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A new era of solar physics commences with observations of the quiet Sun using the 4-metre Daniel K. Inouye Solar Telescope/Visible Spectropolarimeter (DKIST/ViSP). We present full-Stokes observations taken during DKIST’s cycle 1, in the Fe I 630.1/630.2 nm lines, allowing us to examine small-scale magnetism in the photosphere. We use the Stokes Inversion based on Response functions (SIR) code to invert the Fe I line pair. We reveal the existence of a serpentine magnetic element for the first time. A statistical analysis is undertaken, comparing inversions of DKIST data with Hinode data. A novel machine learning technique is used to characterise and contrast the shapes of circular polarisation signals found in the ground-based and space-based data, and synthetic observations produced from MANCHA simulations are used to aid our understanding of the differences between datasets.
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Interactions between the highly dynamic atmosphere of our Sun and the magnetic fields permeating its atmosphere give rise to a wide variety of magnetohydrodynamic (MHD) wave phenomena. Combining observations of MHD waves with an applied mathematical description of the waveguides has allowed researchers to determine elusive physical quantities of the solar atmosphere using the methods of solar magneto-seismolgy. The ‘classical’ models utilised in this discipline describe straight, symmetrical MHD waveguides (slabs or flux tubes). A recent direction of research has focused on wave propagation in asymmetric slab waveguides, where the direction of propagation was strictly parallel to the magnetic field lines within the slab. Here, some further results are presented in the case when a magnetic slab is embedded in a non-magnetic, asymmetric environment, and the direction of propagation is allowed to deviate from the internal magnetic field lines of the slab. We describe this non-parallel wave propagation in various analytical approximations relevant to solar atmospheric waveguides (thin and wide slabs, low-beta plasmas) and present numerical solutions to the full dispersion relation to expand on our findings.
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The solar radiation in the cores of the Mg II h & k spectral lines strongly correlates with solar magnetic activity and global variations of magnetic fields with the solar cycle. This work provides a data-driven model of temporal evolution of the solar full-disk Mg II h & k profiles over the solar cycle. Based on selected 76 IRIS near-UV full-Sun mosaics covering almost the full solar cycle 24, we find the parameters of double-Gaussian fits of the disk-averaged Mg II h & k profiles and a model of their temporal evolution parameterized by the Bremen composite Mg II index. The Markov Chain Monte Carlo algorithm implemented in the IDL toolkit SoBAT is used in modeling and predicting temporal evolution of the Mg II h & k peak-to-center intensity ratio and the Bremen Mg II index. The relevant full-disk Mg II h & k calibrated profiles with uncertainties and spectral irradiances are provided as an online machine-readable table. To facilitate utilization of the model corresponding routines, written in IDL, are made publicly available at GitHub.
Co-authors: Stanislav Gunár (The Czech Academy of Sciences, Czech Republic), Pavol Schwartz (Slovak Academy of Sciences, Slovakia), Petr Heinzel (The Czech Academy of Sciences, Czech Republic; University of Wrocław, Poland), Wenjuan Liu (The Czech Academy of Sciences, Czech Republic)
Web announcement: https://espos.stream/2024/03/21/Koza/
Zoom link: https://zoom.us/j/165498165
(Meeting ID: 165 498 165)
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The solar atmosphere is filled with clusters of hot small-scale loops commonly known as Coronal Bright Points (CBPs). These ubiquitous structures stand out in the Sun by their strong X-ray and/or extreme-ultraviolet (EUV) emission for hours to days, which makes them a crucial piece when solving the solar coronal heating puzzle. Here we present a novel 3D numerical model using the Bifrost code that explains the sustained CBP heating for several hours. We find that stochastic photospheric convective motions alone significantly stress the CBP magnetic field topology, leading to important Joule and viscous heating concentrated around the CBP’s inner spine at a few megameters above the solar surface. We validate our model by comparing simultaneous CBP observations from SDO and SST with observable diagnostics calculated from the numerical results for EUV wavelengths as well as for the Halpha line using the Multi3D synthesis code.
Co-authors: Fernando Moreno-Insertis, Klaus Galsgaard, Kilian Krikova, Luc Rouppe van der Voort, Reetika Joshi, and Maria Madjarska
Web announcement: https://espos.stream/2024/04/04/Nobrega-Siverio/
Zoom link: https://zoom.us/j/165498165
(Meeting ID: 165 498 165)
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I briefly review some methods and measurements of elemental abundances in the solar atmosphere, with emphasis on the transition region and corona. Some limitations in the methods, in the modelling of the spectral line intensities, and in the observations are discussed. Examples from the X-rays, the EUV, the UV, the visible and near-infrared are presented. A significant improvement in the modelling some of the ions is being made available with CHIANTI version 11. All the observations indicate that the solar corona has photospheric abundances and that the hot 3 MK active region cores have stable enhancements of a factor of about 3.2 in the ratios of low to high-FIP elements. A lot of uncertainties and puzzles still exist, requiring further analyses and, more importantly, future instrumentation.
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We present the results of coordinated observations of the Swedish 1-m Solar Telescope with Solar Orbiter that took place from October 12th to 26th 2023. The campaign resulted in 7 datasets of various quality. The observational programs were adjusted to the seeing conditions. The observations cover two active regions and a coronal hole. We focus on the morphology and evolution of several targets that are observed from two vantage points. We share the lessons we learned and give an outline of our plans for October this year and the support we could give during remote sensing windows 16 and 17.
Web announcement:
https://espos.stream/2024/05/02/Danilovic/
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Zoom link: https://zoom.us/j/165498165
(Meeting ID: 165 498 165)
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