The methane habitable zone

The methane habitable zone
Our planet is at just the right distance from the Sun for liquid water to exist on its surface and play a role in life. Image: NASA

In the search for life elsewhere, many studies focus on finding liquid water. But what if life could exist with some other solvent? Saturn’s smoggy moon Titan makes scientists question the possibilities for methane-based life in the galaxy.

The search for is largely limited to the search for – we look for exoplanets at the correct distance from their stars for to splash and flow freely on their surfaces, we ‘follow the water’ on the red planet Mars, and SETI scans radio frequencies in the ‘water hole’ between the 1,420MHz emission line of neutral hydrogen and the 1,666MHz hydroxyl line.

There are two very good reasons why our attention is so strongly focused on water. First, it’s an efficient solvent for biological chemistry, allowing molecules to move around in cells, and has properties that are friendly to life – a high heat capacity, the ability to remain in liquid form across a wide temperature range, and a molecular density that forces molecules to organize themselves, rather than the water organizing around the molecules. Secondly, the biosignatures of a water-based chemistry are a lot easier for us to identify remotely.

Moreover, the most important fact about water’s relationship with life is that it is here on Earth. “Some argue that is the only important thing about water,” says Chris McKay of NASA’s Ames Research Center. McKay is an astrobiologist and planetary scientist who specializes in hunting down alien environments and then asking the question, ‘could something live here?’, rather than deciding what is and isn’t habitable beforehand.

“We live on a planet where water is a liquid and we have adapted and evolved to work with that liquid,” he says. “Life has very cleverly used the properties of water to do things not just in terms of solution, but in using the strong polarity of that solution to its advantage in terms of hydrophobic and hydrophilic bonds, and using the very structure of water to help align molecules.”

Suppose, though, that life needn’t be constrained to a water-based chemistry; would we be able to recognize the signatures of such life and the habitats in which it lives? From one perspective, water seems such a good match for life because it may be the only match – no other liquid has the properties or abundance that water has. On the other hand there is another point of view that says there is more to the story, and that life simply works with whatever materials it has at hand. On Earth, that material is water, but on other planets it may be something else. Already we have discovered another world, in our Solar System, where rivers and lakes are made with a quite different liquid.

Titan’s Liquid for Life?

One point four billion kilometers from the Sun orbits Saturn, the majestic ringed planet. Saturn is a gaseous world with an atmosphere of hydrogen and helium, and no discernible rocky surface below. However, among its retinue of icy moons is Titan, bigger than the planet Mercury and swathed in a dense cloak of hydrocarbon smog suspended in its nitrogen-rich atmosphere. It’s the only moon in the Solar System to have an atmosphere, and it has intrigued astronomers ever since Gerard Kuiper detected methane there in 1944.

The methane habitable zone
Sunlight glints off a methane lake at near Titan’s north pole in this five-micron infrared image taken by the Cassini spacecraft. Image: NASA/JPL/University of Arizona/DLR

When the joint NASA–ESA Cassini–Huygens mission arrived in the Saturnian system in 2004, the truth about Titan was revealed. Infrared cameras and radar on Cassini showed a world riven by black, oily rivers and lakes, whilst the Huygens probe plunged through the opaque atmosphere to land on a soggy floodplain, but not one damp with water. On Titan, where the temperature is just 94 degrees above absolute zero (–179 degrees Celsius) water is as solid as rock and runs through the river valleys and into the high latitude polar lakes. Instead of a water cycle, Titan has a methane cycle, and a complex molecular soup formed from reactions in the upper atmosphere between ultraviolet radiation from the Sun and methane.

Suppose life could exist in an environment like this; it would be a whole new category of habitable planet, one where liquid methane replaces liquid water, consequently leading to an entirely different habitable zone, one that is farther out from a star than the liquid water zone.

McKay is already ahead of the game. Along with Ashley Gilliam of NASA Ames and the University of California, Santa Cruz, he published a paper in the journal Planetary and Space Science in April that describes where a world with temperatures suitable for liquid methane could be found around a red dwarf star.

Methane Worlds

Red dwarfs – also called M-dwarfs after of their classification on the Hertzsprung–Russell diagram – are stars that are smaller and cooler than our Sun, and therefore the planetary systems around them are scaled down accordingly. McKay and Gilliam calculate that a planet would have a surface temperature of –179 degrees Celsius in a zone between 0.63 and 1.66 astronomical units (99 million and 248 million kilometers around the star Gliese 581, an M3-type red dwarf located 20.5 light years away. Four planets have already been confirmed orbiting Gliese 581, but none within the ‘liquid methane habitable zone’. Two more planets have been claimed to exist in the system, and one of these would fall within the zone, at 0.76 astronomical units, but evidence for the existence of this world has proven highly controversial. Alternatively, the liquid methane habitable zone around a cooler M4 type red dwarf would be even closer in, between 0.084 astronomical units and 0.23 astronomical units (12.6 million kilometers to 34.4 million kilometers.

Cold, methane-dominated worlds could easily exist around Sun-like stars, and Titan is proof of that. But there are advantages to finding these worlds around red dwarfs instead. First, their small orbital radii make them easier to detect, whether by transits or via radial velocity Doppler shifts. Second, Titan’s atmosphere is opaque to blue and ultraviolet light, but transparent to red and infrared light, and red dwarfs produce more of the latter than the former. If Titan orbited a red dwarf, more red light would seep through to its surface, warming the planet and extending the range of the liquid methane habitable zone. (Interestingly, a red giant, which is close to the endpoint in the life cycle of a Sun-like star, produces light of similar red wavelengths. When our Sun expands into a bloated red giant in about five billion years, engulfing all the planets up to Earth and possibly Mars, Titan may well reap the benefits – for a short while at least before the red giant puffs away to leave behind a white dwarf star.)

The methane habitable zone
Comparison of the habitable zone in the Solar System and the habitable zone around Gliese 581. Because Gliese 581 is a cooler red dwarf, its liquid water habitable zone is closer in, while its liquid methane habitable zone would be between 0.63 and 1.66 astronomical units. Image: ESO

Red dwarfs are also often highly magnetically active, and experience large stellar flares that emit powerful bursts of ultraviolet radiation. While these flares should not irreversibly damage exoplanet atmospheres, according to research led by Antigona Segura of Universidad Nacional Autonoma de Mexico, they could have a different kind of impact on Titan-esque atmospheres, disassociating molecules to create a haze like we see shrouding ’s largest moon. The more active the red dwarf, the more hazy the atmosphere of a Titan-like planet becomes, and the thicker the haze, the colder the surface and the closer to the star the liquid methane habitable zone has to be.

Greater or lesser haze also would alter the outward appearance of such a world, and if we are to one day hunt for habitable planets in the liquid methane habitable zone, we’ll need to know what they will look like, as well as what biosignatures to search for. It is here that the main stumbling block lies.

“We just don’t know what the tell-tale signs for life would be in such an atmosphere because it is so vastly different from ours,” says Lisa Kaltenegger, who conducts research into habitable exoplanets at the Max Planck Institute in Germany and at the Harvard–Smithsonian Center for Astrophysics. “That said, it will change in a flash if Chris [McKay] finds life on Titan and can tell us what it produces and what we could look for remotely with a telescope.”

Proof of Life

However, McKay already has a few suggestions and, tantalizingly, there may even be supporting evidence from Titan. In 2005 he published a paper with Heather Smith of the International Space University in Strasbourg, building on work by Steven Benner of the University of Florida, describing how methane-based life forms on Titan (‘methanogens’) could consume hydrogen, acetylene and ethane, and exhale methane instead of carbon-dioxide. If such a life form existed, it could reveal itself through a depletion of hydrogen, acetylene and ethane at the surface.

Amazingly, this is what studies of this moon have actually shown, but McKay himself is dubious that these measurements necessarily mean there is life on Titan. Rather, he points to other, more likely explanations including mistakes in the modeling of Titan’s atmosphere upon which these measurements are partially derived, to unknown physical processes occurring on Titan that are not related to life. In regards to using this formula to search for life elsewhere, the depletion of hydrogen, acetylene and ethane on the surface of a hazy planet are not conducive to remote spectroscopic imaging from many light years away.

“It’s not clear that we would be able to see the depletion of hydrogen over interstellar distances,” says McKay. “On Earth, of course, the big biosignature that is visible over interstellar distances is the build-up of oxygen, but even that is not an unambiguous indicator for life, because for most of Earth’s history there has been life but no build-up of oxygen.”

Nevertheless, Jonathan Lunine of the University of Arizona has speculated that there are many more exo-Titans than exo-Earths out there. If Chris McKay is right about methane-based life, such habitats could vastly outnumber planets with water-based life. The trouble is, the cold temperatures in which liquid methane exists would result in life forms with very slow metabolisms. Life would be sluggish. Is there any way it could be warmed up?

“You would have to invoke a lot of pressure to keep methane liquid at warmer temperatures,” says Kaltenegger. “And if you think about it, water and carbon are extremely abundant. So if you make the planet warmer, you are much more likely to get carbon dioxide than methane, and methane would go out of its liquid phase so you wouldn’t have the triple point [where for a given temperature and pressure a material can exist as a liquid, solid or gas] like the triple point of water on Earth.”

Other Solutions

If warm liquid methane is out of the question, what other potential substitutes for water are there? Hydrogen fluoride comes close to the properties of liquid water, but fluoride is relatively rare in the Universe and so is unlikely to play a major factor in life. More common is salt: if temperatures are hot enough, salts will become liquid.

“I can imagine a world where there is sodium chloride liquid and salt is somehow the basis for life,” says McKay, but he admits it is speculative. Rather than spending too much time on outlandish ideas, he believes it’s better to search for the environments first, and then ask, can anything live there?

Lisa Kaltenegger shares the same philosophy. “First we have to figure out using models what it takes for a planet to be habitable, and then we look at the data that comes in about such worlds and see how far we can stretch the habitable definition.”

Yet of the nearly 700 confirmed exoplanets so far (not counting all the unconfirmed candidate worlds detected by NASA’s Kepler mission) only two are potentially suitable for liquid water, and that’s only on the condition that circumstances on the planets themselves are perfect. As for liquid methane, without some hard data on the properties of methane-based life, astronomers are going to err on the side of caution. Even McKay still favors searching for water-based life and habitats.

“We know water works, it’s something that we understand,” he says. “Although I argue that we should consider liquid methane, we don’t know that it works. In that sense we’re still guessing.”

We may be kept guessing until the next mission to Titan, which may not happen until the 2030s. Just as Earth is the template for water-based habitats, Titan is the template for methane-based habitats. However, unless life can be shown to exist there, liquid methane habitable zones will always be passed over in favor of watery zones. Unfortunately, we may be missing a huge chunk of life in the process.


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