Astronomers have identified two different cases of "mini-Neptune" planets that are losing their puffy atmospheres and likely transforming into super-Earths. Radiation from the planets' stars is stripping away their atmospheres, driving hot gas to escape like steam from a pot of boiling water.
The findings, published in two separate papers in The Astronomical Journal, help paint a picture of how exotic worlds like these form and evolve.
Mini-Neptunes are a class of exoplanets, which are planets that orbit stars outside our solar system. These worlds, which are smaller, denser versions of the planet Neptune, consist of large rocky cores surrounded by thick blankets of gas. In the new studies, a team of astronomers led by Caltech used the W. M. Keck Observatory atop Maunakea in Hawaiʻi to study one of two mini-Neptune planets in the star system called TOI 560, located 103 light-years away; and they used NASA's Hubble Space Telescope to look at two mini-Neptunes orbiting HD 63433, located 73 light-years away.
Their results show that atmospheric gas is escaping from the innermost mini-Neptune in TOI 560, called TOI 560.01, and from the outermost mini-Neptune in HD 63433, called HD 63433 c. This suggests that they could be turning into super-Earths.
"Most astronomers suspected that young, small mini-Neptunes must have evaporating atmospheres," says Michael Zhang, lead author of both studies and a graduate student at Caltech. "But nobody had ever caught one in the process of doing so until now."
The study also found, surprisingly, that the gas around TOI 560.01 was escaping predominantly toward the star.
"This was unexpected, as most models predict that the gas should flow away from the star," says Professor of Planetary Science Heather Knutson, Zhang's advisor and a co-author of the study. "We still have a lot to learn about how these outflows work in practice."
Planetary Gap Explained
Since the first exoplanets orbiting sun-like stars were discovered in the mid-1990s, thousands of others have been found. Many of these orbit close to their stars, and the smaller, rocky ones generally fall into two groups: mini-Neptunes and super-Earths. Planets of these types are not found in our solar system. The super-Earths are as large as 1.6 times the size of Earth (and occasionally as large as 1.75 times the size of Earth), while the mini-Neptunes are between two and four times the size of Earth. Few planets with sizes between these two planet types have been detected.
One possible explanation for this gap is that mini-Neptunes are transforming into super-Earths. Mini-Neptunes are theorized to be cocooned by primordial atmospheres made of hydrogen and helium. The hydrogen and helium are left over from the formation of the central star, which is born out of clouds of gas. If a mini-Neptune is small enough and close enough to its star, stellar X-rays and ultraviolet radiation can strip away its primordial atmosphere over a period of hundreds of millions of years, scientists theorize. This would then leave behind a rocky super-Earth with a substantially smaller radius, which could, in theory, still retain a relatively thin atmosphere similar to that surrounding our own planet.
"A planet in the gap would have enough atmosphere to puff up its radius, making it intercept more stellar radiation and thereby enabling fast mass loss," Zhang says. "But the atmosphere is thin enough that it gets lost quickly. This is why a planet wouldn't stay in the gap for long."
Other scenarios could explain the gap, according to the astronomers. For instance, the smaller rocky planets might have never gathered gas envelopes in the first place, and mini-Neptunes could be water worlds and not enveloped in hydrogen gas. This latest discovery of two mini-Neptunes with escaping atmospheres represents the first direct evidence to support the theory that mini-Neptunes are indeed turning into super-Earths.
Signatures in the Sunlight
The astronomers were able to detect the escaping atmospheres by watching the mini-Neptunes cross in front of, or transit, their host stars. The planets cannot be seen directly, but when they pass in front of their stars as seen from our point of view on Earth, telescopes can look for absorption of starlight by atoms in the planets' atmospheres. In the case of the mini Neptune TOI 560.01, the researchers found signatures of helium. For the star system HD 63433, the team found signatures of hydrogen in the outermost planet they studied, called HD 63433 c, but not the inner planet, HD 63433 b.
"The inner planet may have already lost its atmosphere," Zhang explains.
The speed of the gases provided the evidence that the atmospheres are escaping. The observed helium around TOI 560.01 is moving as fast as 20 kilometers per second, while the hydrogen around HD 63433 c is moving as fast as 50 kilometers per second. The gravity of these mini-Neptunes is not strong enough to hold on to such fast-moving gas. The extent of the outflows around the planets also pointed to escaping atmospheres: the cocoon of gas around TOI 560.01 is at least 3.5 times as large as the radius of the planet, and the cocoon around. HD 63433 c is at least 12 times the radius of the planet.
The observations additionally revealed that the gas lost from TOI 560.01 was flowing toward the star. Future observations of other mini-Neptunes should reveal if TOI 560.01 is an anomaly or whether an inward-moving atmospheric outflow is more common.
"As exoplanet scientists, we've learned to expect the unexpected," Knutson says. "These exotic worlds are constantly surprising us with new physics that goes beyond what we observe in our solar system."
The Astronomical Journal study titled "Escaping Helium from TOI 560.01, a Young Mini Neptune" was funded by NASA. Other authors include Lile Wang of the Flatiron Institute, Fei Dai of Caltech, and Oscar Barragán of the University of Oxford.
The Astronomical Journal study titled "Detection of Ongoing Mass Loss from HD 63433c, a Young Mini Neptune" was funded by NASA, European Research Council, Science and Technology Facilities Council (U.K.), National Center for Space Studies (French Space Agency), National Science Foundation, Tennessee State University, and Tennessee's Centers for Excellence Program. Other authors of this paper include Wang and Dai from the first paper, Leonardo dos Santos of the Space Telescope Science institute and University of Geneva; Luca Fossati of the Austrian Academy of Sciences; Gregory Henry of Tennessee State University; David Ehrenreich of University of Geneva; Yann Alibert of University of Bern; Sergio Hoyer of Aix-Marseille University; Thomas Wilson of the University of St. Andrews; and Andrea Bonfanti of the Space Research Institute and Austrian Academy of Sciences.