L_BOTH_LRES_MCAD_Pole-to-Pole - Solar Orbiter

L_BOTH_LRES_MCAD_Pole-to-Pole

General description

This SOOP is designed to be used as a whole- or half-orbit Synoptic campaign that scans the Sun from one high latitude to the other (therefore mainly to be used later in the NMP at min inclination of 15º). Close to the higher latitude windows, we get a radial sweep at nearly constant latitude for in-situ.

This SOOP resembles very much the L_FULL_LRES_MCAD_Coronal-Synoptic (currently deprecated) but this time SPICE is necessary as well.

The SOOP can be scheduled after every Venus GAM during the fast transition from neg-to-pos(pos-to-neg) high latitude

 

Default SOOP duration: 10 days

Pointing requirements: mainly disk centre, with disk pointing necessary to accommodate SPICE rasters and PHI/HRT when inclination is not sufficient enough to cover the poles.

Triggers: TBD

 

Instrument

Mode

Comment

Metis

One of METIS standard modes to observe large scale coronal structures: GLOBAL or LT-CONFIG

Could do a slight offpoint without switching Metis off, depending on distance.

Latitudinal scan of solar corona for morphology, and F-corona.
Cosmic Rays scan out-of-ecliptic

SPICE

SPICE Composition Mapping raster

SPICE scans many latitudes during the SOOP : large swath around the sun

magnetic field spiral less curved at higher latitudes:
SPICE naturally closer to connection point.

EUI

FSI Synoptic mode (S) with FSI

10 min cadence

PHI

FDT in general though HRT could be high resolution, medium cadence (TBC) 

At higher latitudes, point to the poles for polar magnetic field observations.

 

SoloHI

SoloHI synoptic Operations

 

STIX

N/A

 

EPD

Normal + Burst Mode

 

MAG

Normal + Burst Mode

 

RPW

Detection Mode

Burst Triggers Active

SWA

Normal + Burst Mode

 

 

 

SAP objective

Target

Duration

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

Operational constraints 

Additional comments

1.1.3.2 How does the Sun's magnetic field link into space?

 

 

After Venus GAM, when scanning pole to pole

 

 

4.2 What are the properties of the magnetic field at high solar latitudes?

 

 

 

 

 

 

 

 

 

 

 

 

Original SOOP proposers

D. Spadaro, A. Vourlidas, A. Giunta, D. Williams

 
 
 
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