Schematic diagram of the cruise science case studies as related to the instrument devoted for the investigation and to possible multi-spacecraft measurements.

    Adapted from Mangano et al., Space Sci. Rev., 2021.

     

    CRUISE science What should be measured Instrument When? Necessary constellation?
    Small-scale solar wind turbulence: how they evolve with radial distance B field, high-res (min – sec – or less) MPO-MAG radial alignment, behind shock waves, within planetary magnetic sheats
    Small-scale solar wind structures: magnetic holes, what is their relation to mirror mode waves B field, high-res (min – sec – or less) MPO-MAG behind shock waves, within planetary magnetic sheats
    Large-scale solar wind structures: transient CMEs, ICMEs properties and evolution, interaction of multiple CMEs, CME+SIR interaction B field, 5-min – hourly MPO-MAG (particle detector of MMO-MPPE is NOT directly exposed to solar wind), SIXS-P radial alignment
    SEPs: acceleration fluxes of energetic particles (energy spectrum, pitch angle distribution), magnetic field configuration SIXS-P, MPO-MAG, BERM radial alignment + widely separated longitudes, close to shock waves
    SEPs: transport (cross-field diffusion?) fluxes of energetic particles (energy spectrum, pitch angle distribution), magnetic field configuration SIXS-P, MPO-MAG, BERM alignment along Parker spiral + widely separated field lines
    Large-scale solar wind structures: background solar wind, CIRs – radial evolution, backmapping fluxes of energetic particles (energy spectrum, pitch angle distribution), B-field, 5-min – hourly MPO-MAG, SIXS-P radial alignment
    CIRs – magnetic sector boundaries fluxes of energetic particles (energy spectrum, pitch angle distribution), B-field, 5-min – hourly MPO-MAG, SIXS-P same Parker field line
    CIRs – 3d evolution fluxes of energetic particles (energy spectrum, pitch angle distribution), B-field, 5-min – hourly MPO-MAG, SIXS-P latitudinal separation
    Comets – water production rates in the hydrogen coma (+OH) – Panstarss EUV (Lyman-alpha) + FUV PHEBUS IMEX will calculate when each target intersects PHEBUS FOV
    Comets – particles in the cometary trails UV, dust impact flux PHEBUS, MMO-MDM constantly
    Dust – interplanetary dust distribution in the inner solar system dust impact flux within the MDM FOV MMO-MDM (surrounded by MOSIF, but detection possible through MOSIF aperture) constantly
    Solar corona studies – density fluctuations, velocity of SW radio occultation measurements, TEC MORE BC + Akatsuki, occultation
    General relativity tests time delay of radio signals MORE superior conjunction
    Galactic Cosmic Rays MCS emission due to bombardment (local radiation background) MGNS, SIXS-P constantly
    Gamma-ray bursts: localize the sources flux density MNGS constantly
    Gamma-ray of solar flares flux density MNGS constantly