Page tree

Versions Compared

Key

  • This line was added.
  • This line was removed.
  • Formatting was changed.

...

1.2.2.5 Magnetic reconnection in the chromosphere, the transition region and the corona, driven by magnetic field evolutionary processes. Explore reconnection signatures such as brightenings (Harrison et al., 1997), flows and jets (Innes et al., 1997) and plasma evaporation (Klimchuk, 2006). Reconnection between small closed loops and open structures supplying energy to the nascent solar wind in the form of waves and turbulent flows (Tu et al., 2005). [perihelion]

  

Link to 1.1.4.1 Reconnection

This page should be moved under 1.1.4.1 but I keep it here until the meeting.


Operational requirements table: This table will be filled before the SAP meeting (16-17 November), please come back later!

 

Requirement
YES / NO / Not required / MAYBE / GOOD TO HAVE / NUMBERS
Remarks
Duration of the observations ? 
Perihelion Yes, but not only 
RS window Yes 
High latitude Not required 
Solar cycle dependence No 
Radial dependence No 
Linkage science  NoUnless for the solar wind part already included in objectives 1.1
Multiple orbits Good to have 
Far side observations No 
Earth observations No 
EMC Quiet No 
SPP No 
Instruments  SoloHI, EUI, PHI, METIS

RS only

 


Required observations:

  • SoloHI: Contribute (mode: turbulence), no min. obs time, all distances, w/EUI-METIS-SPICE-PHI.
  • EUIEUI synoptic mode (S)
  • PHI

    HRT medium  resolution data

    Requirement

    FOV [pixels]

    1024 x 1024

    Parameters

    Ic, B, γ, φ

    duration

    4 days

    cadence

    1/(5 min)

    N orbits

    4

    solar distance

    <0.5 AU

    PHI operating mode

    2

    co-ordination

    ?

     

     

  • METIS
        • Measurement of the solar wind outflow velocity gradient in the outer corona, to localise regions of energy deposition, via Doppler dimming of the HI Lyα intensity in the field of view 1.5-2.9 degrees. Measurements of the brightness fluctuation spectra to identify waves contribution to acceleration in the context of the coronal magnetic field topology.
        • Products:
          • Global maps of outflow velocity in corona.
          • Global maps of electron density in corona.
          • Brightness fluctuation spectra.
        • Modes:
          • WIND (min. obs time 2 hr, data volume ≤ 300 Mb)
            Repeated each half a day in one observation window. 
          • MAGTOP (min. obs time 1 d, data volume ~ 3.5 Gb), preferably at perihelion.
          • FLUCTS (min. obs time 1 hr, data volume  ~ 2 Gb) at perihelion. 
        • Other instruments: PHI, EUI, SPICE, SoloHI, EPD, MAG, RPW, SWA.

Duration:

Other constraints: