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The Multiview Observatory for Solar Terrestrial Science (MOST) is a comprehensive mission concept to understand the solar drivers and the heliospheric responses as a system, discerning and tracking three-dimensional magnetic field structures, both transient and quiescent, from the solar interior out to 1 au.

Three primary science questions for the MOST mission:

  • How do active regions evolve before and after emerging to the solar surface? Use Doppler measurements from L4, L5 and Sun-Earth line (GONG, HMI) and employ helioseismology techniques with larger range of ray paths to track subsurface signatures of active regions and derive physical properties of the convection zone (e.g., change in CZ thickness with solar cycle). Life cycle of active regions is important for polar field build up and solar dynamo. Distinguish different dynamo paradigms.

  • How do CME flux ropes accelerate, drive shocks, and evolve form near the Sun into the heliosphere? Track and characterize 3-D CME acceleration and the evolution of the CME-shock complex through the outer corona and young solar wind; determine forces acting on CMEs. Track the shock standoff distance and compression ratio between Sun and Earth and compare with those measured in situ; track flux ropes magnetized using flare reconnection flux derived from EUV post-eruption arcades and compare with in-situ flux ropes. Determine the relation between hot-channel flux rope and CME flux rope. Combine Faraday rotation measurements with heliospheric images to determine the magnetic structures far from the Sun. Radial and longitudinal spread of SEP events.

  • How do CIR magnetic fields evolve in the inner heliosphere and accelerate particles? Using type III storms, identify magnetic reconnection in the coronal hole - active region boundary. Determine if this reconnection provides seed particles to CIR particle accelerator by comparing storm and storm-free active regions. Track longitudinal evolution of CIRs from L5 to Earth to L4.

  • MOST will provide comprehensive imagery and time series data needed to understand the magnetic connection between the solar interior and the solar atmosphere. MOST will build upon the successes of SOHO and STEREO with new views and instrumentation and add new capabilities.

    The quad charts of the proposed instruments can be found in this page.

    The detailed information is found in HELIO 2050 Poster.

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    The final program is available here.

    Submitted abstracts are available here.


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    Meeting Registration and Abstract Submission will be closed on Nov 10, 2021.

    • Click here to register the meeting (required) and submit an abstract (optional).
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    Science Organizing Committee

    L. Jian (co-chair), NASA/GSFC
    T. Nieves-chinchilla (co-chair), NASA/GSFC
    S. D. Bale, Berkeley
    C. DeForest, SWRI
    M. I. Desai, SWRI
    L. Golub, CfA
    N. Gopalswamy, NASA/GSFC
    E. A. Jensen, PSI
    S. G. Kanekal, NASA/GSFC
    S. Krucker, Berkeley
    R. J. MacDowall, NASA/GSFC
    A. Pevtsov, NSO
    S. Yashiro, CUA

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