Study 000461:

ACRONYM: HH_Flare+AR_180x152

This study is to hunt for various flow structures in solar flares.
It can also be used as a study for active regions.

Target: Active region / Flare

Type: scanning raster
Field of view: 180"x152"
Exposure time: 9.0 s
Slit: 2"
Step size: 6"
Raster Duration: 6m5s
Data volume: 3.6 Mbits (JPEG75 - default), 4.4 Mbits (JPEG85)
             See note in instruction to planners section

Lines:
------
O V     : detection of TR response at the impulsive phase
Fe X    : hunting of reconnection inflow
Fe XII  : hunting of reconnection inflow
Fe XIV  : study of normal coronal loops with density sensitive pairs
Fe XV   : study of flare loops in a cooling phase
Fe XVI  : study of flare loops in a cooling phase
Fe XVII : study of flare-loop heating and reconnection outflow
Ca XVII : study of reconnection outflow
Fe XXIII: study of loop-top hot region and reconnection outflow
Fe XXIV : study of loop-top hot region and reconnection outflow

The non-thermal velocity component in solar flares is studied by
combinations of Fe XXIII ad Fe XXIV.

Pointing:
---------
Active region including those with the potential for flaring

Instruction to planners:
------------------------

1) Center the raster on an expected site in an active region.
2) When flare hunting, adjust the raster repeat for a maximum
  run-time possible, accounting for the TM constraint.

** Note** : The default compression is JPEG75. For a short time scale runs, the
compression parameter should be changed to JPEG85.

Study 000458:

ACRONYM: CAM_FLARE_DIAG

Perform a high-cadence (2m 47s) small (60"x120") sparse (3")
raster over a small active region  with the 2" slit and 5s exposures.


TARGET        : Small Active region
EXPOSURE TIME : 5s
RASTER        : Scanning
SLIT          : 2"
STEP_SIZE     : 3"
FOV           : 60"x120"
DATA COMP.    : JPEG90
RASTER DURATON: 2m 45s
DATA volume   : 2.56 Mbits
LINES         : Mg V, Si VII, Fe XI, Fe XIII, Fe XIV,
                Fe XVI, Ca XV, Fe XVII, Fe XXIII, Fe XXIV.

POINTING:
---------

The core of an active region observed on-disk, not far from
Sun centre.

INSTRUCTION TO PLANNERS:
------------------------

The active region should have displayed signs  of activity.
Avoid large AR likely to produce X-class flares.
The study should be run continuously for about 10 hours or more.
(230 raster repetitions totals to about 590 Mbits and 10.7 hours).

Study 000472:

ACRONYM: FLAREDOP_EIS

A sit-and-stare study for flares designed to investigate time
differences between brightenings observed in different emission lines,
and resolve the evolution of density, bulk flows and non-thermal
motions at high cadence.

TARGET: flaring active region
EXPOSURE TIME: 10s
RASTER: sit-and-stare
NO. OF EXPOSURES: 300
DURATION: 1 hour
SLIT LENGTH: 184"
COMPRESSION: DPCM
DATA VOLUME: 168.5 Mbits

Pointing:
---------

The target should be a flaring active region either on the disk or at
the limb. The slit should be placed on the location within the active
region that is most likely to flare.

Instructions to planners
------------------------

1) Place the context study PRY_slot_context_v3 on the timeline first
2) Then append the FLAREDOP_EIS study. Adjust The number of repeats to fill
   the available time slot.
3) Then append the context study PRY_slot_context_v3 to FLAREDOP_EIS
   to complete the sequence.

Study 000464:

ACRONYM: QUB_HI-CAD_FLARE_2S-EXP_104"x104"

This is a fast-raster study designed to support ground-based observations from ROSA by
measuring plasma dynamics and density changes during solar flares over a broad range of
temperatures. It is also a potential candidate study to use in response to the EIS flare
trigger.

TARGET: Flare
EXPOSURE TIME: 2s
RASTER: Scanning
SLIT: 2"
STEP SIZE 2"
FOV: 104"x104"
DURATION: 3.5 mins
LINES: He II, O V, O VI, Mg VI, Mg VII, Fe VIII, Fe X, Fe XI, Fe XII (dens. sens. pair),
Fe XIII (dens. sens. pair), Fe XIV (dens. sens. pair), Fe XV, Fe XVI, Fe XVII, Ca XV
(dens. sens. pair), Fe XXIII, Fe XXIV

VOLUME: 18 Mbits (x16 repeats = 300 Mbits per hour = 1200 Mbits for 4 hours)

POINTING:
--------

A flare producing active region (C-class flares or greater) as announced by the Max
Millennium Chief Observers in their daily messages. The region can be anywhere on the
solar disk.

INSTRUCTIONS TO PLANNERS:
------------------------

The scheduling of the proposed HOP is determined by the seeing conditions at Sunspot,
NM at the time of the observing campaign (currently scheduled for 9-14 July 2011,
inclusive). Typically, seeing conditions are optimal during the first few hours after
sunrise (~14:00-18:00 UT). We therefore request that EIS continuously raster over the
chosen Target of Opportunity (ToO) during this 4 hour period, whether on the disk or
at the limb.

Study 000450:

ACRONYM: eis:eitwave_obssns

HOP-180 SNS study

This study is intended to be run in areas located close to the outer edges of active regions
in order to detect the evolution of propagating EIT waves. The main aim is to study the
plasma motions below the EIT wave fronts together with plasma density diagnostics.

TARGET:              Surroundings of active regions
EXPOSURE TIME:       45
RASTER:              Sit-and-stare
SLIT:                2"
NUMBER OF EXPOSURES: 40
FOV:                 2"X512"
RASTER DURATION:     33m 11s
Volume:              33Mbits

Pointing:
---------

Areas located not more than 150" - 200" from the outer edge of an active region.

Use/Instructions to planners:
-----------------------------

Run the observation in the following order:

1) Run eis:eitwave_context. No. of raster repeat is 3

2) Run eis:eitwave_obssns. Optimum number of raster repeat is 8 (or as many as possible)
   - total duration: 4h25m28s

3) Run eis:eitwave_context. No. of raster repeat is 3

Please chain the three runs.

Observation run-time: 4h37m34s
Total data volume: 270 Mbits (8 SNS runs of eis:eitwave_obssns)

INSTRUCTION TO PLANNERS:

- 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 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_v4 (ID #489); Study B, repeating for up to 5 hrs
- run PRY_slot_contextLITE (ID #354); Study A
- run Hot_loop_osci_2_v4 (ID #490); 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)

Note: This observation requires running three studies:

ACRONYM:           PRY_slot_contextLITE (study ID=354)  
ACRONYM:           Hot_loop_osci_1_v4 (ID 489)
ACRONYM:           Hot_loop_osci_2_v4 (ID 490)

This study is designed to detect Doppler shifts and intensity 
variations mainly in hot coronal and flare emission lines. 

The observation consists of three studies. Study A is using slot-40 
to quickly scan whole AR for obtaining a context image. 
Studies B  and C are using the repeated short raster in high 
cadence (< 2 min) to search for flare-excited oscillations in hot 
coronal loops, such as standing slow mode waves as observed by 
SUMER. It also includes a  pair of density sensitive Ca XV lines 
for density diagnostics. The study is designed to detect 
oscillations and waves in coronal loops of T = 1-10 MK.

#Study A: Context study
ACRONYM:           PRY_slot_contextLITE
TARGET:		   AR loops on the limb  
EXPOSURE TIME:     10 s
RASTER:            Scanning
SLOT:              40"
STEP SIZE:         32"
FOV:               488"x488"
RASTER DURATION:   3m29s
REPEAT TIMES:      1

#Study B:
ACRONYM:          Hot_loop_osci_2_v4
TARGET:           AR loops on the limb
EXPOSURE TIME:    10 s
RASTER:           Scanning
SLIT:             2"
STEP SIZE:        4"
FOV:              38"x200"
RASTER DURATION:  2m27s
REPEAT TIMES:     1 
N_LINES           8
       Ca XV, Ca XVII, Fe XII, Ca XV, Fe XVI, Fe XXIII, Fe XVII and Fe XV

#Study C:
ACRONYM:          Hot_loop_osci_2_v4
TARGET:           AR loops on the limb
EXPOSURE TIME:    10 s
RASTER:           Scanning
SLIT:             2"
STEP SIZE:        4"
FOV:              22"x200"
RASTER DURATION:  1m37s
REPEAT TIMES:     1
N_LINES           8
       Ca XV (181.99), Ca XVII, Fe XII, Ca XV (200.98), Fe XVI, Fe XXIII, 
       Fe XVII and Fe XV

Pointing:
--------
Flare-productive active region on the limb, better located at the 
eastern limb.
For Study A, the 1/3 FOV is on the disk and 2/3 FOV off the limb.
For Studies B and C, the slit center position is set about 
30-50 arcsec above the AR on the limb (close to the core of the AR)

Use/Instructions to planners:
-----------------------------
i)   Run Study A (ID=354) first to get a context image of AR. 
ii)  Repeat Study B (Hot_loop_osci_1_V4) for about 5 hours, and then
     run Study A again for a context image.  
iii) Repeat Study C (Hot_loop_osci_2_V4) for about 5 hours, and then
     run Study A again.
iv)  Stop or repeat ii) and iii) once more if possible. 

Note: The above 10 hrs observations are better not interrupted.
We hope to make observations of at least 10 hrs every day
(better 20 hrs/day if allowed), and last for 4-5 days so we can 
track the AR passing from behind the limb to the front disk to 
catch loops of different sizes and different parts of loops
during this period. 

Warning:
--------
The sequence above should be run uninterrupted (preferably use chained 
studies), i.e. append to highlighted entry.

Study 000473:

ACRONYM: CORE_FLARE_TR120X120

Study is focussed on low temperature transition lines. 
It could be run 180 times for a total of about 10.5h (610Mb). 
For comparison, the HH_flare_raster_v2 can be run 127 times for 12.7h (600 Mb). 
Compared to many other studies, e.g. HH_flare_raster_v2, this study includes 
the He II and a good range of TR lines.

It has the Fe XIV density diagnostic, and possibly O V.

EXPOSURE TIME : 4s
SLIT          : 2"
STEP_SIZE     : 4"
FOV           : 120"x120"
DATA COMP.    : JPEG85
RASTER DURATON: 3m 5s
DATA volume   : 3406 kBits (18.4 kBits/s)

Pointing
-----------
Point at the core of an active region observed on disc within a few days of 
central meridian passage.

Instructions to Planners
----------------------------------
Study should be run continuously for about 10 hours or more on a flare-active AR.
----------------------------------------------------------------------------------

Study 000482:

ACRONYM: SI_Venus_slit_v2

Study will be used to clearly detect outflow or eruptive phenomena.			       
Observe limb AR likely to flare.		            
Aim is to study reconnection outflow including non-equilibrium plasma and 
to measure the difference between T (ion) and T (electron).

EXPOSURE TIME:	100s
SLIT:		2”
STEP SIZE:	Sit-and-Stare
FOV:		2” x 256”
DATA COMP:	DPCM – use e.g. JPEG85 if TLM is limited
DURATION:	2m 9s
DATA VOLUME:	7.5 Mbit

Pointing
Beyond the limb (~ 100 arc sec) sit-and-stare observation is required

Instructions to Planners
1. Obtain context image with PRY_slot_contextLITE. 
2. Run for as long as allowed by available telemetry
3. Avoid eclipses.

Study 000498:
ACRONYM: PRY_flare_1
Study is intended to take spectra of flare kernels that appear during the rise phase of 
a flare. 
The parameters have been chosen based on lessons learnt from the data set analyzed by 
Young et al. (2012, arXiv:1212.4388).

EXPOSURE TIME:		10.4s									  
SLIT:			1”
STEP SIZE:		4”
FOV:			40”x120”
DATA COMP:		JPEG85
RASTER DURATION: 	2m
DATA VOLUME:		1.3 Mbit
DATA RATE:		7.2 kb/s

Pointing       
------------
Point at flare kernel 


Instructions to Planners                              
--------------------------------------

1. A potential site for flare kernels should be chosen. Kernels appear near sunspots,
but not within the umbra. A magnetically complex region close to the neutral line but near 
sunspots is appropriate. The active region should be on the disk and preferably close to 
the central meridian.

2. A context raster (e.g., PRY_slot_context_v3) should be run before and after the sequence of 
PRY_flare_1 rasters.