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« Previous Version 3 Next » 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]


Required observations:

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


Other constraints:

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