Under pressure: How the density of exoplanets' atmospheres weighs on the odds for alien life

May 3, 2013 by Adam Hadhazy, Astrobio.net
Earth's atmosphere seen edge-on. Credit: NASA

At this early stage in the search for extraterrestrial life in our solar system and beyond, the emphasis is on liquid water. Where it can exist on a planet's or moon's surface, so the thinking goes, life as we know it has a chance. Much of the observational and theoretical work in astrobiology therefore concerns the "habitable zone," the orbital band around stars where a rocky world's water neither freezes away nor boils off.

In a new contribution to this effort, a recent study has looked at a little-explored influencer on the ability of water to remain liquid on a world's surface: .

"Atmospheric pressure affects the temperature range that is commonly used to define planetary ," said Giovanni Vladilo of the Trieste in Italy and lead author of the paper published in the Astrophysical Journal. "So, if you wish to estimate habitability, you should explicitly take into account pressure in your problem."

On Earth, the space around us is filled with that collectively weigh on our bodies. Although you cannot feel it, Earth's atmosphere presses down with the force of one kilogram per square centimeter, or 14.7 pounds per square inch. That pressure works out to about a ton per square foot. Our terrestrial biology evolved to operate in this pressure, which, while startling-sounding, pales when compared to ' bodies in the deep sea that can withstand dozens of tons per square foot.

Atmospheric pressure has an impact on water's boiling point when it transitions from a liquid to a gas. As anyone who has cooked at high altitudes has experienced, water boils there at a lower temperature than the typical 100 degrees Celsius (212 degrees Fahrenheit). The reason: Atmospheric pressure is lower at than at sea level; there is simply less atmosphere pressing down the higher you go up in the mountains. Lower pressure is why it takes a few minutes longer to make pasta in mile-high Denver than below-sea-level New Orleans—the pasta has to soak and soften in the water longer to become al dente in Denver because the water is boiling at a slightly lower temperature.

Vladilo explained why pressure has this effect. "Temperature is an indicator of the speed of molecular motions. The boiling point occurs when molecular motions are sufficiently fast to allow most molecules to escape from each other," and thus turn into gas, he said. "Pressure keeps molecules tight, so the higher the pressure, the faster the molecules must move—that is, the higher the temperature must be—for evaporation to occur."

Like Earth, give or take an atmosphere

In Vladilo's new paper, he and his colleagues modeled a planet just like Earth in size and atmospheric composition. They ran over 4,000 computer simulations that varied the model planet's atmospheric pressure from one-hundredth to six times the atmospheric pressure of Earth. The researchers also varied the virtual planet's orbital distance from its Sun-like star from about two-thirds of the Earth-Sun distance to around an additional third. To get a sense of these orbital parameters, the former is a bit tighter than Venus and the latter more than half the distance out to Mars.

The researchers' model estimated the global habitability of these Earth-like exoplanets by gauging the extent of the planet's latitudes that could possess liquid surface water.

A figure from Vladilo's paper summarizing the general findings. The area of the circles is proportional to their habitability. The bottom axis shows the virtual worlds' distance from their Sun-like star, with 1 AU (astronomical unit) representing the average Sun-Earth distance of approximately 150 million kilometers (93 million miles). The top axis (insolation) shows solar radiation (in watts) received on a unit area (a square meter). Surface pressure is on the y axis to the left. Credit: Vladilo et al. 2013, ApJ, 767, 65; http://wwwuser.oats.inaf.it/astrobiology/planhab/

Through their modeling, Vladilo and colleagues saw that the habitable zone expanded in width as the atmospheric pressure increased. At a tenth of Earth's atmospheric pressure, the outer edge of the habitable zone reached just two percent farther out than Earth; not a lot of wiggle room for a low-pressure, Earth-like world, in other words, when it comes to habitability. But as the atmospheric pressure increased to threefold that of Earth's, the habitable zone extended out a farther 18 percent.

For the same pressure interval, low-to-high, the inner edge of the habitable zone ranged from 87 percent of the Earth-Sun distance to 77 percent. In this model, for a planet with Earth's atmospheric pressure, cloudiness, and humidity, the inner edge of the habitable zone is smack dab in the middle of this range, at 82 percent of the Earth-Sun distance.

The results indicate that an exoplanet just like Earth in all other respects but with a higher atmospheric pressure could be considered habitable about five percent closer to its Sun-like star. Conversely, a low-pressure Earth would not be considered habitable unless placed in an orbit five percent farther out than a standard-pressure Earth.

The movement of heat

A main factor behind the expanded orbital range of habitability at higher pressures is that higher pressure atmospheres are denser. Denser atmospheres, in turn, transport heat better than thin atmospheres, and promote a stronger "greenhouse effect", whereby atmospheric gases absorb heat.

For exoplanets farther from their star than Earth is from our sun, and therefore receive less sunlight, a high-pressure atmosphere traps heat better and distributes the greater warmth received at the equator. Polar zones that would otherwise freeze instead retain liquid water. A high-pressure planet can remain warmer at farther distances from its star accordingly.

Temperatures on Earth as recorded by an infrared sensor on NASA's Aqua satellite. Credit: AIRS Science Team, NASA/JPL

With regards to low-pressure worlds—hearkening back to the pasta cooking analogy—water boils at lower temperatures than it does on higher atmospheric pressure worlds. In a low-pressure scenario, a world closer to its star than Earth that would otherwise be broadly habitable with Earth's atmospheric pressure would have its water boil off.

For closer-in exoplanets with a high atmospheric pressure, however, the sun-scorched equatorial zones would not heat to a boiling level as readily as in a normal- or low-pressure situation, and thus could still be habitable.

What might live there

In addition to these general findings, the researchers' model offers intriguing insights. For example, much of the gain in survivability on the closer-to-the-star side of the habitable zone for high-pressure worlds is for organisms that, at least by our Earthly standards, are extreme.

The global temperatures on these inner-edge worlds made habitable by their high atmospheric pressures would be too high for complex life forms such as ourselves. So-called thermophiles, however—bacteria that thrive at temperatures more than 45 degrees Celsius (113 degrees Fahrenheit) or so and on up to considerably higher temperatures—might find such heat-blasted worlds quite comfortable.

Overall, the habitable zone for creatures like us that require relatively moderate temperatures actually moves outward somewhat from a Sun-like star in high-pressure scenarios.

Atmospheric pressure could also have a profound effect on biodiversity. Compared to low-pressure worlds, high-atmospheric pressure exoplanets would have rather uniform global surface temperatures, again owing to the efficient transfer of heat amongst their latitudes. These heavy-atmosphere planets might host a fairly narrow range of life forms, since all would be adapted to the same slim temperature regime.

Planets with lower atmospheric pressures than Earth, though, would have even more varied temperatures than our planet. These abodes might then provide an even wider range of habitats than our world, with organisms exotically adapted to their considerably more intensely varied polar-temperate-tropical bands.

A close-up of thermophilic algae living in Yellowstone National Park. Credit: J Schmidt; 1977

Whence atmospheres?

For now, research on a "pressure-dependent " is somewhat purely academic, given that atmospheric pressure is not a property of exoplanets that we can yet measure. But Vladilo believes that work with planets several times larger than Earth, dubbed super-Earths, could be where the atmospheric pressure insights are first able to be applied.

"At the present time, observations are able to determine only a few properties of planetary atmospheres, such as their chemical composition, and mostly for giant planets rather than terrestrial ones," Vladilo said. "However, I'm confident that technological improvements will allow us to characterize, to some extent, the atmospheres of super-Earths, which are reasonable candidates for studies of planetary habitability. If we will be able to estimate some basic planet parameters with observations, such as the planetary albedo [the amount of light reflected by the surface] and infrared flux [the amount of infrared light emitted], then our models will be sufficiently constrained to yield a reasonable estimate of the planet surface pressure."

A major issue for assessing exoplanetary atmospheric pressures is the fact that the formation of atmospheres and the densities they develop is not well understood. Saturn's moon Titan, for instance, has a thick atmosphere with a pressure about 50 percent greater than that of Earth's. Yet similar bodies in the outer solar system, such as Jupiter's moons Ganymede and Callisto, cling to only very tenuous envelopes of gas.

"It's embarrassing that we have almost no idea of atmospheres and where they come from," said Sara Seager, a professor of planetary science and physics at the Massachusetts Institute of Technology who was not involved in the new study. "It's one of those thing we can hope and wait to learn about."

With regards to Vladilo's research, Seager said "it's refreshing to see that a wide range of surface pressures could enable a habitable surface."

Vladilo and his colleagues plan a number of follow-ups with their model. Other subtle aspects of exoplanetary habitability remain to be examined in the ever-expanding scientific literature that matches the growing excitement for possibly detecting alien life in the near future.

Said MIT's Seager: "The uptick in papers on planetary habitability is a telling sign of what's to come."

Explore further: Potential survival of extreme life forms on eccentric exoplanets

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4.2 / 5 (5) May 03, 2013
Why would one planet have a higher atmospheric pressure/density than another? It isn't gravity, or magnetic field. Venus is smaller than Earth (less gravity), and has almost no magnetic field. Yet its surface pressure is 90 bar! And how would you find out the history of atmospheric pressure on a particular planet? Is there an indicator? This is going to be a tough but important field of study.
2.8 / 5 (4) May 03, 2013
Why would one planet have a higher atmospheric pressure/density than another? It isn't gravity, or magnetic field. Venus is smaller than Earth (less gravity), and has almost no magnetic field. Yet its surface pressure is 90 bar! And how would you find out the history of atmospheric pressure on a particular planet? Is there an indicator? This is going to be a tough but important field of study.

Actually it is gravity AND the amount of atmosphere,,,, the pressure in weight of all the molecules pressing down in response to gravity. If ya have an equal mass, Earth and Venus are close, within a factor of 0.1 of each other, then if ya have 90 times more stuff making up the atmosphere, ya will have 90 times more pressure. If the mass of the atmosphere is great enough, as in Jupiter, as ya go down lower and lower, the pressure gets greater until ya gradually find yourself in something getting denser and denser until it seems like a fluid solid.
5 / 5 (1) May 04, 2013
Nice to see that high pressure worlds do indeed make for better habitability! An obvious follow up would be tracking the HZ as a young sun matures (our own sun had ~ 70 of today's irradiance originally). Another one would be checking the model on Mars.

Mars were early habitable, but with a young Sun and a remote distance balancing a predominantly CO2 atmosphere. Curiosity's D/H isotope ratios amend the Viking's spread and the martian meteorite extremes to something like ~ 1/10 Earth atmospheres original pressure. It is hard to see how this model predicts a habitable Mars!
5 / 5 (1) May 04, 2013
Our extremophiles are likely temperature constrained by the pressure of the atmosphere and oceans their ancestors evolved in.

Seager, see the article, has a new article out extending habitable zones inwards. They find that dry planets, no vapor atmosphere cloud greenhouse effect, would be habitable furthest in and use the convenient fact that nucleotides and amino acids both goes into rapid decomposition in water (hydrolysis) first at ~ 500 K at high pressures.

So our extremophiles may easily be beaten by high pressure worlds extremophiles for pressure _and_ temperature. I, for one, bow to Seager's Galactic Extremophile Overlords.

5 / 5 (1) May 04, 2013
@Roland: The main pressure factor would be distance from the star. The reason Titan has a dense atmosphere is because its scale height is large, ~ 40 km vs ~ 10 km for Earth. [Various Wikipedia articles.] This in turn comes out of its low temperature (lower irradiation) and much smaller solar wind, both due to distance.

Similarly the main volatile supply factor should, everything else alike, be distance from the star. The ice line gives outer terrestrials (ice moons) a lot of volatiles.

Venus and Earth are special since they seem marginal for plate tectonics. Venus have none, Earth does. We know that a major factor is water, which makes the mantle much more pliable.

The main theory as far as I know is that early Venus was akin to Earth, but with no magnetic field lost water by UV hydrolysis and hydrogen escape. If plate tectonics never got started or closed down from having water lost from the mantle, there would be no sedimentation keeping carbon out of the atmosphere. ...
5 / 5 (1) May 04, 2013
.... It too would cook out from the mantle, and the carbon and remaining oxygen would form CO2, keeping Venus a dry greenhouse.

This would not then likely not have happened on a more massive terrestrial, which a) ensures plate tectonics, b) likely ensures global magnetic fields by at least active mantle convection*.

* The jury is out on that one. Too large, and the magnetic field may shut down due to complicated reasons. But I don't think anyone knows for sure.
4 / 5 (1) May 04, 2013
Errata: It is the products (polymers) of Ns and AAs that decomposes at that temp&press (re extremophiles), I believe.

The idea would be that since Archaea, Bacteria and Eukrayotes all diversified after the DNA LUCA was in place, they are constrained by the chosen genetic system as for temperature. Modifications only get you so far, you could feasibly had a more radical temperature hardened system evolve as a starting point in a high pressure ocean with heat sources like hydrothermal vents.

2.3 / 5 (3) May 05, 2013
When you look at the narrow bandwidth of properties providing for the habitability of known life, you are left with the impression that even under such limiting constraints complexity and diversity is a rule not an exception.
2.3 / 5 (4) May 06, 2013
"...about a ton per square foot. Our terrestrial biology evolved to operate in this pressure,..."


But ~4 billion yrs ago when life either started or traveled here the atmospheric pressure was likely >200 bar. Since gravity didn't change much since then and the temperature only fluctuated a relatively small amount, this pressure can be calculated from the measured amount of air bleeding off into space today.

(one gets a similar pressure for Mars too)
1 / 5 (1) May 07, 2013
Thought provoking is the role pressure can be considered in relationships to sizes and evolutions of known life.
Under identical conditions one ponders over an experiment what fast dividing bacteria does and how bacteria reacts when varying only the pressure from one generation to the next.

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