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16th European Solar Physics Meeting

6–10 Sept 2021
Online
Europe/Rome timezone

Session

Poster Session 10.5

9 Sept 2021, 11:00
Online

Online

Conveners

Poster Session 10.5

  • Alessandro Bemporad (Istituto Nazionale di Astrofisica (INAF))

Presentation materials

Zoom link
  1. 268. Initiation And Early Kinematic Evolution Of Solar Eruptions
    Dr Xin Cheng (Nanjing University)
    09/09/2021, 11:00
    Session 4 - From Radio to Gamma Rays: Near-Sun Manifestations and Triggering of Solar Flares and Coronal Mass Ejections
    Poster

    We investigate the initiation and early evolution of 12 solar eruptions and conclude: (1) The early evolution of all events consists of a slow-rise phase followed by a main-acceleration phase, the height-time profiles of which differ markedly and can be best fit, respectively, by a linear and an exponential function. This indicates that different physical processes dominate in these phases,...

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  2. 293. Variations of field-aligned currents and ionospheric trough during September 2017 geomagnetic storm
    Ms Agata Chuchra (Space Research Centre of Polish Academy of Sciences)
    09/09/2021, 11:13
    Session 5 - Solar-Terrestrial Relations, Solar Wind, Space Weather and Space Climate
    Poster

    Geomagnetic storms are the temporary variations of the Earth’s magnetic field, induced by the coronal mass ejection (CME) or the high-speed solar wind stream (HSSWS) with a magnetic field directed oppositely to Earth's. The powerful energy injection into the magnetosphere through the magnetic reconnection during such events directly affects the auroral region of the Earth’s ionosphere, where...

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  3. 444. Two-fluid simulations of Rayleigh-Taylor instability in a magnetized solar prominence thread: Magnetic structure formation
    Vyacheslav S. Lukin (National Science Foundation)
    09/09/2021, 11:26
    Session 3 - Fundamental Plasma Processes in the Solar Atmosphere: Magnetic Reconnection, Waves, Emission, Particle Acceleration
    Poster

    We describe turbulent magnetic structure formation via driven magnetic reconnection in the non-linear phase of a Rayleigh-Taylor Instability (RTI) in a solar prominence supported by sheared magnetic field. Solar prominences are formed by partially ionized plasma with inter-particle collision frequencies generally warranting magnetohydrodynamic treatment. In this work, we explore the...

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  4. 518. Magnetic flux emergence and solar eruptions
    Vasileos Archontis (University of St. Andrews)
    09/09/2021, 11:39
    Session 2 - The Solar Atmosphere: Heating, Dynamics and Coupling
    Poster

    A key process which leads to eruptive activity in the Sun, is the emergence of the magnetic flux from the solar interior to the solar surface and into the outer solar atmosphere. We present results from 3D numerical simulations, which show the onset of eruptive jets and CME-like structures in emerging flux regions. We discuss the physical connection between jets and large-scale eruptions and...

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