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Scientists Discover Way to Send Information into Black Holes Without Using Energy

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Scientists Discover Two Dead Stars That Could Trigger a Cosmic Explosion!

The universe is filled with powerful explosions that help scientists understand how stars live, evolve, and die. Among the most important of these events are Type Ia supernovae, incredibly energetic stellar explosions that play a major role in the evolution of galaxies and the formation of chemical elements.

For decades, astronomers have investigated how these explosions begin. One leading explanation involves two white dwarfs, the dense remains of stars that have reached the end of their lives. Now, researchers have identified a remarkable pair of white dwarfs whose combined mass exceeds a critical limit known as the Chandrasekhar limit. This discovery could help scientists understand how some of the universe's most important stellar explosions occur.

The system, named WDJ181058.67+311940.94, is particularly interesting because it is relatively close to Earth and may eventually produce a Type Ia supernova.

What Are White Dwarfs?

White dwarfs are the small, extremely dense remains of stars that have exhausted their nuclear fuel. When a star similar to our Sun reaches the end of its life, it expands into a red giant and eventually sheds its outer layers. Its hot core remains behind as a white dwarf.

Although white dwarfs are roughly comparable in size to Earth, they can contain a substantial fraction of the Sun's mass. This makes them extraordinarily dense.

A white dwarf can remain stable because of a quantum-mechanical effect called electron degeneracy pressure. This pressure resists the inward pull of gravity and prevents the star from collapsing further under ordinary conditions.

However, this stability has a limit.

Understanding the Chandrasekhar Limit

The Chandrasekhar limit is approximately 1.4 times the mass of the Sun. It represents the approximate maximum mass that a non-rotating white dwarf made primarily of carbon and oxygen can support through electron degeneracy pressure.

When a white dwarf approaches or exceeds this limit, its structure and stability can change dramatically. Under suitable conditions, this may lead to a thermonuclear explosion.

Astronomers have long considered the possibility that two white dwarfs orbiting each other could eventually produce a Type Ia supernova. As the stars lose orbital energy, they move closer together. Eventually, they may collide or interact in ways that trigger a runaway nuclear reaction.

However, finding sufficiently massive pairs that can produce an explosion within a cosmologically relevant period has been a major challenge.

A Rare Binary System With an Extraordinary Mass

Researchers led by Munday and colleagues have reported the discovery of WDJ181058.67+311940.94, a binary system containing two white dwarfs.

The combined mass of the pair is approximately 1.555 times the mass of the Sun, with an uncertainty of 0.044 solar masses. This places the system above the commonly quoted Chandrasekhar limit.

Another remarkable feature is its distance from Earth. The binary lies only about 49 parsecs away, equivalent to approximately 160 light-years. In astronomical terms, this makes it a relatively nearby system and an important target for further observations.

The discovery is significant because astronomers have struggled to find enough massive double-white-dwarf systems that could help explain the observed population of Type Ia supernovae.

The newly identified binary provides an important example of the type of system researchers have been searching for.

Could These Two Stars Produce a Supernova?

According to the researchers' predictions, WDJ181058.67+311940.94 could eventually produce a Type Ia supernova through a process called a double detonation.

In this scenario, an explosion begins in a helium-rich outer layer of a white dwarf. The shock generated by that initial detonation can trigger a second explosion deeper inside the star, where carbon and oxygen may undergo rapid nuclear burning.

In a double-white-dwarf system, the interaction between the stars can create conditions that allow explosive burning to begin before the two objects complete their merger.

If the predicted process occurs in this system, both white dwarfs could be destroyed in the resulting explosion.

The researchers expect the event to appear as a subluminous Type Ia supernova. This means it would be less bright than many typical Type Ia supernovae, although it would still release an enormous amount of energy.

Their estimate suggests a peak apparent visual magnitude of approximately −16. For comparison, this would make the explosion roughly 200,000 times brighter than Jupiter in apparent brightness, according to the comparison provided in the study.

Such an event would offer astronomers an opportunity to investigate how thermonuclear explosions develop in massive white-dwarf systems.

A Long Wait for a Cosmic Explosion

Despite its potential, this binary is not expected to explode anytime soon.

The researchers estimate its merger time at approximately 22.6 billion years, with an uncertainty of about 1 billion years.

A merger time is the estimated period remaining before the two stars come together through the gradual loss of orbital energy, largely through gravitational-wave emission.

For context, the universe is approximately 13.8 billion years old. The predicted merger time is therefore longer than the universe's current age.

This does not mean the system is unimportant. Instead, it provides evidence that massive white-dwarf binaries exist and can help scientists understand the possible pathways leading to Type Ia supernovae.

The proposed double-detonation scenario also suggests that an explosion could begin before the stars complete their merger. However, the exact outcome remains a theoretical prediction rather than an observed event.

Why This Discovery Matters for Supernova Research

Type Ia supernovae are especially valuable to astronomy because their brightness can be calibrated to estimate distances across the universe. These measurements have helped researchers study the expansion of the cosmos and investigate the mysterious influence of dark energy.

They also contribute to the chemical enrichment of galaxies by releasing elements produced during thermonuclear burning, including iron-group elements.

Understanding the origins of these explosions is therefore essential.

Scientists have proposed several possible pathways to Type Ia supernovae. One involves a white dwarf gaining material from a companion star. Another involves two white dwarfs interacting or merging. The newly identified system supports the idea that massive double-white-dwarf binaries could contribute to this process.

However, one discovery cannot establish that this is the dominant pathway.

What Do the Numbers Tell Us?

The researchers estimate that super-Chandrasekhar-mass double-white-dwarf systems are born at a rate of at least 6.0 × 10⁻⁴ per year. Meanwhile, the estimated rate of Type Ia supernovae in the Milky Way arising from such systems is approximately 4.4 × 10⁻⁵ per year.

The predicted Type Ia supernova rate from all proposed progenitor pathways is about 60 times higher than the rate attributed to these massive binary systems.

This difference is important. Although massive double white dwarfs may explain some Type Ia supernovae, they do not appear sufficient on their own to account for the entire observed population.

The discovery helps address the shortage of massive double-white-dwarf systems identified in carefully selected stellar populations. Nevertheless, astronomers need more observations and stronger evidence to determine which pathways produce most Type Ia supernovae.

Conclusion

The discovery of WDJ181058.67+311940.94 offers an important new clue in the search for the origins of Type Ia supernovae. With a combined mass of approximately 1.555 solar masses and a location only 160 light-years away, this rare binary provides an opportunity to study massive white-dwarf systems in greater detail.

Researchers predict that the two stars could undergo a double detonation, potentially destroying both stars in a relatively faint Type Ia supernova. However, the estimated merger time of 22.6 billion years means that this particular event is not expected in the near future.

More importantly, the system helps scientists investigate a longstanding question: how do white dwarfs trigger the powerful explosions observed throughout the universe?

While this discovery brings researchers closer to an answer, the mystery is not yet solved. Further discoveries will be needed to establish which stellar systems are responsible for the majority of Type Ia supernovae.

Reference: Munday, J., Pakmor, R., Pelisoli, I. et al. A super-Chandrasekhar mass type Ia supernova progenitor at 49 pc set to detonate in 23 Gyr. Nat Astron 9, 872–882 (2025). https://doi.org/10.1038/s41550-025-02528-4

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