COSMOS Science - Bepicolombo YSSG-CS - Cosmos

Science - Bepicolombo YSSG-CS

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.

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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

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