We envision realistic, 3D models of prominences, simulated far into the turbulent regime and plan to make direct contact with modern turbulence studies. We are working on coronal rain simulations at extreme resolutions, and are investigating the intricacies of linear waves in plasmas and how these connect to prominence dynamics.
Our grid-adaptive, massively parallel software MPI-AMRVAC allows us to identify and predict detailed solar prominence and coronal rain aspects at extreme resolutions. These are supplemented with MHD linear eigenspectrum studies using Legolas, our new, modern linear MHD solver.
A dedicated team effort embedded within the Centre for mathematical Plasma-Astrophysics at KU Leuven and led by prof. Rony Keppens sets forth to guide, interpret and confront solar prominence activity.
Unraveling prominence secrets
How, where and why does the million degree solar corona spontaneously form these gigantic structures? What causes finestructure throughout the prominence body? How do they relate to coronal rain? What is the role of solar tornadoes often found at their feet?
Latest updates on the PROMINENT front
Solving a century-old question in Solar Physics
Rendering the successful simulation of a fully 3D solar filament/prominence, down to scales of ~20 km, using MPI-AMRVAC.
Using MPI-AMRVAC, we performed a 2.5D MHD simulation to investigate the formation and evolution of the coronal rain phenomenon.
We performed a 2.5D flare simulation from pre-flare phase all the way into the gradual phase to study the formation of coronal rain in post-fflare loop.
MHD workshop at Leiden Lorentz Center.
Novel results from applying Legolas to a self-consistent solar atmosphere model.
We show that condensation can happen inside post-flare loop without background heating with a test.
Postdoc in numerical solar physics research.
MPI-AMRVAC is successfully deployed to study the formation and evolution of a prominence in a 2.5D translationally-invariant setup.
Read up on the launch of the new Legolas code, a novel tool for MHD spectroscopy.