JSPWiki: EisCoreStudy

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Page References

Incoming links	Outgoing links
EisCoreStudy...nobody	EisCoreStudy

Version management

Difference between version and

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[{ALLOW edit EISMainUsers}]

[{ALLOW view Anonymous}]

[{ALLOW view jsun,eiscorestudy}]

[{ALLOW edit jsun}]

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%%roundedCorners-yyyy-E3F0EE-808080

{{

=> The conventions of title: HEADERyyyymmdd-Index => brief descriptions\\

    HEADER: qs (Quite Sun); ar (Active Region); hop (Hinode Operation Plan); test (Test studies)\\

    yyyymmdd: the date when the study is added; For "hop" and "test" header, it may be different\\

  For example: ar20100417-13 => Nanoflare heating of coronal loops\\ \\

=> study qs20091216-09 has been replaced by a new study (ie. syo20100504-01) since 2010-May-04\\

=> study ar20100329-12 has been replaced by a new study (ie. syo20100504-01) since 2010-May-04\\

=> study ar20110209-20 has been replaced by a new study (ie.  ar20110404-21) since 2010-Apr-04

}}

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

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[{TableOfContents}]

%%(text-align:center;font-size:20px;bold;)

!!!Available EIS Core Team Studies

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

Available EIS Core Team Studies

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!!!Quiet Sun\\

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!!A. Quiet Sun\\

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

At line 29 changed 5 lines

!qs20091216-01 => Evolution of X-ray bright point

  – Kamio ([kamio@linmpi.mpg.de|mailto:kamio@linmpi.mpg.de])\\

%%roundedCorners-yyyy-E3F0EE-808080

%%roundedCorners-yyyy-99ccff-000000

At line 35 changed 6 lines

-- 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|https://vsolar.mssl.ucl.ac.uk/SolarB/ShowEisStudy.jsp?study=295] (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\\

- 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\\

At line 43 removed 87 lines

%%center

||Study ID||Acronym|| ||

!qs20091216-02 => 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])\\

%%roundedCorners-yyyy-E3F0EE-808080

{{

-- 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\\

}}

%%center

||Study ID||Acronym|| ||

!qs20091216-03 => QS Brightenings

  – Bewsher ([d.bewsher@rl.ac.uk|mailto:d.bewsher@rl.ac.uk]), Young \\

%%roundedCorners-yyyy-E3F0EE-808080

{{

-- 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__\\

}}

%%center

||Study ID||Acronym|| ||

!qs20091216-04 => 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])\\

%%roundedCorners-yyyy-E3F0EE-808080

{{

-- 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__\\

}}

%%center

||Study ID||Acronym|| ||

At line 131 changed 89 lines

!qs20091216-05 => 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])\\

%%roundedCorners-yyyy-E3F0EE-808080

{{

-- 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__\\

}}

%%center

||Study ID||Acronym|| ||

!qs20091216-06 => Coronal Jets

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

%%roundedCorners-yyyy-E3F0EE-808080

{{

-- 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\\

}}

%%center

||Study ID||Acronym|| ||

!qs20091216-07 => Quiet Sun diagnostics/evolution

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

%%roundedCorners-yyyy-E3F0EE-808080

{{

-- 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)\\

}}

%%center

||Study ID||Acronym|| ||

!qs20091216-08 => Coronal Hole Density Measurement

  – Young ([peter.young.ctr.uk@nrl.navy.mil|mailto:peter.young.ctr.uk@nrl.navy.mil]) \\

%%roundedCorners-yyyy-E3F0EE-808080

{{

-- 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\\

__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\\

At line 222 changed 71 lines

}}

%%center

||Study ID||Acronym|| ||

!qs20091216-10 => 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]) \\

%%roundedCorners-yyyy-E3F0EE-808080

{{

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

}}

%%center

||Study ID||Acronym|| ||

!qs20091216-11 => Quiet sun dynamics study

  – Muglach __\\

%%roundedCorners-yyyy-E3F0EE-808080

{{

-- 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)\\

}}

%%center

||Study ID||Acronym|| ||

!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__\\

At line 294 changed 68 lines

!qs20091216-12 => Filament Evolution

  – Green ([lmg@mssl.ucl.ac.uk|mailto:lmg@mssl.ucl.ac.uk])\\

%%roundedCorners-yyyy-E3F0EE-808080

{{

-- 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__\\

}}

%%center

||Study ID||Acronym|| ||

!qs20091216-13 => Interchange Reconnection at CH Boundaries

  – Search for closed/open field interactions at CH boundaries with adjacent activity\\

  – Baker ([db2@mssl.ucl.ac.uk|mailto:db2@mssl.ucl.ac.uk]), Van Driel ([lidia.vandriel@obspm.fr|mailto:lidia.vandriel@obspm.fr]) \\

%%roundedCorners-yyyy-E3F0EE-808080

{{

-- 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__\\

}}

%%center

||Study ID||Acronym|| ||

!!B. EIS HOP Obs.\\

!hop-a => 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])\\

!hop-b => 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])\\

!hop-c => 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])\\

__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)\\

At line 363 removed 7 lines

!hop-d => EIS CORE HOP 137

Evolution of Network Boundary Elements: Possible Connections to the Corona\\

  – Warren ([hwarren@nrl.navy.mil|mailto:hwarren@nrl.navy.mil])\\

At line 371 removed 48 lines

!hop-e => EIS CORE HOP 131 (ToO)

Helioseismology Observations of Coronal Holes with SOT\\

  – Harra ([lkh@mssl.ucl.ac.uk|mailto:lkh@mssl.ucl.ac.uk]), Zharkov ([sz2@mssl.ucl.ac.uk|mailto:sz2@mssl.ucl.ac.uk]), Sekii ([sekii@solar.mtk.nao.ac.jp|mailto:sekii@solar.mtk.nao.ac.jp])\\

__Note__: ToO is for "Targets of Opportunity"\\

!hop-f => EIS CORE HOP 150 (ToO)

Flows during a filament eruption\\

  – Harra ([lkh@mssl.ucl.ac.uk|mailto:lkh@mssl.ucl.ac.uk]), Culhane ([jlc@mssl.ucl.ac.uk|mailto:jlc@mssl.ucl.ac.uk]), Demoulin, Mandrini, Kliem, Williams\\

__Note__: ToO is for "Targets of Opportunity"\\

!hop-g => EIS CORE HOP 160 (ToO)

Long-term Evolution of AR from Flux Emergence through Decay\\

  – Del Zanna ([GDelZanna@spd.aas.org|mailto:GDelZanna@spd.aas.org]), van Driel-Gesztelyi ([lvdg@mssl.ucl.ac.uk|mailto:lvdg@mssl.ucl.ac.uk])\\

__Note__: ToO is for "Targets of Opportunity"\\

!hop-h => EIS CORE HOP 163 (ToO)

Variations in Line Width Across kG Magnetic Field Patches in Coronal Holes\\

  – Harra ([lkh@mssl.ucl.ac.uk|mailto:lkh@mssl.ucl.ac.uk]), Tsuneta, Ito, Shiota\\

__Note__: ToO is for "Targets of Opportunity"\\

!!C. Active Region, Flare, CME\\

%%information

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

At line 420 removed 64 lines

!ar20091216-01 => 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\\

}}

%%center

||Study ID||Acronym|| ||

!ar20091216-02 => AR dynamics and CME watch

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

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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\\

}}

%%center

||Study ID||Acronym|| ||

!ar20091216-03 => 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\\

}}

%%center

||Study ID||Acronym|| ||

At line 485 changed 107 lines

!ar20091216-04 => 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\\

}}

%%center

||Study ID||Acronym|| ||

!ar20091216-05 => 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.\\

}}

%%center

||Study ID||Acronym|| ||

!ar20091216-06 => 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])\\

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{{

-- 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__\\

}}

%%center

||Study ID||Acronym|| ||

!ar20091216-07 => 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: 45s; raster: scanning; slit: 2"; step Size: 2", FOV: 322"X376";\\

  -- raster duration: 2h13m15s; Data volume: 186 Mbits;\\

}}

%%center

||Study ID||Acronym|| ||

!ar20091216-08 => 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 \\

-- run context study PRY_slot_context_v3 before and after\\

}}

%%center

||Study ID||Acronym|| ||

!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])__\\

At line 593 changed 358 lines

!ar20091216-09 => CME onsets

  – Bewsher ([danielle.bewsher@stfc.ac.uk|mailto:danielle.bewsher@stfc.ac.uk]), Harrison([Richard.Harrison@stfc.ac.uk|mailto:Richard.Harrison@stfc.ac.uk])\\

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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\\

}}

%%center

||Study ID||Acronym|| ||

!ar20091216-10 => CORE EIS Flare Study 1

  – 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 as long as possible with available TLM; data volume: 37 Mbit/hr\\

-- target: any AR with significant flare probability\\

-- see [http://www.mssl.ucl.ac.uk/www_solar/eisflarestudy.html] for further details\\

}}

%%center

||Study ID||Acronym|| ||

!ar20091229-11 => CORE EIS Flare Study 2

  – Hara ([hara@solar.mtk.nao.ac.jp|mailto:hara@solar.mtk.nao.ac.jp])\\

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{{

-- study used to search for flow structures in flares\\

-- run HH_Flare+AR_180x152 (ID # 461)\\

-- exposure: 9s; raster: scanning, sparse; slit: 2”; step: 6”; FoV: 180” x 152”;\\

-- raster time: 6m 5s, data volume: 3.6 Mbit (JPEG75), 4.4 Mbit (JPEG85)\\

-- default compression is JPEG75; use JPEG85 for short runs\\

-- centre raster on expected AR flare site; adjust raster repeat for maximum possible runtime within telemetry constrainta\\

-- see [http://www.mssl.ucl.ac.uk/www_solar/eisflarestudy.html] for further details\\

}}

%%center

||Study ID||Acronym|| ||

!ar20100417-13 => Nanoflare heating of coronal loops

  – Klimchuk ([james.a.klimchuk@masa.gov|mailto:james.a.klimchuk@masa.gov]), Patsourakos ([spatsurakos@gmail.com|mailto:spatsurakos@gmail.com]), Young ([pyoung@ssd5.nrl.navy.mil|mailto:pyoung@ssd5.nrl.navy.mil])\\

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{{

-- test theory that coronal loops are bundles of unresolved, impulsively-heated strands by searching for spectral signatures in the wings of hot (~ 5MK) emission lines\\

-- run PRY_slot_context_v3 (4.9 Mbits, 3min 29s), nanoflare_sas_v1 (82.5 Mbits, 31min 24s)\\

-- run sequence: PRY_slot_context_v3, then nanoflare_sas_v1, finally PRY_slot_context_v3\\

-- run nanoflare_sas_v1 multiple times with raster repeats to fill available time\\

-- AR pointing for nanoflare_sas_v1 to be at lower legs of loops\\

-- select inner part of AR; not perimeter “fan” loops\\

-- choose side of AR with legs oriented along line-of-sight to maximize Doppler shift due to field-aligned flows\\

-- prefer ARs near disk center\\

-- for wavelength calibration, position hot loops towards either bottom or top of slit; ensure that the opposite side of the slit observes a quiet Sun region.\\

__NOTE__: for pointing confirmation, please send screen grab from eis_image_tool to all three study authors showing suggested pointing. See [http://tiny.cc/43rcc] for typical pointing examples\\

}}

%%center

||Study ID||Acronym|| ||

!ar20100423-14 => Active Region Transient Brightening Lite

  – Mason ([hm11@damtp.cam.ac.uk|mailto:hm11@damtp.cam.ac.uk])\\

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{{

-- run cam_artb_cds_a_lite\\

-- observe on-disc active region close to disc centre; study AR transient brightening and density structure\\

--   raster to be centred on AR core or polarity inversion line\\

--   exposure time: 10s; raster scanning; slit: 2"; step size: 2"; FOV: 200" x 400"\\

--   raster duration: 21m09s; data volume: 108 Mbits\\

--   run context study PRY_slot_context_v3 before and after

}}

%%center

||Study ID||Acronym|| ||

!ar20100423-15 => Multi-temperature Observation of Sigmoids

  – Mason ([hm11@damtp.cam.ac.uk|mailto:hm11@damtp.cam.ac.uk])\\

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{{

-- run cam_sigmoid_study_v1\\

-- observe temperature structure of cooling plasma in sigmoidal structures on newly reconnected flux rope field lines\\

--   select small to medium size ARs; the AR should be in the centre of the raster\\

--   exposure time: 10s; raster scanning; slit: 2"; step size: 2"; FOV: 400" x 400"\\

--   raster duration: 41m33s; data volume: 125 Mbits\\

--   repeat to fill available time slot; minimum of 4 repeats preferred (needs 500 Mbits)\\

}}

%%center

||Study ID||Acronym|| ||

!ar20100426-16 => Outflows from Small Active Regfions

  – Young ([pyoung@ssd5.nrl.navy.mil|mailto:pyoung@ssd5.nrl.navy.mil])\\

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{{

-- observe small ARs simultaneously with QS regions to obtain accurate outflow velocities\\

-- run PRY_loop_velocity\\

--   duration: 4h33m; volume:230 Mbits\\

--   position AR near top or bottom of slit; see example at *[http://tiny.cc/qccji|http://tiny.cc/qccji]*\\

--   ensure that any fan loops visible in 171 Å images are contained within raster\\

--   avoid complex ARs\\

}}

%%center

||Study ID||Acronym|| ||

!ar20100622-17 => AR Temperatures and Flows Optimized for Eclipse Observing

  – Warren ([harry.warren@nrl.navy.mil|mailto:harry.warren@nrl.navy.mil])\\

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{{

-- run hpw021_vel_120x512v1\\

--   duration should allow it to be run between eclipses; can be run multiple times to cover a larger area; avoid SAA.\\

--   target: active region\\

--   full slit is taken; position active region near top or bottom of slit so that there is ample quiet Sun for velocity calibration.\\

--   exposure time: 60s; raster: scanning; slit: 1"; step Size: 2", FOV: 120"x512";\\

--   raster duration:1h4m58s; data volume: 135 Mbits \\

}}

%%center

||Study ID||Acronym|| ||

!ar20101109-18 => Dynamic events at the limb with EIS and AIA

  – Young ([pyoung@ssd5.nrl.navy.mil|mailto:pyoung@ssd5.nrl.navy.mil])\\

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{{

-- pointing should be above the limb, preferably an active region; quiet Sun or prominence cavity also acceptable\\

-- sequence: first run PRY_slot_context_v3, then PRY_sit_stare_1 (repeat for several hours), then PRY_slot_context_v3\\

-- XRT: high cadence, long duration, Y-coverage: 512”; spatial resolution: 1-2” preferred\\

-- SOT: Ca II and/or H-alpha, with high cadence, long duration preferred over spatial resolution \\

}}

%%center

||Study ID||Acronym|| ||

!ar20110120-19 => AR Loop footpoint studies using the bright point trigger

  – Young ([pyoung@ssd5.nrl.navy.mil|mailto:pyoung@ssd5.nrl.navy.mil])\\

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{{

-- observe AR on the disc with bright loop footpoints (check AIA 171 image)\\

-- target region near central meridian preferred\\

-- run Hunter_loop_fe8 (ID: 445, 3.1 Mbits, 24min); set response study to be Cool_loop_response\\

   (ID: 444, 268 Mbits, 2hr 52m)\\

-- BP trigger parameters are given in the Hunter_loop_fe8 study description, but change the Xthresh \\

   value to 5000 (instead of 5460)\\

}}

%%center

||Study ID||Acronym|| ||

!ar20110404-21 => Search for slow mode oscillations in coronal loops

  – Wang ([tongjiang.wang@nasa.gov|mailto:tongjiang.wang@nasa.gov]), Mariska ([john.mariska@nrl.navy.mil|mailto:john.mariska@nrl.navy.mil])\\

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{{

-- pointing is to a possibly flare-productive active region on the limb.\\

-- for Study A, 1/3 FOV on the disk and 2/3 FOV off the limb.\\

-- for Studies B and and C, the slit center position is set about 30-50 arcsec above the AR on the \\

   limb (close to the AR core)\\

-- run PRY_slot_contextLITE (ID #354); Study A\\

-- run Hot_loop_osci_1_v3 (ID #459); Study B, repeating for up to 5 hrs\\

-- run PRY_slot_contextLITE (ID #354); Study A\\

-- run Hot_loop_osci_2_v3 (ID #460); Study C, repeating for up to 5 hrs\\

-- run PRY_slot_contextLITE (ID #354); Study A\\

-- runs can be done in two parts: A B A as one part and A C A as the second part.\\

-- each sequence above should be run uninterrupted (preferably use chained studies)\\

}}

%%center

||Study ID||Acronym|| ||

!ar20110411-22 => Cambridge Diagnostic Study for the Impulsive Phase of Small Flares

  – DelZanna ([gdelzanna@spd.aas.org|mailto:gdelzanna@spd.aas.org]), Mason ([h.e.mason@damtp.cam.ac.uk|mailto:h.e.mason@damtp.cam.ac.uk])\\

%%roundedCorners-yyyy-E3F0EE-808080

{{

-- run on small flare-productive AR as it crosses the disc; avoid X-flare regions\\

-- run a high-cadence (2m 47s), small (60” x 120”), sparse (3”) raster on a small AR; 2” slit; 5s exposure\\

-- point to AR core; on-disc and near CM\\

-- run Cam_flare_diag (ID # 458)\\

-- run continuously for ~ 12 hr; 230 repetitions for 10.7 hr and 590 Mbit\\

-- request XRT: FoV ≥ 384” x 384”; use AEC; 2 x 2 binning acceptable; Filters: at least Al_poly_open and one thick filter\\

-- request SOT/FG: NFI Na I 589.6 shuttered Stokes IV with partial FoV (164” x 164”); 2 x 2 binning; 1 – 3 min or longer cadence\\

-- request SOT/SP: Fast map Stokes IQUV 164” x 164”; run at beginning and possibly at end of SOT/FG sequence\\

}}

%%center

||Study ID||Acronym|| ||

!!D. Synoptic and Other Studies\\

!syo20100504-01 => EIS Spectral Atlas Synoptic Programme

  – Young ([pyoung@ssd5.nrl.navy.mil|mailto:pyoung@ssd5.nrl.navy.mil]), Warren, Mason, Del Zanna\\

%%roundedCorners-yyyy-E3F0EE-808080

{{

-- run twice each month; in the first and third full weeks of the month\\

-- run PRY_slot_context_v3; Duration: 3min 29s; Data volume: 5 Mbit\\

-- follow with either Atlas_30s (34min, 257 Mbit), or Atlas_60s (65min, 257 Mbit)\\

-- pointing to be specified by email to CO at start of observing week by P. Young\\

-- in absence of specific target, CO is free to choose any solar feature on- or off-disc\\

--   *NOTE: use Atlas_30s only if an AR is forecast to produce M-class or greater flares; use Atlas_60s for all other targets*\\

}}

%%center

||Study ID||Acronym|| ||

!syo20100713-02 => Full CCD Study to Measure Relative Wavelengths

  – Warren ([hwarren@nrl.navy.mil|mailto:hwarren@nrl.navy.mil])\\

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{{

-- run HPW020_VEL_FULLs1 (ID # 413)\\

-- full CCD sit-and-stare study; Duration: 45 min; Data volume: 243 Mbits.\\

-- prefer run above limb on AR 11087; EIS pointing: x = R_Sun + 15 arc sec, y = 0\\

}}

%%center

||Study ID||Acronym|| ||

!!E. Test and Calibration Studies \\

!test-01 => EIS slit calibration

  – Young ([pyoung@ssd5.nrl.navy.mil|mailto:pyoung@ssd5.nrl.navy.mil])\\

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{{

-- Obtain co-spatial data in the 1", 2" and 40" slits for various calibration tests (slit widths, tilt, intensity calibration)\\

-- run CALIB_slit_slot_v2 (ID # 389)\\

-- 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_v2 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: 35 Mbits\\

-- duration: 56m.\\

}}

%%center

||Study ID||Acronym|| ||

__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]) __\\

At line 152 added 97 lines

__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 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 \\

__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.\\

At line 953 removed 55 lines

!test-02 => EIS velocity calibration

  – Kamio ([kamio@linmpi.mpg.de|mailto:kamio@linmpi.mpg.de])\\

%%roundedCorners-yyyy-E3F0EE-808080

{{

-- 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.\\

}}

%%center

||Study ID||Acronym|| ||

!test-03 => EIS Slot Deconvolution Test

  – Sun ([js2@mssl.ucl.ac.uk|mailto:js2@mssl.ucl.ac.uk])\\

%%roundedCorners-yyyy-E3F0EE-808080

{{

-- Develop method to deconvolve EIS slot data\\

-- Two studies:\\

   * js2_decon_slot_sc_LT (ID # 429): data volume: 3.71Mbits; duration: 1m51s\\

   * js2_decon_ref_vel_LT (ID # 430): data volume: 87.87Mbits; duration: 47m37s\\

-- Instructions for planner:\\

   - Run study (ID # 429) first, then consecutively run study (ID # 430), then run study (ID # 429) again.\\

   - It's prefer that the slot study (ID # 429) repeats a few times, \\

     eg. study429 (x6), study430 (x1), study429 (x6) \\

-- Target: \\

   - simple active region; \\

   - FoV to cover AR edge to detect outflows; \\

   - both rasters to have identical pointing\\

-- Run during SAA-free interval preferred\\

}}

%%center

||Study ID||Acronym|| ||

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

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