R_BOTH_HRES_HCAD_Filaments - Solar Orbiter

R_BOTH_HRES_HCAD_Filaments

General description

Description copied from the SAP paper:

This SOOP is intended to study the structure and dynamics of filaments at high spatial resolution. It supports both high and low cadence, depending on structural or dynamic aims. For the highest spatial sampling it is recommended for use during perihelion and will potentially be used in quadrature with Earth for coordinated stereoscopic observations with DKIST and other Earthbased (e.g. SST, GST, NVST, Gregor, ALMA) or near-Earth observatories and instruments. The default SOOP duration is one hour for telemetry reasons since EUI/HRI will operate at medium cadence (10–60 s), but other instruments will observe for a longer period, such as Metis when off-pointing is not needed. SO/PHI/FDT observations will be taken for context and to facilitate extrapolations and SO/PHI/HRT at low cadence for magnetic stereoscopy. SPICE observes in the Dynamics mode with the raster centred at the filament. 

 

Flavour 1: Structure and dynamics of filaments

High resolution observations of Filaments (AR or QS) to study structure and dynamics. SOOP supports both high and low cadence, depending on structural or dynamic aims. Perihelion preferred. Can potentially be used in quadrature with Earth for coordinated observations with DKIST and other Earth-based observatories/instruments.

Prominence instance would be pointed towards the limb. Science goals include:

  • To better understand the formation and internal energy transport within solar prominences, including:
    • Small scale structure and (kinetic) flow and wave dynamics
    • Chromospheric and intra-prominence radiation pumping
  • To determine prominence composition so as to distinguish and bound possible prominence formation mechanisms
  • Estimate total CME mass and proportion of prominence material retained in ICMEs
    • Evaluate the column depth and composition

Pointing requirements: 

Filament instance: Preferably run on disk center, may be pointed off-limb (without Metis) 

Prominence instance:

  • Pointing at the limb, possibly in quadrature with Earth.
  • At least one instance at perihelion even if we are not in quadrature with Earth.

Target will need to be selected as close to observing time as possible.

Default SOOP duration: 1 hour for EUI. Will need to be longer for SPICE – 4-10 hours.

Triggers: Disabled

 

Flavour 2: Footpoint/endpoint of filaments

Objective: Coordinated observations of the footpoint/endpoint (not barbs) of a solar filament, at high resolution and relatively high cadence to simultaneously probe internal structure and dynamics of associated plasma. If orbit allows it, two separate observations of the target from e.g., 45 and 0 degrees (to the side and directly above from the perspective of Solar Orbiter) will provide stereoscopic information about internal structuring. 

Science goal is complimentary to the first two Science Activity Plans (SAPs) (Extention to 5.1: ‘Resolve fine structure of filaments’ & ‘Resolve dynamics of filament fine structure’), tailored for observations on-disk given experience gained post-launch.

Target: Primary target of interest is an ‘intermediate’ filament, with backup target of a polar crown filament. Quietest of visible filament footpoints/endpoints (not barbs). 

Duration & Opportunity: Two slots of two hours, first on approach and second at point closest to quadrature (+/- 10°) with Earth. 

Coordination: Coordination sought with as many Earth-based telescopes and platforms (GREGOR, DST, SST, DKIST, Hinode, IRIS) as possible, depending on timing. Given SPICE limitations on spectral and spatial resolution, IRIS and EIS are musts for optical depth information. Ideal case is to have coordination for both windows and identical instrumentation. Where this is not possible, priority is coordination during quadrature.

 

 

Observations requirement (baseline)

Filament (on disk)

Instrument

Mode

Comment

EUI

HRI in highest spatial resolution. EUV & LYA Quiet Sun modes (Q) or EUV & LYA Active Region modes (A), HIGH-MID CADENCE: 10-60 second. FOV: Full (no rebinning)

Will limit telemetry for entire orbit, therefore recommended to only run for 1 hour.

PHI

PHI science mode 2 (FDT)

Observations used for context and extrapolations.

SPICE

SPICE Dynamics mode. 8 spectral windows

Observation details as in SPICE Dynamics. Centre of raster at centre of EUI provided that filament is at centre of EUI FOV

Metis

GLOBAL Observing mode

Not a priority instrument, data is complimentary to other observations. Duration: 3 hours, first hour alongside EUI and remaining two after EUI has completed observing run.

 

Prominence (on the limb)

Instrument

Mode

Comment

SPICE

1 at the limb

Slit: 4”

Exposure time 90 s

96 exposures

FOV ~6.3x12.8’

Observation time about 2.4 hours/raster

 

Also smaller faster rasters for dynamics

 

90 s exposure reference spectrum (45 min)

 

Lines from both short and long wavelength range.

Lines selected for DEM and composition, especially using Long-wavelength detector. Lyman beta and gamma,  Continuum

 

 

EUI

High resolution field of view, mostly 174 Å.

3-5 sec cadence

 

FSI 304 or 171 at ~ 1mcadence for a longer period.

Adjust for telemetry

PHI

Magnetograms for context

 

 

Filament footpoints

Instrument

Mode

Comment

SPICE

MODE: SPICE_DYNAMICS

STEP SIZE: 4′′

ROW HEIGHT: 768

EXPOSURE: 19.7s

N EXPOSURES: 32

FOV: 128′′ X (12.8′?)

REPEATS: 8

MIRROR STEP TIME: 0.25

N PROFILES: 8

SLIT: SLIT 4

 

Fast scanning over the footpoint of a filament.

Needs multiple of 32 steps.

Instrument PSF is larger than 4′′, 8 pixels in spectral

Idea is to run over the filament footpoint with ‘as many repeats as possible’.

On-disk exposures to be refined.

(Taken from header of equivalent LTP17 SOOP)

SCIFlow: 39316.78 — 38.245 Mibytes

 

EUI

HRIEUV 171A (No Lyα)

Exposure: ∼3.6s +

Cadence: ∼5s

FSIEUV 171A + 304A

Cadence: ∼1m

(Taken from header of equivalent LTP17 SOOP)

FSI for context

EUVFlow: 1677721.6 — 1632 Mibytes

PHI

MODE: PHI_RAW_HRT_6

Cadence: 1.5min = 90s

 

Binning a possibility depending on overlap between

EUI and SPICE FOV. 

(Taken from header of equivalent LTP17 SOOP)

RAWFlow: 6717440 — 6534.375 Mibytes

Science objectives

 

SAP objective

Target

Duration

Opportunity
(e.g., orbital requirements, solar cycle phase, quadrature ...)

Operational constraints 

Additional comments

5.1 Additional Science Objectives of EUI

Resolve fine structure of filaments

Extension to 5.1.1 (Study the corona and its phenomena in a high spatial and temporal scale (active regions during flares or in quiescent conditions, coronal holes, quiet Sun).)

Quiescent Filament

≤ 1 hour

Perihelion for highest spatial sampling.

Observation with PHI is required, else co-observation with Earth magnetographs (DKIST, SDO/HMI, Hinode/SOTSP)

lower cadence (1 minute) observations by HRI Lyalpha and HRI EUV on EUI. Objective is to study the appearance of filament fine structure, extent of dips, curvature, angle of threads to PIL, etc.

5.1 Additional Science Objectives of EUI

Resolve dynamics of filament fine structure

Extension to 5.1.1 (Study the corona and its phenomena in a high spatial and temporal scale (active regions during flares or in quiescent conditions, coronal holes, quiet Sun).)

Quiescent Filament

≤ 1 hour

Perihelion for highest spatial sampling.

Observation with PHI is required if not observed from Earth side, else co-observation with Earth magnetographs (DKIST, SDO/HMI, Hinode/SOTSP)

Higher cadence observations (1-10s) using the HRI Lyalpha on EUI, HRI EUV lower cadence (1 minute), other instruments operate as normal. Objective is to study evolution of fine structure features, oscillations, counterstreaming, density, etc.

5.1 Additional Science Objectives of EUI

Better resolve connection of a quiescent filament host field to the photospheric network

Extension to 5.1.1 (Study the corona and its phenomena in a high spatial and temporal scale (active regions during flares or in quiescent conditions, coronal holes, quiet Sun).)

Quiescent Filament

≤ 1 hour

Perihelion for highest spatial sampling.

Observation with PHI is required if not observed from Earth side, else co-observation with Earth magnetographs (DKIST, SDO/HMI, Hinode/SOTSP)

High-mid cadence observations (10s-1m) HRI Lyalpha and low cadence HRI EUV (1 minute) EUI, other instruments operate as normal. Objective is to study location of rooting of filament field w.r.t flux rope, observations of material dynamics used in tandem with ex- trapolations.

5.1 Additional Science Objectives of EUI

Co-temporal observations of polar crown (PC) filament from SO and Earth.

Extension to 5.1.1 (Study the corona and its phenomena in a high spatial and temporal scale (active regions during flares or in quiescent conditions, coronal holes, quiet Sun).)

PC Filament

≤ 1 hour

Perihelion for highest spatial sampling, during period when SO is elevated (> 25 degrees latitude) w.r.t the ecliptic for observation of PC Filament from above. Quadrature with Earth for coordination with DKIST and other Earth-based observatories/instrumentation. Will likely be a goal for later in the mission due to latitude requirements.

Observation with PHI is required.

Mid cadence observations (1 minute) EUI, other instruments operate as normal. Objective is to observe the filament environment from Earth (cavity) vs. the environment from above with SO (filament channel). HRI EUV + HRI Lyalpha.

5.8 Additional Science objective of SPICE

 

5.8.1 Obtain spectral atlas of representative features in the solar atmosphere.

Target on limb or disk

~1 hr

Perihelion for highest spatial sampling.

 

Length will depend on exposure time needed

1.2.1.2 Energy and mass flux in the corona.

 

Active or quiescent prominence at or close to limb

 

 

Perihelion for highest spatial sampling.

 

This objective does not explicitly mention prominences, it should – they are a part of the whole coronal heating question

1.2.1.5 Determine whether coronal heating is spatially localized or uniform, and time steady or transient or impulsive for a wide range of magnetic loops with different spatial scales.

 

Active or quiescent prominence at or close to limb

 

Perihelion for highest spatial sampling.

 

 

2.1.1.1 CME initiation

 

Filament or prominence

 

Perihelion for highest spatial sampling.

 

This will be the result of luck unless a very long observing program is established

Instances run / planned

Prominence instance run as part of Nanoflare SOOP 15-April-2023

Science outcomes

 

Original SOOP proposers

Jack Jenkins, Lidia van Driel-Gesztelyi, David Long

Prominence instance added by Terry Kucera, Susanna Parenti, Jack Jenkins

 
 
 
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