- 77
- 177 298
Relastro @ ITP - Goethe University, Frankfurt
Приєднався 16 вер 2015
The Relativistic Astrophysics (RelAstro) group has been built at the end of 2013 at Goethe University in Frankfurt, Germany. The interests of the group cover a large area of topics. In essence, we use Einstein’s theory of general relativity to describe and explain high-energy astronomical observations of black holes and neutron stars.
The group combines analytical perturbative tools with numerical nonlinear simulations in which we solve the Einstein equations together with those of relativistic hydrodynamics or magnetohydrodynamics. We do this in the endless process of comparing theoretical results and predictions with astronomical observations. More information can be found under the research menu and browsing through the pages of the group members.
The group is led by Prof. Dr. Luciano Rezzolla.
For more information visit our website at relastro.uni-frankfurt.de/
The group combines analytical perturbative tools with numerical nonlinear simulations in which we solve the Einstein equations together with those of relativistic hydrodynamics or magnetohydrodynamics. We do this in the endless process of comparing theoretical results and predictions with astronomical observations. More information can be found under the research menu and browsing through the pages of the group members.
The group is led by Prof. Dr. Luciano Rezzolla.
For more information visit our website at relastro.uni-frankfurt.de/
Black hole - neutron star merger: Tidal disruption
The evolution of a black hole - neutron star binary system, with mass ratio q=4, using the DD2 equation of state, and with the neutron star mass of 1.4 solar masses. The black hole is rapidly rotating, with the dimensionless spin parameter equal to 0.8. The neutron star is disrupted and forms a massive tidal tail, which leaves behind a substantial amount of baryonic matter in the form of an accretion disc.
Authors: Morten Will, Konrad Topolski, Marie Cassing, Luciano Rezzolla
Authors: Morten Will, Konrad Topolski, Marie Cassing, Luciano Rezzolla
Переглядів: 4 187
Відео
Black hole - neutron star merger: Plunge
Переглядів 1,8 тис.2 місяці тому
The evolution of a black hole - neutron star binary system, with mass ratio q=4, using the DD2 equation of state, and with the neutron star mass of 1.4 solar masses. Both objects are irrotational. The neutron star enters the black hole essentially intact and there is no accretion disc formed. Authors: Morten Will, Konrad Topolski, Marie Cassing, Luciano Rezzolla
Black hole - neutron star merger: dependence on the mass ratio
Переглядів 2,4 тис.2 місяці тому
Evolution of a black hole - neutron star system as a function of binary mass ratio. The neutron stars are identical in each case, with mass equal to 1.4 solar masses and modeled with the DD2 equation of state. The dimensionless black hole spin parameter is set to 0.8 in each case. The ratio of the black hole to the neutron star mass from left to right is 5, 6 and 7, respectively. Larger mass as...
Black hole - neutron star merger: dependence on the black hole spin
Переглядів 2,7 тис.2 місяці тому
Evolution of a black hole - neutron star system as a function of black hole spin. The neutron stars are identical in each case, with mass equal to 1.4 solar masses and modeled with the DD2 equation of state. The ratio of the black hole to the neutron star mass in each case is 4.The dimensionless black hole spin parameters from left to right are 0.4, 0.6 and 0.8, respectively. Higher prograde bl...
Evolution of Special Relativistic Turbulent Plasma
Переглядів 474Рік тому
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 tw...
Crustal magnetic field amplification in BNS mergers: Co-rotating sources of magnetic energy
Переглядів 3672 роки тому
The movie shows the merger and post-merger evolution of two equal mass neutron star binaries with a total mass of approximately 2.5 solar masses. 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 the sources and sinks of magnetic-energy density are shown fo...
Crustal magnetic field amplification in BNS mergers: Co-rotating vorticity
Переглядів 2292 роки тому
The movie shows the merger and post-merger evolution of two equal mass neutron star binaries with a total mass of approximately 2.5 solar masses. 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 the density-weighted vorticity are shown for the xy-plane. Th...
Crustal magnetic field amplification in BNS mergers: Co-rotating magnetic-field strength
Переглядів 2212 роки тому
The movie shows the merger and post-merger evolution of two equal mass neutron star binaries with a total mass of approximately 2.5 solar masses. 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 the absolute magnetic-field strength are shown for the xy-pla...
Crustal magnetic field amplification in binary neutron star mergers: Vorticity
Переглядів 9412 роки тому
The movie shows the merger and post-merger evolution of two equal mass neutron star binaries with a total mass of approximately 2.5 solar masses. The 2D slices of the density-weighted vorticity are shown for the xy-plane in the top row and for the xz-plane in the bottom row. The contours of constant baryonic density are shown in dashed (10^13 g cm^-3) and solid (7x10^14 g cm^-3) green lines. Th...
Crustal magnetic field amplification in binary neutron star mergers: Sources of magnetic energy
Переглядів 3112 роки тому
The movie shows the merger and post-merger evolution of two equal mass neutron star binaries with a total mass of approximately 2.5 solar masses. The 2D slices of the sources and sinks of magnetic-energy density are shown for the xy-plane in the top row and for the xz-plane in the bottom row. Red color coding shows the regions where the magnetic energy is increasing at the expense of the availa...
Crustal magnetic field amplification in binary neutron star mergers: Magnetic-field strength
Переглядів 2,2 тис.2 роки тому
The movie shows the merger and post-merger evolution of two equal mass neutron star binaries with a total mass of approximately 2.5 solar masses. The 2D slices of the absolute magnetic-field strength are shown for the xy-plane in the top row and for the xz-plane in the bottom row. The contours of constant baryonic density are shown in dashed (10^13 g cm^-3) and solid (7x10^14 g cm^-3) green lin...
Quark matter formation in a binary neutron star merger with VQCD equation of state
Переглядів 4832 роки тому
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 orb...
Phase transition triggered collapse in an unequal mass binary neutron star merger with V-QCD EoS
Переглядів 2972 роки тому
The movie shows the late inspiral and post-merger evolution in an unequal mass merger event with the soft version of the EoS. 2D slices of density (in units of nuclear saturation density) and temperature are shown in the orbital and the XZ plane, along with the contours of the quark volume fraction. Additionally, the gravitational wave signal of the event (in red) is contrasted against the sign...
Comparing two supermassive black holes: Sgr A* vs M 87*
Переглядів 3,7 тис.2 роки тому
The two supermassive black holes that have been observed by the EHT have considerable differences in mass. M87* is more than a thousand times larger than the black hole at the centre of our galaxy, Sgr A*, which means that the gas goes around the latter much faster (on the timescale of minutes) than it goes around the former (on the timescale of days to weeks). When using the Dolomites as an an...
General Relativistic-Magnetohydrodynamic and Radiative-Transfer simulations of accretion onto Sgr A*
Переглядів 1,3 тис.2 роки тому
The movie shows the evolution of black hole and magnetised accretion disk system, and radiation at radio frequencies emitted by the hot plasma (red colours) falling onto the rotating black hole and launching a high magnetised jet where the plasma is moving at relativistic speeds (blue colours). The zoom-in shows details of the plasma near the black hole and transits to the a vision of the radia...
Clustering und Mittelung der Bilder von Sgr A*
Переглядів 1042 роки тому
Clustering und Mittelung der Bilder von Sgr A*
GRMHD Simulations and Best-bet Model for Sagittarius A*
Переглядів 3,7 тис.2 роки тому
GRMHD Simulations and Best-bet Model for Sagittarius A*
Clustering and averaging the images of Sgr A*
Переглядів 1302 роки тому
Clustering and averaging the images of Sgr A*
Vergleich zweier supermassiver Schwarzer Löcher Sgr A* vs M 87*
Переглядів 2602 роки тому
Vergleich zweier supermassiver Schwarzer Löcher Sgr A* vs M 87*
Constraining Black Hole Models with EHT Observations
Переглядів 3073 роки тому
Constraining Black Hole Models with EHT Observations
Simulation of a common envelope evolution interacting with a stellar black hole
Переглядів 3684 роки тому
Simulation of a common envelope evolution interacting with a stellar black hole
Delayed phase transition to quark-gluon plasma in binary neutron star merger
Переглядів 9 тис.4 роки тому
Delayed phase transition to quark-gluon plasma in binary neutron star merger
Simulation of binary neutron-star merger with quark-hadron phase transition
Переглядів 6625 років тому
Simulation of binary neutron-star merger with quark-hadron phase transition
Accreting black hole in Virtual Reality
Переглядів 2,6 тис.5 років тому
Accreting black hole in Virtual Reality
Accretion flow onto a Kerr Black Hole and Raytraced Emission (Italian)
Переглядів 1,4 тис.5 років тому
Accretion flow onto a Kerr Black Hole and Raytraced Emission (Italian)
Telescopes in the Event Horizon Telescope Collaboration for future Observations
Переглядів 3455 років тому
Telescopes in the Event Horizon Telescope Collaboration for future Observations
Accretion flow onto a Kerr Black Hole and Raytraced Emission (Spanish)
Переглядів 2,6 тис.5 років тому
Accretion flow onto a Kerr Black Hole and Raytraced Emission (Spanish)
Accretion flow onto a Kerr Black Hole and Raytraced Emission (English)
Переглядів 7 тис.5 років тому
Accretion flow onto a Kerr Black Hole and Raytraced Emission (English)
Accretion flow onto a Kerr Black Hole and Raytraced Emission (Chinese)
Переглядів 3775 років тому
Accretion flow onto a Kerr Black Hole and Raytraced Emission (Chinese)
Using VLBI to create an Image of the black hole in the center the Galaxy M87
Переглядів 16 тис.5 років тому
Using VLBI to create an Image of the black hole in the center the Galaxy M87
Sooo because space has no sound it be like this
Sagittarius A* is definitely way bigger then that goofy little Messier-87* lol
this is super fascinating
We'll information good 😅
We'll information good show 😊
What is this I don't believe that
Guys i dont think it's an app
Correct. Because the spin determines the velocity at which they combine and mix. To fast it'll through the matter away instead of taking it all in.
❤
❤❤
Apps name??
big no
Black hole name?
2
I liked every comment on this video
What’s the app
it’s a simulation, not an app/game and requires a pretty good pc to run.
Black hole eating star
Very cool
Great
kirohmatikaya.ha ma tomis
Kiris.mus takak.tok
Kiro.nate.kolax.tik.c.
Sequel to the 5 dimensional chess
The actual black hole: Grey sphere: Event horizon Sphere the black hole: Photon sphere Checker pattern around the black hole: Actual accretion disk What we see: Black circle: Shadow Ring: Photon ring Checker pattern arounf the shadow: What it looks like
Hmmmm
🔞
﴿ خِتَٰمُهُۥ مِسۡكٞۚ وَفِي ذَٰلِكَ فَلۡيَتَنَافَسِ ٱلۡمُتَنَٰفِسُونَ ﴾ [ المطففين: 26]
That's sick, dawg.
Pretty cool video, binary neutron star merger. Thanks for the vid :)
Thank you for sharing this 😊! Such a cool simulation
Cewl
Awesome! Thank you for sharing this
what do I cite when i show this video? is there a paper attached to it?
Excellent work!
ㅈ...주모!!!
Absurd quality.
Awesome simulation! Would you recommend learning Python as a first language for computational physics? I'm looking for something more versatile than Excel for statistical analysis and for making graphs for my lab reports and Python seems like a good choice.
Yeah I would recommend Python. I've been using it for a while, there isn't too much tricky syntax and there are plenty of useful libraries. Moreover, I think it's the go-to for many universities. Best of all, it's free.
@@IoannisChatzikyriakos That's about what I gathered, thank you!
Question is why electric current curved if it is not a ball. According to me Black ball is ancient large sun And our sun is it's core that again reforming. That's why big fire is seen in total. Some time these core burst mean outerest seen as also being seen in other case. So our solar system is new mean next generation of black ball that mean black ball is dying so milkiway. Hence 3d animation being used with reverse theory mean wrong interpretation.
No idea what you are saying. Did you use Google translate?
I agree! Nearly all pictures and videos of black holes show them from one perspective and that perspective is 2D. I would think that a black hole would appear like a star/sun to the observer. If it is a sphere then doesn't it absorb light from all (3D) directions? It would only look black once you pass the event horizon.The ENTIRE sphere would be surrounded by the light which is just about to become absorbed into it (cross the event horizon). Whenever I ask this question people are confused and regurgitate "standard" information. Does anyone else question this?
Money not only from government but also from readers.
Exactly. See four components mean elements we find everywhere. 1. Air 2. Dust. 3. Water 4. Vacuum mean space Electric generate by rotation of these four like we get fire form stones matching.
@@manojsaxena1462 lmao those are NOT elements. Go educate yourself
Dat Schwaze Loch :)
beautiful
Nice video #trackias for upsc ias
Hello
The linked video of Sag A* (youtu . be / VnsZj9RvhFU) is a simulation, not the real thing. See the comments on that video for an explanation. Long story short, Sag A* is more difficult to image, due in part to the far shorter timescale of variability, but also due to obscuration by foreground material. They're still working on the Sag A* data, but since M87 was easier to analyze, they announced it first.
amazing.
this is dope
is this simulated image of m87 galaxy? because isn't the released image.
I think it is a simulated image of what is expected to be seen of Sgr A* at the center of the Milky Way. No data has been published yet.
This is the image of Sagittarius A*, the black hole in the center of our galaxy. It's significantly smaller and less massive than the black hole in M87, but it's also far closer. The image released and published on news outlet is the image of the black hole at M87.
@@arnavipanda6503 I don't think it is real data but only simulated based on M87 data latest release.
MC Squared It is a real image of Sagittarius A*. Not sure where you're getting this bit of simulated data from. The EHT team explicitly stated that during the observation period in April of 2017, they pointed the telescopes toward both black holes.
@@arnavipanda6503 yes, but no data has been released about Sgr A*. I would be extremely surprised that they allow anyone to publish an image based on the real data before any official publication. Today, Shep Doeleman said they have a lot to do before publishing an image of Sgr A* and he said it is possible that the result will be inconclusive.
Amazing discovery and collaboration people!
Hi Relastro group, This may be a bigger problem than you think. Over half a million people have already watched Veritasium's video claiming this is the real image. If it is based on preliminary data, it may develop into a "leak"...
This is going to turn into a gong show, I wager.
In the credits at the end of the video, you forgot ALMA and ESO which is partner in APEX and ALMA
Why are you posting a video of Sagittarius A* if that image hasn't been released yet?
this is a simulation of how SgrA* would be processed. mainly using the actual process of M87 but, left, on the map you see telescopes used for SgrA*, some of which weren't used for M87