Conveners
Poster Session 6.2
- Ramon Oliver (University of the Balearic Islands)
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Julia Thalmann (University of Graz, Austria)08/09/2021, 11:00Session 2 - The Solar Atmosphere: Heating, Dynamics and CouplingPoster
In this ISSI-supported series of studies on magnetic helicity in the Sun, we implement and systematically compare different magnetic helicity calculation methods on high-quality solar magnetogram observations. We apply finite-volume, discrete flux tube (in particular, connectivity-based), and flux-integration methods to magnetogram series from Hinode's Solar Optical Telescope. Finite-volume...
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Kilian Krikova (Rosseland Centre for Solar Physics, ITA, University of Oslo)08/09/2021, 11:13Session 2 - The Solar Atmosphere: Heating, Dynamics and CouplingPoster
The Hydrogen Balmer lines show enhanced emission in various energetic phenomena in the solar atmosphere. For example, the H$\alpha$ line shows complex wing enhancements in the Ellerman Bomb phenomenon. Recently, Ellerman bombs have been detected in the H$\beta$ line at high number densities in the Quiet Sun and it was concluded that these mark the ubiquitous presence of small-scale magnetic...
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Korsos Marianna08/09/2021, 11:26Session 2 - The Solar Atmosphere: Heating, Dynamics and CouplingPoster
The magnetic helicity slowly and continuously accumulates in response to plasma flows tangential to the photosphere and magnetic flux emergence normal to it, it into the solar atmosphere. Analyzing the evolution of magnetic helicity flux at different atmospheric heights is key for identifying its role in the dynamics of ARs. The 3D magnetic field is obtained from PF extrapolations in order to...
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Dr Kostadinka Koleva (Space Research and Technology Institute, Bulgarian academy of Sciences)08/09/2021, 11:39Session 2 - The Solar Atmosphere: Heating, Dynamics and CouplingPoster
We present the first results from the investigation of a filament eruption (FE) and associated ribbon flare, occurring in the southern solar hemisphere on 2021 May 9. Before the eruption, the filament was located in a plage region, close to the disk center and lay along the S-shaped magnetic polarity inversion line, i.e. it represented a sigmoid filament. The filament began to rise slowly at...
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Dr Kostas Tziotziou (IAASARS, National Observatory of Athens, Greece)08/09/2021, 11:52Session 2 - The Solar Atmosphere: Heating, Dynamics and CouplingPoster
Ubiquitous small-scale vortical motions that are generated on the solar surface at intergranular lanes by the turbulent dynamics of solar convection, are observed in the quiet-Sun atmosphere with dynamic timescales of a few minutes. Most of these convectively driven vortex motions harbour magnetic fields whose forced photospheric rotation often leads to the formation of magnetic tornadoes that...
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Luc Rouppe van der Voort (Rosseland Centre for Solar Physics, University of Oslo)08/09/2021, 12:05Session 2 - The Solar Atmosphere: Heating, Dynamics and CouplingPoster
Ellerman bombs are regions with enhanced Balmer line wing emission and mark magnetic reconnection in the deep solar atmosphere in active regions and quiet Sun. Recent observations suggest that Ellerman bombs are more prevalent than thought before. We aim to determine the occurrence of Ellerman bombs in the penumbra of sunspots. We analyze high spatial resolution observations of sunspots in...
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Maciej Zapiór (Astronomical Institute Czech Academy of Sciences)08/09/2021, 12:18Session 2 - The Solar Atmosphere: Heating, Dynamics and CouplingPoster
Single fluid MHD theory is not able to fully describe observed plasma motions in solar prominences. Several authors (see Khomenko et al. (2016), Anan et al. (2017), Wiehr et al. (2019)) observed discrepancy between Doppler velocity measured in different spectral lines of ions and neutrals. However they give different answers to the question if motions of the plasma lead to decoupling of ions...
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