Recorded 7 October 2021. Manuela Campanelli of the Rochester Institute of Technology presents "Merging black hole binaries: accretion dynamics and outflows" as part of IPAM's Workshop I: Computational Challenges in Multi-Messenger Astrophysics.
Learn more online at: http://www.ipam.ucla.edu/programs/workshops/workshop-i-computational-challenges-in-multi-messenger-astrophysics/?tab=schedule
This animation was produced by Leo Werneck at the University of West Virginia using IllinoisGRMHD. The movie displays results from an equal-mass (~1.4 solar masses), magnetized binary neutron star system with initial separation of 50km. The code uses the LS220 tabulated equation of state of O’Connor & Ott (freely available at stellarcollapse.org). The left panel shows the base-10 logarithm of the baryonic density, while the right panel shows the temperature on our numerical grids. We model the inspiral, merger and black hole formation, evolving the remnant black hole for an additional 14ms (~1000M).
This simulations shows the accretion patterns around two merging black holes. This is to show the smoothness of the transition between IllinoisGRMHD to harm3d, which are two different magnetohydrodynamics codes.
Manuela Campanelli, astrophysicist and Professor of Mathematical Sciences at Rochester Institute of Technology, simulates compact objects in the universe, like black holes and neutron stars. Frontera allows her team of researchers to simulate these complex systems twice as fast as previous systems.
Simulation is the same as the previous movie (https://youtu.be/Kp6i8N4DiaQ), except there is a very large high-res box centered at the origin at all times. This box has the same resolution (~191m) as the boxes around the NSs, both in this simulation and in the previous one. The black hole coordinate drift velocity is only about 60km/sec in this case, where it was about 200km/sec in the previous simulation.
Initial central density is about 1e-3 in these units.