Evolution of Special Relativistic Turbulent Plasma @relastroitp-goetheuniversi1616

Relastro @ ITP - Goethe University, Frankfurt | Evolution of Special Relativistic Turbulent Plasma @relastroitp-goetheuniversi1616 | Uploaded 1 year ago | Updated 1 hour ago
The movie shows the electron and proton number density, the trajectories, and the Lorentz factor of most energetic particles. The initial configuration corresponds to a plasma with magnetization sigma=1, plasma beta=10^-3, electron-to-proton temperature ratio Te/Tp = 1, and realistic mass ratio between electrons and protons, which is a representative simulation of a comprehensive campaign of two-dimensional kinetic particle-in-cell simulations of special-relativistic turbulence. The interaction between plasmoid islands produces multiple reconnection regions accelerating and heating the particles, producing non-thermal particles.

Publications:
arxiv.org/abs/2301.02669

Credits:
Claudio Meringolo, Alejandro Cruz-Osorio, Luciano Rezzolla and Sergio Servidio

Links:
Relativistic Astrophysics group page: https://relastro.uni-frankfurt.de/
JETSET page: jetset-erc.org
ELEMENTS page: https://elements.science

Code:
Zeltron: https://ipag.osug.fr/~ceruttbe/Zeltron/index.html

Inspiral and Merger of equal-mass Relativistic Neutron Stars

$NewCompStar: Binary neutron star merger with tracer evolution The origin of the heavy elements in our universe is an open problem in astronomy. The production of the heavy element is formed through a certain type of nucleosynthesis called rapid neutron capture process or r-process. The environment required for r-process requires a neutron rich environment and for many years it was thought that the only production sites could be from supernova explosions. However, more detailed numerical simulations have shown that the environments from supernovas isnt neutron-rich enough and that another source is required. New simulations from binary neutron star (BNS) mergers have been very promising candidates for the progenitors of the heavy elements. In order to study r-process nucleosynthesis, the history of the fluid element is required, along with key properties that are illustrated in the animation. These include density, electron fraction, and kinetic energy. By taking the time series of this data and plugging it into a nuclear network, abundancy curves of heavy elements can be produced. In this animation, we show the merger of two 1.35 solar mass neutron stars with the LS220 equation of state. To capture the evolution of the fluid, we use tracers that can track the evolution of the fluid elements through time. The distribution of the tracers can provide insight into how the heavy elements are made. The code used is the EinsteinToolkit with WhiskyTHC. Creating this visualization of the simulation data was supported by NewCompStar (MPI304 Cost Action). COST (European Cooperation in Science and Technology) is a pan-European intergovernmental framework. Its mission is to enable break-through scientific and technological developments leading to new concepts and products and thereby contribute to strengthening Europe’s research and innovation capacities. The original video can be found here: https://cloud.itp.uni-frankfurt.de/index.php/s/D4D5JqxFYbOciiP$

Crustal magnetic field amplification in BNS mergers: Co-rotating sources of magnetic energy

Gravitational Collapse to a Rotating Black Hole

GRMHD Simulations and Best-bet Model for Sagittarius A*

Black hole surrounded by an accretion disc

Crustal magnetic field amplification in BNS mergers: Co-rotating vorticity