Conveners
Poster Session 5.3
- Mats Carlsson (Rosseland Centre for Solar Physics, University of Oslo, Norway)
Computing synthetic spectra from model atmospheres is a fundamental tool to understand the formation of complex spectra and help guide observations. Forward modelling using 3D MHD simulations is becoming widespread, and with it the need to efficiently carry out radiative transfer computations. This is particularly acute for the solar chromosphere, where out of equilibrium conditions dictate...
In the corona, the (apparent) thermal equilibrium arises from a delicate balance between radiative losses and some unknown heating mechanism(s). The effect of these heating and cooling mechanisms varies with the plasma parameters, such as density, temperature and potentially magnetic field strength. Meanwhile, slow magnetoacoustic waves can perturb the density and temperature of the hosting...
We aimed to study the damping mechanism of the large-amplitude longitudinal oscillations (LALOs) in solar prominences hidden by numerical dissipation. We performed the numerical simulations of LALOs using the 2D magnetic configuration that contains the dipped region. After the prominence mass loading in the magnetic dips, we triggered LALOs perturbing the prominence mass along the magnetic...
We aim at setting and driving 3D magneto-hydrodynamic simulations of the Sun with photospheric magnetogram observations to get a better understanding of the heating mechanism and energy dissipation in the solar corona and thus aiming to move a step closer towards the long-standing solar coronal heating problem. There are already some models that study coronal heating using different heating...
Despite the recent lull in solar activity, the community has seen new observational discoveries and new advances in the modelling of the umbra. The presence of coronal and transition region downflows have been repeatedly reaffirmed, their role in the typical umbral upper chromosphere remaining unconstrained. A connection between small-scale dynamic fibrils and umbral flashes has been...
Solar prominences are cold, dense structures nested in the hot and tenuous solar corona, made up of thread-like fibrils. Embedded in the magnetically dominated, dynamic corona, prominences also exhibit oscillatory behavior [1]. Understanding the interplay of mechanisms that cause prominence and thread oscillations provides important insight into the solar corona. Numerical simulations have...
