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

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How Can We Tell Whether an Object Is a Planet or a Failed Star?

In the vast universe, not everything is easy to classify. Some objects sit right on the boundary between planets and stars, making astronomers scratch their heads. Two such mysterious objects are giant planets and brown dwarfs—often called “failed stars.” At first glance, they can look almost identical. But now, scientists have discovered a powerful new way to tell them apart: their spin.

A recent study based on observations from the W. M. Keck Observatory has revealed that how fast these objects rotate can uncover their true identity. This breakthrough is helping scientists better understand how planets and stars form in the universe.

The Cosmic Identity Problem

Distinguishing between giant planets and brown dwarfs has always been difficult. Both types of objects can have similar:

  • Sizes

  • Masses

  • Temperatures

  • Brightness

  • Atmospheric composition

Brown dwarfs are larger than planets but smaller than stars. Unlike stars, they cannot sustain nuclear fusion in their cores. Because of this, they emit only faint light, much like giant planets.

This overlap creates confusion. In some cases, the largest planets can be as massive as the smallest brown dwarfs. So, how do scientists tell them apart?

The Breakthrough: Spin as a Clue

A research team from Northwestern University discovered that rotation speed, or spin, is the key difference.

By studying:

  • 6 giant exoplanets

  • 25 brown dwarfs

they found a clear pattern:

👉 Giant planets spin much faster than brown dwarfs.

This discovery was published in the The Astronomical Journal and is based on one of the largest datasets of its kind.

According to lead researcher Chih-Chun Hsu,
“Spin is like a fingerprint from the time an object was formed.”

How Scientists Measured Spin

Measuring the spin of distant worlds is not easy. These objects are incredibly far away and faint. To solve this, scientists used a powerful technique called spectroscopy.

With the help of advanced instruments at Keck Observatory, they observed how light from these objects behaves. When an object spins, its light gets slightly stretched or compressed due to a phenomenon called Doppler broadening.

By analyzing this effect, scientists can calculate how fast an object is rotating.

A Clear Pattern Emerges

After analyzing the data, researchers compared their results with over 200 other celestial objects. They found something fascinating:

  • Giant planets rotate at a higher fraction of their maximum possible speed

  • Brown dwarfs rotate at a much slower fraction

This maximum limit is known as the breakup velocity—the speed at which an object would tear itself apart due to centrifugal force.

👉 In simple terms:
Giant planets spin closer to their limit, while brown dwarfs spin more slowly and safely.

Why Do They Spin Differently?

The answer lies in how these objects form.

Giant Planets

Giant planets form in disks of gas and dust surrounding young stars. During formation:

  • They gain angular momentum (spin)

  • Interactions with the disk can increase their rotation speed

Brown Dwarfs

Brown dwarfs form differently:

  • Either like stars, from collapsing gas clouds

  • Or like planets, but with higher mass

However, they experience a strong “cosmic braking” effect. Their powerful magnetic fields interact with surrounding gas, slowing their rotation over time.

👉 This means brown dwarfs lose more spin during formation compared to planets.

Interesting Exceptions

The study also found some surprising cases.

In the HR 8799 system:

  • A giant planet about 7 times the mass of Jupiter spins extremely fast

Meanwhile:

  • A nearby brown dwarf, even though it is heavier, spins six times slower

This clearly shows that mass alone does not determine spin—formation history matters more.

Even Stranger: Orbiting Brown Dwarfs Spin Slower

Another surprising discovery was that brown dwarfs orbiting stars spin even more slowly than isolated ones.

This suggests:

  • Their environment plays a role

  • Interactions with nearby stars may further slow them down

It highlights how complex and diverse the universe really is.

Why This Discovery Matters

This research is important for several reasons:

1. A New Identification Tool

Astronomers now have a reliable way to distinguish:

  • Giant planets

  • Brown dwarfs

Just by measuring their spin.

2. Understanding Formation

Spin acts like a “fossil record” of how an object formed. By studying it, scientists can:

  • Trace the history of planetary systems

  • Understand the physics of star and planet formation

3. Expanding Future Research

Scientists are now planning to study:

  • Free-floating planets (objects not orbiting any star)

  • Atmospheric chemistry

  • More distant planetary systems

This will help build a complete picture of how worlds form and evolve.

The Bigger Picture

This discovery reminds us that the universe still holds many secrets. Objects that look identical on the surface can have completely different origins.

By simply observing how fast something spins, scientists can now unlock its past—like reading a cosmic story written billions of years ago.

As technology improves and more powerful telescopes are built, we can expect even deeper insights into the hidden lives of planets and stars.

Conclusion

The difference between a giant planet and a brown dwarf is no longer just about size or brightness. It’s about motion—specifically, spin.

Thanks to advanced observations from the Keck Observatory and the work of dedicated scientists, we now know:

👉 Fast spin = likely a giant planet
👉 Slow spin = likely a brown dwarf

This simple yet powerful idea is changing how we understand the universe.

And as researchers continue exploring, one thing is certain—
every spinning world has a story to tell.

Learn more:

  • Read the article “ Distinct Rotational Evolution of Giant Planets and Brown Dwarf Companions ” in The Astronomical Journal , by Chih-Chun Hsu, Jason J. Wang, Jerry W. Xuan, Yapeng Zhang, Jean-Baptiste Ruffio, Dimitri Mawet, Luke Finnerty, Katelyn Horstman, Julianne Cronin, Yinzi Xin , Ben Sappey, Daniel Echeverri, Nemanja Jovanovic, Ashley Baker, Randall Bartos, Geoffrey A. Blake, Benjamin Calvin, Sylvain Cetre, Jacques-Robert Delorme, Gregory W. Doppmann, Michael P. Fitzgerald, Quinn M. Konopacky, Joshua Liberman, Ronald A. López, Evan Morris, Jacklyn Pezzato, Tobias Schofield, Andrew Skemer, J. Kent Wallace, and Ji Wang

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