Accretion flow onto a Kerr Black Hole and Raytraced Emission (Spanish) @relastroitp-goetheuniversi1616

Relastro @ ITP - Goethe University, Frankfurt | Accretion flow onto a Kerr Black Hole and Raytraced Emission (Spanish) @relastroitp-goetheuniversi1616 | Uploaded 5 years ago | Updated 1 hour ago
Version without text: youtu.be/XmvpKFSvB7A
English version: youtu.be/p0jq8ErfGCA
German version: youtu.be/G4G6J8VOtKs
Chinese version: youtu.be/mkx56MuSmPE
Italian version: youtu.be/kQpap2iOIXg
Japanese version: youtu.be/dgb7UfJTX6g
Spanish version: youtu.be/q2Rycr-IdfU

In the video we show a zoom in from optical telescope images to the heart of the galaxy M87.
There, a plasma of several billion degrees Celsius is swirling around the black hole at over a 3,600,000 km/h.
This system is simulated on a supercomputer. Analyzing the simulation we can create an image of what the black hole should look like as seen from Earth.
With the global EHT collaboration we were able to combine telescopes all around the world to create a single, Earth sized telescope, which can then observe the actual black hole.
After the observation in April 2017 it took hundreds of scientists two years to create the final image presented in this video.
This observational image can then be compared to the simulation of the black hole, and with this we can once again test Einsteins Theory of Relativity against reality.

The galaxy M87 is 55 million light years away or 52x10²⁰ km
Its central black hole has a mass of 7.22 billion solar masses, or 1.4356x10³⁷ kg or 3.1651x10³⁷ lb

Link to our homepage: https://relastro.uni-frankfurt.de/
Link to our gallery: https://relastro.uni-frankfurt.de/gallery/

Link to the EHT website: eventhorizontelescope.org

Link to the Black Hole Cam Website: blackholecam.org

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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

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