Neptune-Like Planets Could Transfom Into Habitable Worlds

In a paper published this month in the journal Astrobiology,

UW doctoral student Rodrigo Luger and co-author Rory Barnes, research

assistant professor, say the two forces could combine to transform

uninhabitable “mini-Neptunes” — big planets in outer orbits with solid

cores and thick hydrogen atmospheres — into closer-in, gas-free,

potentially habitable worlds.

Most of the stars in our galaxy are low-mass stars, also called M

dwarfs. Smaller and dimmer than the sun, with close-in habitable zones,

they make good targets for finding and studying potentially habitable

planets. Astronomers expect to find many Earthlike and “super-Earth”

planets in the habitable zones of these stars in coming years, so it’s

important to know if they might indeed support life.

Super-Earths are planets greater in mass than our own yet smaller

than gas giants such as Neptune and Uranus. The habitable zone is that

swath of space around a star that might allow liquid water on an

orbiting rocky planet’s surface, perhaps giving life a chance.

“There are many processes that are negligible on Earth but can affect

the habitability of M dwarf planets,” Luger said. “Two important ones

are strong tidal effects and vigorous stellar activity.”

A tidal force is a star’s gravitational tug on an orbiting planet,

and is stronger on the near side of the planet, facing the host star,

than on the far side, since gravity weakens with distance. This pulling

can stretch a world into an ellipsoidal or egglike shape as well as

possibly causing it to migrate closer to its star.

“This is the reason we have ocean tides on Earth, as tidal forces

from both the moon and the sun can tug on the oceans, creating a bulge

that we experience as a high tide,” Luger said. “Luckily, on Earth it’s

really only the water in the oceans that gets distorted, and only by a

few feet. But close-in planets, like those in the habitable zones of M

dwarfs, experience much stronger tidal forces.”

This stretching causes friction in a planet’s interior that gives off

huge amounts of energy. This can drive surface volcanism and in some

cases even heat the planet into a runaway greenhouse state, boiling away

its oceans, and all chance of habitability.

Vigorous stellar activity also can destroy any chance for life on

planets orbiting low-mass stars. M dwarfs are very bright when young and

emit lots of high-energy X-rays and ultraviolet radiation that can heat

a planet’s upper atmosphere, spawning strong winds that can erode the

atmosphere away entirely. In a recent paper, Luger and Barnes showed

that a planet’s entire surface water can be lost due to such stellar

activity during the first few hundred million years following its

formation.

“But things aren’t necessarily as grim as they may sound,” Luger

said. Using computer models, the co-authors found that tidal forces and

atmospheric escape can sometimes shape planets that start out as

mini-Neptunes into gas-free, potentially habitable worlds.

How does this transformation happen?

Mini-Neptunes typically form far from their host star, with ice

molecules joining with hydrogen and helium gases in great quantity to

form icy/rocky cores surrounded by massive gaseous atmospheres.

“They are initially freezing cold, inhospitable worlds,” Luger said.

“But planets need not always remain in place. Alongside other processes,

tidal forces can induce inward planet migration.” This process can

bring mini-Neptunes into their host star’s habitable zone, where they

are exposed to much higher levels of X-ray and ultraviolet radiation.

This can in turn lead to rapid loss of the atmospheric gases to

space, sometimes leaving behind a hydrogen-free, rocky world smack dab

in the habitable zone. The co-authors call such planets “habitable

evaporated cores.”

“Such a planet is likely to have abundant surface water, since its

core is rich in water ice,” Luger said. “Once in the habitable zone,

this ice can melt and form oceans,” perhaps leading to life.

Barnes and Luger note that many other conditions would have to be met

for such planets to be habitable. One is the development of an

atmosphere right for creating and recycling nutrients globally.

Another is simple timing. If hydrogen and helium loss is too slow

while a planet is forming, a gaseous envelope would prevail and a rocky,

terrestrial world may not form. If the world loses hydrogen too

quickly, a runaway greenhouse state could result, with all water lost to

space.

“The bottom line is that this process — the transformation of a

mini-Neptune into an Earthlike world — could be a pathway to the

formation of habitable worlds around M dwarf stars,” Luger said.

Will they truly be habitable? That remains for future research to learn, Luger said.

“Either way, these evaporated cores are probably lurking out there in

the habitable zones of these stars, and many may be discovered in the

coming years.”

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Neptune-Like Planets Could Transfom Into Habitable Worlds