A fascinating discovery has been made regarding a white dwarf star, situated about 1,700 light-years from Earth. This white dwarf, known as RX J0648.0–4418, is part of a unique binary system where it is continuously drawing stellar material from its companion star, HD 49798, a helium-burning hot subdwarf. Despite its shrinking size, the white dwarf maintains a surprisingly rapid spin, completing a full rotation approximately every 13 seconds. This rapid rotation has raised new questions about the dynamics of binary star systems and the potential fate of this star in the future.
The white dwarf’s behavior is especially intriguing as it appears to be approaching a critical mass known as the Chandrasekhar limit. Once a white dwarf reaches this mass, it can no longer support itself against gravity and may explode in a supernova. In the case of RX J0648.0–4418, this could occur within the next 100,000 years, providing a rare opportunity to study the final stages of a star’s life. The discovery, published in a study by Dr. Sandro Mereghetti of the National Institute of Astrophysics (INAF), shines a light on this star’s exceptional rotational speed and its interaction with its companion.
What makes this system particularly remarkable is the nature of the interaction between the two stars. In most X-ray binary systems, a neutron star or black hole typically pulls material from its companion, but in this case, it’s the white dwarf that is accreting material from a hot subdwarf star. This evolutionary phase is quite rare and typically short-lived, which makes the RX J0648.0–4418 system even more exceptional. The relationship between the two stars offers a unique glimpse into the diverse ways binary systems can evolve.
One of the greatest mysteries surrounding this white dwarf is its incredibly rapid spin, which cannot be fully explained by the material it is accumulating from its companion. The accretion rate has been measured, and it turns out to be too low to account for the extraordinary spin observed. This suggests that there may be other factors at play, possibly related to the star’s internal structure or its history of material accumulation. Further study of RX J0648.0–4418 could offer valuable insights into the complex behavior of white dwarfs and their eventual fate in the cosmos.
