Visualization of GW190814
A visualization I created in 2020 with Python and ParaView, published under the MIT license.
Renderings of the highly unequalmass gravitationalwave event measured by LIGO and Virgo on Aug 14, 2019.
From README.md in the nilsvu/gw190814movie GitHub repository:
Visualization of the GW190814 gravitationalwave signal
Visualisation of the coalescence of two black holes that inspiral and merge, emitting gravitational waves. One black hole is 9.2x more massive than the other and both objects are nonspinning. The high massratio amplifies gravitationalwave overtones in the emitted signal. The gravitationalwave signal produced is consistent with the observation made by the LIGO and Virgo gravitationalwave detectors on August 14th, 2019 (GW190814).

Video:
 More information and images available at: https://www.aei.mpg.de/263744/gw190814 and https://dcc.ligo.org/LIGOG2000730/public
 Credit: N. Fischer, S. Ossokine, H. Pfeiffer, A. Buonanno (Max Planck Institute for Gravitational Physics), Simulating eXtreme Spacetimes (SXS) Collaboration
 Selected media coverage:
 https://www.aei.mpg.de/267070/ablackholewithapuzzlingcompanion
 https://www.ligo.org/detections/GW190814
 https://www.space.com/smallestblackholebiggestneutronstarymysteryobject.html
 https://www.dailymail.co.uk/sciencetech/article8451939/Mysteriouscosmicobjectlighterblackholeheavierneutronstardiscovered.html
Details on the visualization
The visualization shows the gravitationalwave signal and trajectories of the horizons of the black holes. It begins about 10 seconds before merger. At this stage, the black holes have about 160 orbits left until they merge, and the gravitationalwave frequency is about 20Hz. This inspiral is longer than any available NR simulations with physical parameters consistent with the event. Therefore, the visualization combines results from an effectiveonebody model (the SEOBNRv4HM waveform model) and numerical relativity. In particular:
 The gravitationalwave strain is computed with the SEOBNRv4HM waveform model.
 The trajectories of the black holes and the shapes of their horizons: Up to 0.7 seconds to merger, the trajectory data is computed with the SEOBNRv4HM model, and the horizons are shown as coordinate spheres, with radii proportional to the their masses. For the last 0.7 seconds to merger, for the merger itself, and for the ringdown the visualization shows trajectories and apparent horizons from an NR simulation by the SXS collaboration of a system with the same mass ratio (SXS:BBH:1108).
 The gravitational radiation is translated to colors around the black holes. Specifically, the colors represent the real part of the gravitationalwave strain with its inverse radial scaling removed for visualization.
 The left (main) panel always shows the full radiation content, with colors transitioning from blue, representing weak radiation, to orange, representing strong radiation.
 Each of the four panels to the right shows a separate component (or overtone) of the gravitationalwave signal in a different color. From left to right and top to bottom, the panels show the quadrupolar (l=2, m=+/2), octupolar (l=3, m=+/3), hexadecupolar (l=4, m=+/4) and 32polar (l=5, m=+/5) modes. Each mode is scaled in amplitude to its respective maximum. The colors in these four panels transition from dark to bright, representing weak to strong radiation of each respective mode.
 The simulation was performed with the SpEC numerical relativity code by the Simulating eXtreme Spacetimes (SXS) Collaboration.
 The visualization is based on the gwpv code, using the ParaView scientific visualization toolkit.