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X-ray tracking reveals uneven expansion in young supernova remnant G292.0+1.8
By analyzing data from NASA's Chandra X-ray Observatory, Dutch astronomers have investigated a young, oxygen-rich supernova remnant known as G292.0+1.8. Results of the new study, published June 29 on the arXiv preprint server, yield important insights into the expansion of this remnant.
Supernova remnants (SNRs) are the remains of a supernova explosion, observed as diffuse, expanding structures. Studies indicate that SNRs harbor ejected material expanding from the supernova explosion. They also contain other interstellar material that has been swept up by the passage of the shock wave from the exploded star.
A well-known SNR as seen by Chandra
Located some 15,000 light-years away, G292.0+1.8 is a young (estimated to be a few hundred years old), oxygen-rich supernova remnant first identified in 1961. It is a galactic core-collapse supernova remnant (CCSNR), which shows no detectable lines of hydrogen and helium and the presence of only oxygen and neon.
A team of astronomers led by Maria Aslanidou of the University of Amsterdam decided to reinvestigate the properties of G292.0+1.8, focusing mainly on its expansion during a span of approximately 10 years. For this purpose, they analyzed available data from observations of this remnant conducted with Chandra's Advanced CCD Imaging Spectrometer (ACIS).
"This study examines the expansion rate of the Galactic SNR G292.0+1.8 using deep X-ray observations in order to better understand its dynamical evolution and the structure of the ejecta," the researchers wrote in the paper.
What the Chandra data says
Based on the data from ACIS, Aslanidou's team managed to conduct the first estimation of the weighted-mean X-ray expansion rate for G292.0+1.8, which was measured at approximately 0.016% per year.
The expansion rate indicates that the expansion age of G292.0+1.8 lies between 2,500 and 4,200 years. This is broadly consistent with previous estimates based on optical filament proper motions and the central pulsar's spin-down age.
Furthermore, the astronomers identified significant azimuthal variations in the expansion of G292.0+1.8. It turned out that the eastern portion expands more than other regions. This, according to the authors of the paper, can be explained by the interaction between the pulsar wind nebula and the reverse shock, which creates a reflected shock that further affects the surrounding ejecta.
A paradox arises
The researchers noted that their findings regarding the expansion of G292.0+1.8 introduce an apparent paradox.
"In some sectors, the largest expansion is observed broadly in the same direction as the neutron-star kick, rather than opposite to it as a simple momentum argument might suggest," they concluded.
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Publication details
Maria Aslanidou et al, Expansion rate of the young, oxygen-rich supernova remnant G292.0+1.8, arXiv (2026). DOI: 10.48550/arxiv.2606.30643
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Citation: X-ray tracking reveals uneven expansion in young supernova remnant G292.0+1.8 (2026, July 11) retrieved 11 July 2026 from https://phys.org/news/2026-07-ray-tracking-reveals-uneven-expansion.html
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