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You can access our paper on Apep for free on arXiv: arXiv:2507.14610
You can also access our book chapter on Wolf-Rayet colliding wind binaries for free on arXiv: arXiv:2412.12534

Stars come in all shapes and sizes, and the main property that affects their life is their mass. Massive stars end their lives in the spectacular fireworks we call supernovae, and the most massive stars get rid of all of their hydrogen before they do it; we call these most-massive stars Wolf-Rayet stars. Wolf-Rayet (WR) stars have uniquely strong stellar winds, and they are constantly pumping out enriched material like carbon or nitrogen into the interstellar medium. Most massive stars are in binary systems, though, and when one of these carbon-type WR stars is in a close binary with another star they produce dust. This is because the winds of the stars collide, get compressed and mix together; this allows the gas to cool down into dust when it's far enough away from the stars. This dust is formed along a shock cone, but as the two stars in the binary orbit each other, the position of this cone rotates around the centre of mass. Hence, the dust is wrapped into a beautiful geometric spiral which gives us all the information we could ever want about the stars' orbits and their winds. These spirals look something like this:

The above image was taken by the James Webb Space Telescope (JWST), and is a false-colour image made from data in mid-infrared wavelengths (which is where the thermal dust is bright!). We describe this system and a bunch of others like it in a book chapter published in Elsevier's Encyclopedia of Astrophysics (see link at top).

With the new JWST data that you see above, I wrote a paper describing everything we can learn from the dust geometry of the system (see link at top) which we call Apep (after the Egyption god of chaos). We found that the two WR stars at the centre of the system (the only star system we know of in this configuration!) are on a very long period, eccentric orbit. We also found that there is a third star in the system, a blue supergiant star, whose wind and ionising radiation is destroying dust in a circular cavity as the nebula expands. I like to refer to this third star as Ouroboros — the serpent eating it's own tail (which is what I titled the paper!). Take a look at the animation below and see if you can spot the circular imprint of destruction!

The bright dot in the centre of the above animation is the two WR stars in the Apep system, and the dot just nearby is the third supergiant star.
Our paper has received some media attention, and I was very lucky to be interviewed by Stephen Luntz for a story in IFLScience. My supervisor and collaborator A/Prof Benjamin Pope was also invited to write a story on our work in The Conversation. I'd highly recommend checking it out!

As with my DES Time Dilation paper, I've made an annotated accessible summary of my paper which you can see below. I'd like to once again thank Dr Claire Lamman, for first doing these annotated summaries — they're a great idea!