JWST observations of the ultra-hot super-Earth exoplanet TOI-561 b provide the strongest evidence to date for an atmosphere surrounding a rocky planet beyond our Solar System.
A team of astronomers led by Carnegie researchers has uncovered the clearest evidence so far that a rocky planet outside our Solar System possesses an atmosphere. The findings, reported in The Astrophysical Journal Letters, are based on observations from NASA’s James Webb Space Telescope (JWST). The data point to the presence of an atmosphere on an unlikely world: an ancient, extremely hot super-Earth that is thought to be covered by a global ocean of molten rock.
The planet, called TOI-561 b, is roughly twice as massive as Earth but is otherwise very different from our planet. Its extreme conditions are driven by its tight orbit around its star. While the star itself is slightly smaller and cooler than the Sun, TOI-561 b circles it at just one fortieth the distance between Mercury and the Sun. Because of this close orbit, the planet completes a full year in only 10.56 hours, and one hemisphere is constantly exposed to starlight.
“Based on what we know about other systems, astronomers would have predicted that a planet like this is too small and hot to retain its own atmosphere for long after formation,” explained Carnegie Science Postdoctoral Fellow Nicole Wallack, the paper’s second author. “But our observations suggest it is surrounded by a relatively thick blanket of gas, upending conventional wisdom about ultra-short-period planets.”
Challenging Planetary Expectations
Within our own Solar System, planets that are both small and intensely heated were unable to keep the original gaseous envelopes they acquired early in their histories. In contrast, TOI-561 b appears to have held on to its atmosphere even though it orbits a star that is much older than the Sun.
This lingering atmosphere may also account for another puzzle: the planet’s surprisingly low density. Despite being rocky, TOI-561 b is lighter than scientists would expect based on its size alone, and the presence of an atmosphere could help explain why.
“It’s not what we call a super-puff—or ‘cotton candy’ planet—but it is less dense than you would expect if it had an Earth-like composition,” explained Carnegie Science astronomer Johanna Teske, the paper’s lead author.
In designing the observing program, the team considered that the planet’s low density could be explained by a relatively small iron core and a mantle made of rock that is less dense than the rocks that comprise Earth’s interior.
Teske notes that this could make sense: “TOI-561 b is distinct among ultra-short period planets in that it orbits a very old—twice as old as the Sun—iron-poor star in a region of the Milky Way known as the thick disk. It must have formed in a very different chemical environment from the planets in our own Solar System.”
This means that its composition could be representative of planets that formed when the universe was relatively young.
But an exotic interior composition can’t explain everything.
Searching for an Atmosphere
In deciding to study TOI-561 b, the research team also suspected that it might be surrounded by a thick atmosphere that makes it look larger and thus less dense.
To test the existence of TOI-561 b’s atmosphere, the astronomers used JWST’s Near-Infrared Spectrograph (NIRSpec) instrument to measure the planet’s dayside temperature based on its brightness in the near-infrared. The technique, which involves measuring the decrease in brightness of the star-planet system as the planet moves behind the star, is similar to that used to search for atmospheres in the TRAPPIST-1 system and on other rocky worlds.
If TOI-561 b were a bare rock with no atmosphere to carry heat around to the nightside, its dayside temperature should be approaching 4,900 degrees Fahrenheit (2,700 degrees Celsius). But the NIRSpec observations show that the planet’s dayside appears to be closer to 3,200 degrees Fahrenheit (1,800 degrees Celsius)—still extremely hot, but far cooler than expected.
To explain the results, the team considered a few different scenarios. The magma ocean could circulate some heat, but without an atmosphere, the nightside would probably be solid, limiting flow away from the dayside. A thin layer of rock vapor on the surface of the magma ocean is also possible, but on its own would likely have a much smaller cooling effect than observed.
“We really need a thick volatile-rich atmosphere to explain all the observations,” said co-author Anjali Piette, of University of Birmingham, United Kingdom—a former Carnegie Science Postdoctoral Fellow. “Strong winds would cool the dayside by transporting heat over to the nightside. Gases like water vapor would absorb some wavelengths of near-infrared light emitted by the surface before they make it all the way up through the atmosphere. (The planet would look colder because the telescope detects less light.) It’s also possible that there are bright silicate clouds that cool the atmosphere by reflecting starlight.”
How Does the Atmosphere Survive?
While JWST’s observations provide compelling evidence for such an atmosphere, the question remains: How can a small planet exposed to such intense radiation hold on to any atmosphere at all, let alone one so substantial? Some gases must be escaping to space, but perhaps not as efficiently as expected.
“We think there is an equilibrium between the magma ocean and the atmosphere. At the same time that gases are coming out of the planet to feed the atmosphere, the magma ocean is sucking them back into the interior,” said co-author Tim Lichtenberg from the University of Groningen in the Netherlands, who is also a member of the Carnegie-led Atmospheric Empirical Theoretical and Experimental Research (AEThER) project team. “This planet must be much, much more volatile-rich than Earth to explain the observations. It’s really like a wet lava ball.”
Concluded Teske: “What’s really exciting is that this new data set is opening up even more questions than it’s answering.”
JWST Observations and Future Work
These are the first results from JWST’s General Observers Program 3860, which involved observing the system continuously for more than 37 hours while TOI-561 b completed nearly four full orbits of the star. The team is currently analyzing the full data set to map the temperature all the way around the planet and narrow down the composition of the atmosphere.
Teske and Wallack’s leadership on this JWST paper represents a tradition of Carnegie Science excellence dating back to the mission’s earliest conception three decades ago and extending through the first four cycles of time allocation on the revolutionary space telescope.
Since JWST finished calibrations and began collecting data for astronomical research programs, Teske, Wallack, and other Carnegie Earth and Planets Laboratory and Observatories-affiliated scientists have led more than a dozen JWST teams and announced groundbreaking results about exoplanet atmospheres, galaxy formation, and more.
“These JWST-powered breakthroughs tap directly into our long-standing strength in understanding how exoplanet characteristics are shaped by planetary evolution and dynamics,” said Earth and Planets Laboratory Director Michael Walter. “There are more exciting results on the horizon and we’re poised for a new wave of Carnegie-led JWST science in the year ahead.”
Reference: “A Thick Volatile Atmosphere on the Ultrahot Super-Earth TOI-561 b” by Johanna K. Teske, Nicole L. Wallack, Anjali A. A. Piette, Lisa Dang, Tim Lichtenberg, Mykhaylo Plotnykov, Raymond Pierrehumbert, Emma Postolec, Samuel Boucher, Alex McGinty, Bo Peng, Diana Valencia and Mark Hammond, 11 December 2025, The Astrophysical Journal Letters.
DOI: 10.3847/2041-8213/ae0a4c
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