HOP list   Monthly Events

HINODE Operation Plan (HOP)

accepted on

26-oct-11


 HOP No.

 HOP title

HOP 0081

CORE (HOP0002) Polar Monitoring Campaign during the Solar Cycle

plan term

2008/09/20-2008/09/25
2008/10/22-2008/10/23
2008/11/20-2008/11/21
2008/12/19-2008/12/20
2009/01/28-2009/01/29
2009/02/19-2009/02/20
2009/03/16-2009/03/21
2009/04/13-2009/04/14
2009/05/23-2009/05/24
2009/06/22-2009/06/23
2009/07/31-2009/08/01
2009/08/30-2009/08/30
2009/09/13-2009/09/18
2009/10/30-2009/10/31
2009/11/27-2009/11/28
2009/12/25-2009/12/26
2010/01/29-2010/01/30
2010/02/21-2010/02/22
2010/03/18-2010/03/18
2010/03/20-2010/03/21
2010/03/23-2010/03/24
2010/03/26-2010/03/26
2010/05/07-2010/05/08
2010/05/27-2010/05/28
2010/06/16-2010/06/17
2010/07/24-2010/07/25
2010/08/28-2010/08/29
2010/09/27-2010/10/02
2010/11/04-2010/11/05
2010/12/03-2010/12/04
2010/11/04-2010/11/05
2011/01/07-2011/01/08
2011/02/04-2011/02/05
2011/03/04-2011/03/05
2011/03/22-2011/03/27
2011/04/22-2011/04/23
2011/05/27-2011/05/28
2011/06/06-2011/06/07
2011/07/03-2011/07/04
2011/07/29-2011/07/30
2011/08/26-2011/08/27
2011/09/21-2011/09/27
2011/11/04-2011/11/05
2011/11/25-2011/11/26
2011/12/08-2011/12/09
2012/01/27-2012/01/28
2012/02/24-2012/02/25
2012/03/22-2012/03/24
2012/05/25-2012/05/26
2012/06/22-2012/06/23
2012/07/22-2012/07/23
2012/09/06-2012/09/08
2012/10/24-2012/10/30
2012/11/28-2012/11/29
2012/12/08-2012/12/09
2013/01/09-2013/01/15
2013/02/06-2013/02/12
2013/03/03-2013/03/08
2013/04/10-2013/04/16
2013/05/15-2013/05/20
2013/06/12-2013/06/18
2013/07/09-2013/07/16
2013/08/06-2013/08/12
2013/09/08-2013/09/08
2013/09/09-2013/09/09
2013/10/08-2013/10/14
2013/11/06-2013/11/12
2013/12/06-2013/12/09
2014/01/09-2014/01/10
2014/02/06-2014/02/07
2014/03/05-2014/03/07
2014/04/08-2014/04/08
2014/04/10-2014/04/10
2014/05/06-2014/05/06
2014/05/08-2014/05/08
2014/06/06-2014/06/07
2014/07/08-2014/07/08
2014/07/10-2014/07/10
2014/08/12-2014/08/12
2014/08/14-2014/08/14
2014/09/07-2014/09/09
2014/10/14-2014/10/14
2014/10/16-2014/10/16
2014/11/11-2014/11/11
2014/11/13-2014/11/13
2014/12/07-2014/12/08
2015/01/18-2015/01/18
2015/01/19-2015/01/19
2015/02/11-2015/02/11
2015/02/13-2015/02/13
2015/03/04-2015/03/06
2015/04/07-2015/04/07
2015/04/09-2015/04/09
2015/05/12-2015/05/12
2015/05/14-2015/05/14
2015/06/05-2015/06/05
2015/06/07-2015/06/07
2015/07/09-2015/07/09
2015/07/11-2015/07/11
2015/08/09-2015/08/10
2015/09/07-2015/09/07
2015/09/09-2015/09/09
2015/10/06-2015/10/06
2015/10/08-2015/10/08
2015/11/03-2015/11/03
2015/11/05-2015/11/05
2015/12/06-2015/12/06
2015/12/08-2015/12/08
2016/01/05-2016/01/05
2016/01/07-2016/01/07
2016/02/09-2016/02/09
2016/02/11-2016/02/11
2016/03/04-2016/03/05
2016/03/06-2016/03/06
2016/04/12-2016/04/12
2016/04/14-2016/04/14
2016/05/03-2016/05/03
2016/05/05-2016/05/05
2016/06/05-2016/06/05
2016/06/08-2016/06/08
2016/07/05-2016/07/05
2016/07/07-2016/07/07
2016/08/16-2016/08/16
2016/08/18-2016/08/18
2016/09/06-2016/09/06
2016/09/08-2016/09/08
2016/10/08-2016/10/08
2016/10/10-2016/10/10
2016/11/05-2016/11/05
2016/11/08-2016/11/08
2016/12/05-2016/12/05
2016/12/07-2016/12/07
2017/01/10-2017/01/10
2017/01/12-2017/01/12
2017/02/06-2017/02/06
2017/02/09-2017/02/09
2017/03/04-2017/03/04
2017/03/05-2017/03/05
2017/04/08-2017/04/08
2017/04/11-2017/04/11
2017/05/04-2017/05/04
2017/05/07-2017/05/07
2017/06/06-2017/06/06
2017/06/08-2017/05/08
2017/07/04-2017/07/04
2017/07/06-2017/07/06
2017/08/08-2017/08/08
2017/08/10-2017/08/10
2017/09/06-2017/09/06

@ @

proposer

 name : Shimojo, Tsuneta, Ishikawa,Itoh, Kamio, Fujimura @  e-mail : shimojo[at]nro.nao.ac.jp

contact person in HINODE team

 name : Shimojo @  e-mail : shimojo[at]nro.nao.ac.jp

 abstract of observational proposal
Objectives:
1: To observe the evolution of the magnetic field distribution around the poles during the solar cycle.
2: To understand the relationship between photospheric magnetic field and the coronal structures (include the solar wind) around the poles.

Scientific Background:
The polar observations by SOT/SP revealed that there are many strong patchy magnetic poles around the poles. Such strong magnetic fields in the polar region may strongly relate with the dynamo and it is very important to observe the evolution of the magnetic field distribution for understanding the dynamo.
The strong patchy magnetic poles have the trumpet-like vertical magnetic structure. Although we think that the trumpet structures may relate with the fast solar wind, there are no coronal (X-ray/EUV) structures on most of the magnetic structures. To understand the fast solar wind, the relationship between photospheric magnetic fields and coronal structures in the polar coronal hole is very essential. During the polarity reversal, the opposite polarity magnetic field invade the polar region. At the time, the relationship between coronal activities/structures and photospheric magnetic field is very interesting for understanding the solar wind.

 request to SOT
For DSM
Day 1
E BFI G-band: FoV 221"x111", Binning: 2x2, Time resolution: 30 min,
     JPEG Quality: Q75 Note: One image per one observation period.
E NFI Na I: IVDG mode, FoV: 328h x 164h, Binning: 2x2, Time resolution: 5 min,
     JPEG Quality: Q75 Note: One image per one observation period.
E SOT-SP FoV 320h x 164h, Pixel size: 0.16h/pix, Binning: 1x1, Single side mode
 Exposure: 12.8 sec (16 Cycles), JPEG Quality: Q75, Data rate: >2280Mbits/map

Note: If the exposure time may cause the saturation, please decrease it.
Note: Since the data size of SP is very huge for the allocation data size of SOT, we can observe only one SP map during two days. It is OK.
Note: set margin factors to 1.4 for FG and SP

Day 2
EBFI G-band: FoV 221"x111", Binning: 2x2, Time resolution: 30 min,
    JPEG Quality: Q75, Data rate: 9 Mbits/h
ENFI Na I: IVDG mode, FoV: 328h x 164h, Binning: 2x2, Time resolution: 5 min,
    JPEG Quality: Q75, Data rate: 102 Mbits/h
ESP FoV 320h x 164h, Pixel size: 0.32h/pix, Binning: 2x2, Single side mode
 Exposure: 4.8 sec (6 Cycles), JPEG Quality: Q75, Data rate: 600Mbits/map
Note: The G-band images are used for mainly co-alignment. Please insert a G-band image when the observation starts.
Note: One map per one day.
Note: set margin factors to 1.4 for FG and SP

Day 3
The observation plan for Day 3 is same as Day 2. The target is different. In March, the target is the north-polar region. In September, the target is the south-polar region.

For FSM
EBFI G-band: FoV 221"x111", Binning: 2x2, Time resolution: 30 min,
    JPEG Quality: Q75, Data rate: 9 Mbits/h
ENFI Na I: IVDG mode, FoV: 328h x 164h, Binning: 2x2, Time resolution: 5 min,
    JPEG Quality: Q75, Data rate: 102 Mbits/h
E SP FoV 320h x 164h, Pixel size: 0.32h/pix, Binning: 2x2, Single side mode
Exposure: 4.8 sec (6 Cycles), JPEG Quality: Q75, Data rate: 600Mbits/map
Note: The G-band images are used for mainly co-alignment. Please insert a G-band image when the observation starts.

Note: One map per one day.

 request to XRT
<Al/poly>
FoV 384 pix x 384 pix, Binning: 1 x 1, Time resolution: < 1 min.
Exposure time: 16.34 sec, JPEG Quality: Q75
Data rate: 7.6 Mbits/h (one image/1 min)

<G-band>
FoV 384 pix x 384 pix, Binning: 1 x 1, Time resolution: 30 min

Note1: Please shift the center of images to the center of SOT image using the SOT-XRT offset written in Shimizu et al., 2007.

Note2: The G-band images are used for mainly co-alignment. Please insert a G-band image when the observation starts.

Note3: The plan for FSM is same as that for DSM.
<G-band>
FoV 384 pix x 384 pix, Binning: 1 x 1, Time resolution: 30 min

Note1: Please shift the center of images to the center of SOT image using the SOT-XRT offset written in Shimizu et al., 2007.

Note2: The G-band images are used for mainly co-alignment. Please insert a G-band image when the observation starts.

Note3: The plan for FSM is same as that for DSM.

 request to EIS
EIS Study ID: 304 SK_CH_DIAG_320x284

This study performes a large scan for coronal holes with low temperature lines (log T < 6.2).
It is designed for polar monitoring campaign with SOT/SP measurement of magnetic fields.

TARGET        : Coronal hole
EXPOSURE TIME : 50s
RASTER        : Scanning
SLIT          : 1"
STEP_SIZE     : 1"
FOV           : 320"x384"
SPECTRAL WIND.: 12
DATA COMP.    : JPEG90
RASTER DURATON: 4h50m
DATA VOLUME   : 150 Mbits
LINES         : Fe VIII, Fe X, Fe XI, Fe XII, Fe XIII,
              He II, O V, Mg VI, Mg VII, Si VII, Si X

POINTING:
Polar coronal hole with fixed pointing.
Make sure to cover SOT FOV and the solar limb.

INSTRUCTION TO PLANNERS:
Start this study at the beginning of SAA free period (roughly 10-15UT)
The later part may coincide with a short SAA.

WARNING:
Large data volume (150 Mbits), duration 4h 50m. Avoid SAAs as much as possible (SAA degrade data compression factors and mutilate the data)

FOV: 320" x 384" exposure: 50sec duration: 4h50m compression: JPEG90 data volume: 132Mbits

lambda Te Ion
184.54 6.0 Fe X
186.60 5.8 Fe VIII
186.88 6.1 Fe XII
192.83 6.1 Fe XI
192.90 5.4 O V
195.12 6.1 Fe XII
202.04 6.2 Fe XIII
248.46 5.4 O V
256.32 4.7 He II
261.04 6.0 Si X
268.99 5.7 Mg VI
275.35 5.8 Si VII
278.39 5.8 Mg VII
280.75 5.8 Mg VII

Density diagnostics O V 192.90 / 248.46 (10-13) Mg VII 278.39 / 280.78 (8-12) Fe XII 186.88 / 195.12 (8-12)

Note: The plan for FSM is same as that for DSM.


 other participating instruments

 remarks
1. Based on the polar condition of the Sun, HOP81 requests the following items to Hinode operation.
  Although the flare activity becomes active, please keep the routine of HOP81 gOne HOP81 observation per one month.h

2. Except June and December, HOP81 can accept changing the observing day from the planned day.

3. During the eclipse season, the SOT-SP observes the polar region without the RESUME command.

4. In June and December, Hinode performs the HOP81 observation within - 7/+ 3 days from the requested day.

- 2011: 7 June & 8 December
- 2012: 6 June & 8 December
- 2013: 7 June & 8 December

----

1: Deep Scan Mode (DSM) around the poles
The number of times: 2 times per a year when the pole is watched from the earth.

Time period: 3 days within one month around the core week.
We request 7.5 hours including the SAA free period (roughly 10--15UTC).

Target: March: South Pole (Day 1,2) + North Polar Region (Day 3)
       September: North Pole (Day 1,2) + South Polar Region (Day 3)

Flexibility: The observations can be shifted by } 2--3 days relative totheir scheduled days
            if active region observations are needed.

Pointing: March // Day 1(0, -940), Day 2(0,-900), Day 3, (0, 900)
                September // Day 1(0, 940), Day 2(0, 900), Day 3, (0, -900)
         >>When CP fixs the coordinates of the pointing for HOP81,
           CP must apply the SOT-UFSS offset to the coordinates.<<

2: Fast Scan Mode (FSM) for the polarity reversal monitoring
The number of times: 1 time per a month except March and September

Time period: 2 days per one observation

Time window: 6 hours per day. We request the SAA free period (roughly 10--15UTC)

Target: North Polar Region (Day 1) and South Polar Region (Day 2)

Flexibility: Except June & December, the observations can be shifted by about 1 week relative to
                  their scheduled days if active region observation are needed.

Pointing: Day 1(0, 900), Day 2(0,-920)
         >>When CP fixs the coordinates of the pointing for HOP81,
           CP must appl

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