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

Relastro @ ITP - Goethe University, Frankfurt | Accretion flow onto a Kerr Black Hole and Raytraced Emission (Italian) @relastroitp-goetheuniversi1616 | Uploaded 5 years ago | Updated 2 hours 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

$Simulation of binary neutron-star merger with quark-hadron phase transition The video shows a computer simulation of a binary neutron-star merger. The simulation makes use of a special prescription for describing nuclear matter, so that during the merger the matter undergoes a phase transition from ordinary hadronic matter to quark matter. Shown are density, quark fraction and the temperature. More details can be found in the original publication by Most et al. (2019): https://arxiv.org/pdf/1807.03684.pdf Link to our homepage: https://relastro.uni-frankfurt.de/ Link to our gallery: https://relastro.uni-frankfurt.de/gallery/ Copyright: Lukas R. Weih & Luciano Rezzolla (2019)$

Clustering und Mittelung der Bilder von Sgr A*

Inspiral and Merger of equal-mass Relativistic Neutron Stars

Using VLBI to create an Image of the black hole in the center the Galaxy M87

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

NewCompStar: Binary neutron star merger in 3D

Telescopes in the Event Horizon Telescope Collaboration for future Observations

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

Electromagnetic Counterparts to Inspiralling Black Holes

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