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HINODE Operation Plan (HOP)

accepted on


 HOP No.

 HOP title

HOP 0366

Coordination with Parker Solar Probe

plan term


@ @


 name : Warren @  e-mail : harry.warren[at]nrl.navy.mil

contact person in HINODE team

 name : Warren @  e-mail : harry.warren[at]nrl.navy.mil

 abstract of observational proposal
Main Objective:
Observations of solar wind source regions observed by Parker Solar Probe

Scientific Justification:
Parker Solar Probe (PSP) will provide unprecedented observations of the conditions in the inner heliosphere. Remote sensing observations from EIS, XRT, SOT, and IRIS are needed to help identify and understand the solar origin of the plasma that PSP is observing.

 request to SOT
Limb: If the PSP's magnetic footpoint on the disk is on or close to limb, give all telemetry to EIS & XRT for their limb observations of a reasonable duration.

Coronal Hole: If the footpoint is on disk in quiet sun or CH or CH boundary: fast map, full FOV, at start and end of encounter (avoiding SAA); also one in the middle of the encounter, if telemetry permits. Deep mode fast maps (longer integration time for greater sensitivity) can be run if the SAA-free time is long enough to include them (~3 hours).

Active Region: If the footpoint is on or close to active region or plage: more or less continuous full-FOV fast maps, with FOV chosen to cover AR and the surroundings, especially on the side where the footpoint is predicted to be.

Far side: No observations

 request to XRT
Limb w/AR: High cadence (10s) 512x512 Be-thin, 384x384 FOV OK for telemetry
Limb wo/AR: CME watch Be-thin 60s cadence
Coronal Hole: CME watch Al-poly 60s cadence
Active Region: High cadence (10s) 512x512 Be-thin, 384x384 FOV OK for telemetry
Far side: Run HOP 349 (disk-center, full-disk mosaics)

 request to EIS
For on disk targets: Run a full-disk slit scan (see IHOP 344 for details) approximately two days before the encounter begins. IRIS full-disk scan is not required.

Limb: Run study DHB_007 using HOP130 limb pointings (6T, 1T&B, and 11B) once each day; approximately 4 hours
Coronal Hole: Repeat study DHB_007 over target
Active Region: Repeat HPW021VEL260x512v1 over target
Far side: No observations

 other participating instruments
Limb: Alternating orbits of two-step raster
High data rate version: 3680109414  |  Very large coarse 2-step raster 2x175 2s  Si IV  Mg II h/k Deep x 8 S
Low datarate version: 3600109414  |  Very large coarse 2-step raster 2x175 2s  Si IV   Mg II h/k Deep x 8 S

Coronal Hole or Active Region: Very large raster  
High data rate version: 3620259477  |  Very large dense 320-step raster 105.3x175 320s  Si IV   Mg II h/k Dee
Low datarate version: 3600109477  |  Very large dense 320-step raster 105.3x175 320s  Si IV   Mg II h/k Dee

Far side: No observations

COROTATION PERIOD FOR ORBIT 1 - Duration [days] 1.85
2018-NOV-02 08:22:45 to 2018-NOV-04 08:25:29

Target: PSP may map to source regions that are on the disk, at the limb, or on the far side. Disk source regions could be coronal holes or active region outflow regions. Observations for all scenarios are described here.
For disk targets, SOT, XRT, EIS, and IRIS observations should be run as continuously as possible during the encounter. Breaks for participation in previously scheduled HOPS are ok.
For limb targets, at least one set of XRT and EIS observations should be taken on each day of the encounter. Again, continuous observations are preferred.
Note that target information requires using models to map the PSP location back to the solar surface. At present it is not clear who will provide these calculations.

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