Observed spectral profiles of emission lines from the corona are found to have widths exceeding the thermal line width. To investigate the physical mechanism behind this, we run a 3D MHD model of a single loop in which we partially resolve the turbulent motions within the loop and the substructures that form self-consistently in response to the driving by magneto-convection in the photosphere. The loop is modelled as a straightened-out magnetic flux tube with a shallow, self-consistently evolving convection zone layer at each end. This allows us to include the response of the chromosphere to heating events. From the model we synthesize spectral profiles of emission lines. We investigate the strongest heating events in the coronal loop and discuss the relation between footpoint motions and

The magnetic field of solar-type stars is generated and sustained through an internal dynamo process. This process is mostly determined by the combined action of turbulent convective motions and differential rotation. It can sometimes lead to magnetic cyclic variabilities, like the 11-years solar cycle. Evidence of magnetic cycles have been detected for other solar-type stars as well, ranging from a few years to a few tens of years. How are these cycles controlled? Observations and stellar evolution models show that solar-like stars spin-down during their main-sequence. In parallel, numerical simulations of these stars show that different regimes of differential rotation can be reach and are characterized with the Rossby number. Read more at https://espos.stream/2022/12/01/Noraz/.

Vincenzo Andretta, Mariarita Murabito

The Dark Halos (DHs) are regions of reduced emission in the neighborhood of solar active regions (ARs). Since their discovery (Hale & Ellerman, 1903), DHs have been called with various names, the first one being circumfacules (Deslanders, 1930), as they were first identified in the chromosphere as faint areas surrounding plages in the Ca II K-line, and later also in the Ca II 8542 Å line (D’Azumbuja, 1930). Bumba & Howard (1965) proposed that the Ca II circumfacules are composed of dark features corresponding to dark Hα fibrils, and this suggestion was supported by different authors (e.g. Rutten et al. 2007, Pietarila et al. 2009). Read more at https://espos.stream/2023/02/16/Lezzi/.

The solar atmosphere undergoes several changes during the solar cycle. Those changes can be identified by observing several solar features and their respective dynamics, which can be observed in many different wavelengths, and by analyzing the variations in the total solar irradiance. The latter is characterized by an increase in the total solar irradiance during the solar maximum and a decrease in the decay phase. In this talk, we will present the intensity variations of the Mg II h&k lines emission peak, observed by IRIS, under quiet sun conditions close to the disk center over the decaying phase of the solar cycle. The observed variations will then be interpreted and put in the context of the solar atmospheric physical conditions.