HOP 0435

HINODE Operation Plan (HOP)

accepted on

17-feb-2022

HOP No.

HOP title

HOP 0435

Observations of a coronal hole during PSPs 11th encounter

contact person in HINODE team

name :

Savage, Watanabe, De Pontieu

e-mail :

sabrina.savage[at]nasa.gov, watanabe.tetsuya[at]nao.ac.jp, bdp[at]lmsal.com

abstract of observational proposal

Main Objective: Support PSPs 11th encounter by performing a mosaic scan over a single coronal hole

Scientific Justification:
1 carrington observation before PSPs 11th encounter, there is a coronal hole right at the solar equator. If it persists, it will allow PSP to measure the plasma properties of a high-speed solar wind stream in its center close to the Sun for the very first time. These observations shall scan this coronal hole in supportof PSPs encounter.

request to SOT

SOT shall run IHOP 415:
SOT/SP shall perform a single fast scan over a region of 320”x164” within the coronal hole. Amount of data: ~1 Gigabit for the entire scan. Duration: ~1 hour. In case of insufficient telemetry for SOT, these scans can be skipped.

request to XRT

XRT shall run IHOP 415:
XRT shall take 512”x512” observations, alternating the thin-Be filter (exposure time: 32 seconds) and the Al-poly/Ti-poly filter (exposure time: 12 seconds), at a cadence of 4 minutes.

request to EIS

EIS shall run IHOP 415:
EIS shall scan the entire coronal hole including its nearby boundary region, using multiple tile windows of 130”x512”. The individual tile windows shall use the study definition CH_funnels+FIPv2, and be performed outside SAAs.
Size: ~37.5 Mbyte x n_tile_windows

Line list:
Line(s) Central wavelength (A)
S X 180.53
O VI 184.05
Fe XII 186.75
Fe XI 188.53
Fe X 189.87
S XI 191.27
Ca XVII 192.82
Fe XII 193.54
Fe XII 195.12
S VIII 198.55
Fe XIII 203.40
O V 249.29
He II 256.32
Fe X 257.75
Si X 261.04
S X 264.23
Mg VI 269.05
Mg VI 270.40
Si VII 272.65
Si VII 275.97
Mg VII 278.39
Mg VII 280.15
Fe XV 284.16

other participating instruments

IRIS requests:
IRIS shall run IHOP 415:
IRIS shall scan the entire coronal hole by multiple mosaic cells distributed over the coronal hole. The exact number of mosaic cells depends on the size of the coronal hole, but will be likely 3x3. The coordinates of each mosaic cell will be provided by the PI. The planner is free to choose one of the following observing IDs, depending on the downlink rate available:
3821854096 (Very large dense raster 131.7x175 400s Deep x 2 Spatialx2 Spectralx2 FUVx8) . Data rate: 0.6 Mbit/s.
3821834096 (Very large dense raster 131.7x175 400s Deep x 2 Spatial x 2, Spectralx1 FUVx8) Data rate: 1.0 Mbit/s.
3821754096 (Very large dense raster 131.7x175 400s Deep x 2 Spatialx1 Spectralx1 FUVx8) . Data rate: 1.97 Mbit/s.

Additional instrument coordination:
GST, DST

remarks

Dates: One to two days between February 22nd-26th. The exact dates still need to be specified to coordinate best with other observatories.

Time window: About 5 hours of observations between 16 UT and 23 UT, to be able to coordinate with GST and DST.

Target(s) of interest: Low-latitude coronal hole

Previous HOPs:
IHOP 415 and 416 . These observations have been taken during a larger coordinated observing campaign during PSPs 8th perihelion, and are currently analyzed.

Additional remarks:
We are aware of the actual Hinode issues, but hope that Hinode is up again in time for PSPs 11th encounter (February 22nd-26th, 2022.). We will also coordinate the observations with IHOP 408 and 409 (led by Kathy Reeves, Alphonse Sterling, and Kevin Reardon).