HOP 0427

HINODE Operation Plan (HOP)

accepted on

26-aug-21

HOP No.

HOP title

HOP 0427

Emergence, evolution, and structure of the network magnetic field: Photosphere, chromosphere, and transition region

proposer

name :

Hansteen, Gosic, De Pontieu, Sainz-Dalda

e-mail :

viggoh[at]gmail.com, gosic[at]baeri.org, bdp[at]lmsal.com, asainz.solarphysics[at]gmail.com

abstract of observational proposal

Main Objective: Finding the correspondence between the structure of the network photospheric/chromospheric magnetic field and the topology and evolution of the atmosphere above.

Scientific Justification: This programme is designed to observe the chromospheric network over periods of time long enough to follow the evolution of the network magnetic field and the possible capturing of ephemeral active regions.

At the same time to observe any related changes in coronal structures, particularly above the network cell boundaries. Using SST, IRIS, Hinode/EIS and SDO AIA data will allow the diagnosis of emerging flux into the upper atmosphere through the entire solar atmosphere. The pointing of this HOP will be driven and requested by observations made with the SST that will attempt to find network intense regions where ephemeral active regions may occur.

request to SOT

Fast-map during observations start to show the pattern of strong network flux elements in its FOV (~164"x164" or as large as possible) - the main instrument is EIS, the fast map with SOT is a good backup/supplement to the SST field measurements.

request to XRT

Deep integrations with the cooler filters (thin-Al-mesh or thin-Al-poly) for QS observations. FoV is larger than 128"x128", and temporal cadence of 90 sec to match SST observations as closely as possible.

request to EIS

Rapid slot context image ST_ID: 354, FOV: 488"x488", Exp.: 10s, Dur.:3m30s PRY_slot_contextLITE. Followed by raster FOV: 60"x160", Exp.: 120s, Dur.:1h4m21s, dhb_atlas_120m_30" ST_ID: 468

other participating instruments

IRIS requests:
This proposal has been chosen and selected by the IRIS team.
High-telemetry OBSID:
3620506848 | Large sparse 32-step raster 31x120 32s Si IV Mg II h/k Mg II w De | 167.51 |281.46 | 1.14 | 5.2+/-0.1 | 168+/-0 | 0.0+/-0.0 | 20.9+/-0.0 | 20.9+/-0.0 | 20.9+/-0.0

Low-telemetry OBSID:
3620606849 | Very large sparse 32-step raster 31x175 32s Si IV Mg II h/k Mg II | 163.58 |141.25 | 0.58 | 5.1+/-0.1 | 164+/-0 | 0.0+/-0.0 | 20.4+/-0.0 | 20.4+/-0.0 | 20.4+/-0.0

Additional instrument coordination:
SST - IRIS team at LMSAL.

remarks

Dates: September 11 - September 24 is the time LMSAL has access to the SST. 2-3 observations days
during this period. It is not necessary for observations to be on consecutive day, but this will be decided by which targets are available/interesting to the LMSAL/SST team in the days before the observations.

Time window: The minimum is 1 hour in the range 7 UT - 11 UT, several hours is preferable. Short interruptions are allowed.

Target(s) of interest: Quiet Sun (strong) network, on disk.

Previous HOPs:
No prior HOP submission.