund01; raster scanning: 2” slit and 3” step; exposure: 45s; FOV: 194"x280; duration: 53 m 19s; Data: DCPM/64Mbit.\\

-- run PRY_slot_contextLITE for context after each raster\\

}}

!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\\

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{{

-- 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])\\

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{{

-- 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])\\

%%roundedCorners-yyyy-E3F0EE-808080

{{

-- 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])\\

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{{

-- run cam_ar_limb_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])\\

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{{

-- 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|mailto:danielle.bewsher@stfc.ac.uk]), Harrison\\

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{{

-- 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])\\

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{{

-- 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])\\

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{{

At line 880 changed one line

-- run ID 375 SK_DEEP_5x512_SLIT1 – the 1" slit study, with Y initial positions\\

-- run ID 375 SK_DEEP_5x512_SLIT1 \u2013 the 1" slit study, with Y initial positions\\

At line 882 changed one line

-- run ID 376 SK_DEEP_10x512_SLIT2 – the 2" slit study, with Y initial positions\\

-- run ID 376 SK_DEEP_10x512_SLIT2 \u2013 the 2" slit study, with Y initial positions\\

At line 890 changed one line

This page (revision-186) was last changed on 18-Apr-2021 19:09 by Jian Sun Top

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