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16th European Solar Physics Meeting

6–10 Sept 2021
Online
Europe/Rome timezone

Session

Poster Session 10.3

9 Sept 2021, 11:00
Online

Online

Conveners

Poster Session 10.3

  • Georgia Tsiropoula (National Observatory of Athens)

Presentation materials

Zoom link
  1. 431. Wave propagation in a sunspot atmosphere at high resolution
    Diego Prado Barroso (Instituto Nacional de Pesquisas Espaciais (INPE))
    09/09/2021, 11:00
    Session 3 - Fundamental Plasma Processes in the Solar Atmosphere: Magnetic Reconnection, Waves, Emission, Particle Acceleration
    Poster

    Waves and oscillatory phenomena have been observed in the solar atmosphere as mechanisms that transfer energy through its different heights, from the photosphere to outer layers. Hence, they are considered as one of the main processes responsible for heating the upper solar atmosphere. This study aims to detect and characterize various MHD wave modes in a sunspot atmosphere (i.e., active...

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  2. 340. Time signatures of quasi-periodic fast-propagating waves in the solar corona
    Dr Dmitrii Kolotkov (University of Warwick)
    09/09/2021, 11:13
    Session 3 - Fundamental Plasma Processes in the Solar Atmosphere: Magnetic Reconnection, Waves, Emission, Particle Acceleration
    Poster

    Observations of fast magnetoacoustic wave trains, also known as quasi-periodic fast-propagating (QFP) waves, at large heights of the Sun’s corona suggest that these waves can travel long distances from the excitation locations. We study characteristic time signatures of fully developed fast magnetoacoustic wave trains guided along the magnetic field by dense plasma slabs in the linear regime....

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  3. 297. KAPPA package - the latest update
    Elena Dzifčáková (Astronomical Institute of the Czech Academy of Sciences, Fricova 298, 251 65 Ondrejov, Czech Republic)
    09/09/2021, 11:26
    Session 3 - Fundamental Plasma Processes in the Solar Atmosphere: Magnetic Reconnection, Waves, Emission, Particle Acceleration
    Poster

    The presence of non-Maxwellian distributions in the solar corona is supported by many theoretical calculations and several successful spectroscopic diagnostics from UV and EUV lines in the flares, solar corona and transition region. The kappa-distributions or any other distributions exhibiting high-energy tails can also be expected as a result of particle acceleration processes by nanoflare...

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  4. 453. How does numerical diffusion affect high resolution two-fluid simulations of magnetized turbulence?
    Elena Khomenko (Instituto de Astrofisica de Canarias)
    09/09/2021, 11:39
    Session 3 - Fundamental Plasma Processes in the Solar Atmosphere: Magnetic Reconnection, Waves, Emission, Particle Acceleration
    Poster

    Numerical magnetohydrodynamic (MHD) simulations have become a dominant tool in studies of the non-linear dynamics of solar plasma, such as shock formation, instabilities or magnetic reconnection. Many of the numerical codes used for such simulations have to deal with the stability issues caused by unresolved motions on scales below the grid scale. For that, several algorithms have been...

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  5. 436. Simulations of the Biermann battery mechanism in two-fluid partially ionised plasmas
    David Martínez Gómez (Instituto de Astrofísica de Canarias)
    09/09/2021, 11:52
    Session 3 - Fundamental Plasma Processes in the Solar Atmosphere: Magnetic Reconnection, Waves, Emission, Particle Acceleration
    Poster

    In the absence of an initial seed, the Biermann battery term of a non-ideal induction equation acts as a source that generates weak magnetic fields. These fields are then amplified via a dynamo mechanism. The Kelvin-Helmholtz instability is a fluid phenomenon that takes place in many astrophysical scenarios and can trigger the action of the Biermann battery and dynamo processes. In this talk,...

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