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ESPOS videos
European Solar Physics Online Seminars
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https://espos.stream
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Field of research
Natural Sciences (Astrophysics and Astrononmy)
Email
shahin.jafarzadeh@astro.uio.no
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Sunspot MHD simulations: subsurface structure and penumbral filament formation | Mayukh Panja
Natural Sciences (Astrophysics and Astrononmy)
451 views
Date of upload:
19.05.2021
Co-author:
Caption:
Penumbral filaments do not form naturally in MHD simulations of sunspots. This is typically circumvented by modifying the top boundary: the field is made 2-3 times more horizontal than a potential field configuration. In this talk, I will explore the possibility that penumbral filament formation is governed by the subsurface structure of sunspots. We conducted a series of numerical experiments where we used flux tubes with different initial curvatures to study the effect of the fluting instability on the subsurface structure of spots using the MURaM code. We find that the curvature of a flux tube indeed determines the degree of fluting the flux tube will undergo—the more curved a flux tube is, the more fluted it becomes. In addition, sunspots with strong curvature have strong horizontal fi
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Mode coupling at the transition region and the validity of line-tied boundary conditions | Alex Prokopyszyn
Natural Sciences (Astrophysics and Astrononmy)
403 views
Date of upload:
19.05.2021
Co-author:
Caption:
In this seminar, we aim to show why Fast/Alfvén waves couple at the solar surface. We will also show that the polarisation of the waves changes upon reflection at the solar surface. Finally, we will test the validity of line-tied boundary conditions for highly phase-mixed Alfvén waves. For most parameters, line-tied boundary conditions provide a good approximation. However, for highly phase-mixed waves, the coronal transverse length scales can be shorter than the corresponding parallel length scales in the chromosphere. In that case, we find that the line-tied model produces unphysically large boundary layers. Hence, we have the counter-intuitive result that the length scales parallel to the solar surface play a key role in determining the validity of line-tied boundary conditions.
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Investigating small solar flares with NuSTAR | Kristopher Cooper
Natural Sciences (Astrophysics and Astrononmy)
1030 views
Date of upload:
20.05.2021
Co-author:
Caption:
Small, highly frequent flares are thought to contribute to heating the Sun’s atmosphere, particularly in active regions. This impulsive energy release would heat plasma >5 MK and accelerate electrons, producing weak thermal and non-thermal signatures that could be observed by a very sensitive X-ray telescope. No such solar telescope exists currently so we use the Nuclear Spectroscopic Telescope Array (NuSTAR), an astrophysical X-ray telescope, with focusing optics imaging spectroscopy providing a unique sensitivity for observing the Sun above 2.5 keV. In this seminar, I will present an overview of the discoveries from NuSTAR solar observations where decreasing solar activity between cycle 24 and 25 has allowed GOES sub-A class microflares to be observed regularly within, and small brighten
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The Kelvin-Helmholtz Instability in the Fan-spine Magnetic Topology in the Solar Corona | Sudheer K. Mishra
Natural Sciences (Astrophysics and Astrononmy)
398 views
Date of upload:
20.05.2021
Co-author:
Caption:
Using multi-wavelength imaging observation obtained from the Atmospheric Imaging Assembly (AIA) onboard Solar Dynamics Observatory (SDO), we study the evolution of Kelvin-Helmholtz (K-H) instability in a fan-spine magnetic topology. This fan-spine configuration is situated near the Active Region 12297 and is rooted in a nearby sunspot. The two layers of the cool plasma flows lift up from the fan plane in parallel and interact with each other at the maximum height of the elongated spine in the lower corona. The first layer of the plasma flow (F1) moving with a slow velocity (5 km/s) reflected from the spine’s field lines. Subsequently second layer of plasma flow (F2) with impulsive velocity (114-144 km/s) interacts with the first layer at the maximum height and generating the shear motion ,

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