Quark matter formation in a binary neutron star merger with VQCD equation of state @relastroitp-goetheuniversi1616

Relastro @ ITP - Goethe University, Frankfurt | Quark matter formation in a binary neutron star merger with VQCD equation of state @relastroitp-goetheuniversi1616 | Uploaded 1 year ago | Updated 3 minutes ago
The movie shows the inspiral and post-merger evolution of an unequal mass neutron star binary with the soft version of the V-QCD EoS. The orbital rotation of the binary is counteracted by rotating by (half of) the phase angle of the gravitational wave strain, to achieve an approximately co-rotating frame. The 2D slices of quark volume fraction (left) and temperature (right) are shown in the orbital plane, along with the contours of the baryonic density (in units of nuclear saturation density). The bottom panel shows the evolution of the plus polarization of the gravitational wave strain.

Publications:
Quark formation and phenomenology in binary neutron-star mergers using V-QCD:
scipost.org/SciPostPhys.13.5.109

Dense and Hot QCD at Strong Coupling:
journals.aps.org/prx/abstract/10.1103/PhysRevX.12.041012

Equations of state (soft, intermediate and stiff version) used in the simulations, available on the CompOSE database:
https://compose.obspm.fr/eos/290
https://compose.obspm.fr/eos/289
https://compose.obspm.fr/eos/291

Credits:
Samuel Tootle, Christian Ecker, Konrad Topolski, Tuna Demircik, Matti Järvinen, Luciano Rezzolla

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

$Quark matter formation in a binary neutron star merger with VQCD equation of state The movie shows the inspiral and post-merger evolution of an unequal mass neutron star binary with the soft version of the V-QCD EoS. The orbital rotation of the binary is counteracted by rotating by (half of) the phase angle of the gravitational wave strain, to achieve an approximately co-rotating frame. The 2D slices of quark volume fraction (left) and temperature (right) are shown in the orbital plane, along with the contours of the baryonic density (in units of nuclear saturation density). The bottom panel shows the evolution of the plus polarization of the gravitational wave strain. Publications: Quark formation and phenomenology in binary neutron-star mergers using V-QCD: https://scipost.org/SciPostPhys.13.5.109 Dense and Hot QCD at Strong Coupling: https://journals.aps.org/prx/abstract/10.1103/PhysRevX.12.041012 Equations of state (soft, intermediate and stiff version) used in the simulations, available on the CompOSE database: https://compose.obspm.fr/eos/290 https://compose.obspm.fr/eos/289 https://compose.obspm.fr/eos/291 Credits: Samuel Tootle, Christian Ecker, Konrad Topolski, Tuna Demircik, Matti Järvinen, Luciano Rezzolla Links: Relativistic Astrophysics group page: https://relastro.uni-frankfurt.de/ JETSET page: https://jetset-erc.org/ ELEMENTS page: https://elements.science$

Accretion flow onto a Kerr Black Hole and Raytraced Emission (Spanish)

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

Delayed phase transition to quark-gluon plasma in binary neutron star merger

Black hole surrounded by an accretion disc

Black hole - neutron star merger: dependence on the black hole spin

Gravitational Collapse to a Rotating Black Hole

Evolution of Special Relativistic Turbulent Plasma

Inspiral and Merger of equal-mass Relativistic Neutron Stars

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