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HINODE Operation Plan (HOP)

accepted on

23-feb-2017


 HOP No.

 HOP title

HOP 0336

Cycle 25 Bright Points

plan term

2017/03/06-2017/03/06
2017/03/13-2017/03/13
2017/03/20-2017/03/20
2017/03/27-2017/03/27
2017/04/03-2017/04/03
2017/04/10-2017/04/10
2017/04/17-2017/04/17
2017/04/24-2017/04/24
2017/05/01-2017/05/01
2017/05/08-2017/05/08
2017/05/15-2017/05/15
2017/05/21-2017/05/21
2017/05/29-2017/05/29
2017/06/05-2017/06/05
2017/06/12-2017/06/12
2017/06/19-2017/06/19
2017/06/26-2017/06/26
2017/07/03-2017/07/03
2017/07/10-2017/07/10
2017/07/17-2017/07/17
2017/07/24-2017/07/24
2017/07/31-2017/07/31
2017/08/07-2017/08/07
2017/08/14-2017/08/14
2017/08/21-2017/08/21
2017/08/28-2017/08/28

@ @

proposer

 name : Bryans, Centeno @  e-mail : pbryans[at]ucar.edu, rce[at]ucar.edu

contact person in HINODE team

 name : Savage @  e-mail : sabrina.savage[at]nasa.gov

 abstract of observational proposal
Main Objective:
To find the magnetic and chromospheric signatures of the onset of cycle 25.

Scientific Justification:
Small magnetic features and coronal bright points have been shown to indicate the bands of activity associated with the solar cycle. The precise location of these bands is important for predicting the timing of solar minimum and, more generally, the long-term variability of the Sun.

Recently, the onset of the activity bands of solar cycle 25 have been observed at high latitudes (McIntosh et al. 2014, McIntosh & Leamon 2017). These authors found a periodicity within the activity bands that is on the order of the solar rotation rate, but offset between the north and south.

To date, the signatures of solar cycle 25 have been measured by SDO/AIA and SDO/HMI. However, these instruments do not allow us to measure the spectral signatures of these features nor their vector magnetic field. Hinode SP measurements will give us high resolution vector field data, and IRIS will show the chromospheric spectral signature of the bright points.

McIntosh, S. W., et al., 2014, ApJ, 792, 12
McIntosh, S. W. & Leamon, R. J., 2017, ApJL, Submitted

 request to SOT
Modification from original request:
During eclipse season, please run a full width, full height fast map at the same pointing, instead of the normal map. This should run in 2 or 3 orbits for redundancy. Full height is requested because SOT offsets in Y are large and slightly uncertain during eclipse season.

Half of the FOV has been determined to be sufficient.  Request changed to one full resolution, full width, half slit (512 px), normal map centered at longitude 0W and latitude 42.5N for the northern hemisphere.

Request to add observations in the Southern hemisphere, with a map of the same size, centered at longitude 0W and latitude 47.5S.

NOTE TO COs:  During Focused Mode, northern hemisphere observations take priority over the southern hemisphere when the number of tracking curves is limited.

Original request:
For each observation we require two full resolution, full width, half slit (512 px), normal map.
Each map:
FOV: 320 x 82
Data: 2000x(512x112x1x4)
Duration 166 minutes
Data volume 1.140 Mbits
The total volume estimate is ~1.14 gigabit per map (~2.3 gigabit per observation)
The total time estimate is 166 minutes per map (~5.5 hours per observation)
We request weekly observations in the Northern hemisphere around 42.5 degrees latitude (so that the SP slit spans between 40 and 45 degrees) and ~300h at each side of the central meridian. A similar observing program is desired for the southern hemisphere, at an average latitude of 47.5 degrees from the equator.
Northern hemisphere: two points at (-150, 655) and (150, 655).
Southern hemisphere: two points at (-150, -685) and (150, -685).

 request to XRT
single filter Al_poly long/short pairs
384x384 FOV

 request to EIS
HOP177_CH - cadence 1 hour

 other participating instruments
IRIS Requests:
Each observation requires 4 pointings for each raster. Northern hemisphere pointings: [-150, 640], [-50,640], [50, 640], [150,640]. Southern hemisphere pointings: [-150, -695], [-50, -695], [50, -695], [150, -695].

Timing should follow the Hinode pointing as closely as possible, but at the least we request all rasters span no more than 12 hours. Avoid SAAs if possible.

High data rate:
3620258076 | Large dense 320-step raster 105.3x120 320s Deep x 8 FUV spectrally | 2993.20 | 3785.93 | 0.9 | 9.4+/-0.1 | 2993+/-0 | 37.4+/-0.0 | 37.4+/-0.0 | 37.4+/-0.0 | 37.4+/-0.0

Low data rate:
3620108076 | Large dense 320-step raster 105.3x120 320s Deep x 8 Spatial x 2, Spe | 2932.08 | 1268.12 | 0.3 | 9.2+/-0.1 | 2932+/-0 | 36.7+/-0.0 | 36.7+/-0.0 | 36.7+/-0.0 | 36.7+/-

 remarks
Requirements and desires: weekly observations of a high latitude band in the northern hemisphere are required. A similar set of observations in the Southern hemisphere is desired.

Time window: coordination with IRIS is desired, within the same 24 hour interval is required. Short interruptions (eclipse season or other) are allowed.

Target(s) of interest: High latitude bands (600h around the central meridian) of quiet Sun in the Northern (between 40 and 45 degrees) and the Southern (between 45 and 50 degrees) hemispheres.

Additional Remarks:
This IHOP is concerned with detecting the bright point signals of solar cycle 25. These bright points have been shown to be periodic with a period close to the rotation rate, and confined to narrow latitude bands. Therefore, we request the observations be performed ~weekly at specific locations in the northern and southern hemispheres, on precise dates selected by the proposer. The periodicity and locations of the BPs differs between the northern and southern hemispheres. Our primary science goal is to measure the northern hemisphere. If time/telemetry allows, we wish to measure the southern hemisphere separately.

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