Welcome to my website! This gallery contains some basic information on some current and past projects that I have done for the curious reader.
Synchrotron emission
Shocks can accelerate thermal electrons living in the magnetised intracluster medium. After these events, electrons start to lose energy. For example, they can lose energy as they spiral around magnetic field lines and emit radiation. If the intracluster medium is turbulent, this will be reflected in synchrotron emission.
Magnetised shock
The intracluster medium hosts magnetic fields. Merger events induce shocks that can amplify a tangled magnetic field through compression.
Shock dynamics
Previous merger events in galaxy clusters induce fluctuations in the intracluster medium. New merger events could induce low Mach number (weak) shocks. As they propagate through the already turbulent intracluster medium, there is extra shock-induced turbulence generated in the downstream of the shock.
Galaxy clusters merging
The largest gravitational systems in the Universe assemble through merger events. As they grow in mass (lower panels) there can be also magnetic amplification (upper panels) induced by compression and turbulence.
Center of mass
The center of mass of the forming galaxy cluster could vary in cosmological simulations since various components are infalling towards it. In this simple test, one can see that out of the maximun of the density (blue), magnetic field (green) and thermal energy (purple), the trajectory of the center is best followed by the thermal gas energy of the system.
Spectral evolution
Following the center of the galaxy cluster as it forms, one can compute its magnetic (purple) and kinetic (green) energies. The energy power-spectrum (Fourier transform of the energy) as function of the wavenumber (scale), shows the complex evolution of a galaxy cluster undergoing various merger events. The magnetic amplification is found at large wavenumbers (in this case, scales < 160 kpc).