by Neil deGrasse Tyson
From Natural History Magazine, May 1998
From the looks of some dry and unfriendly-looking places in our solar system, you might think that water, while plentiful on Earth, is a rare commodity elsewhere in the galaxy. But of all molecules with three atoms, water is by far the most abundant. And in a ranking of the cosmic abundance of elements, water's constituents of hydrogen and oxygen are one and three in the list. So rather than ask why some places have water, we may learn more by asking why all places don't.
Starting in the solar system, if you seek a waterless, airless place to visit then you needn't look farther than Earth's Moon. Water swiftly evaporates in the Moon's near-zero atmospheric pressure and its two-week-long, 200 degree Fahrenheit days. During the two-week night, the temperature can drop to 250 degrees below zero, a condition that would freeze practically anything.
The Apollo astronauts brought with them to and from the Moon all the air and water (and air conditioning) they needed for their round-trip journey. But missions in the distant future may not need to bring water or assorted of products derived from it. Recent evidence from the Clementine lunar orbiter strongly supports a long-held contention that there may be frozen lakes lurking at the bottom of deep craters near the Moon's north and south poles. Assuming the Moon suffers an average number of impacts per year from interplanetary flotsam, then the mixture of impactors should include sizable water-rich comets. How big? The solar system contains plenty of comets that, when melted, could make a puddle the size of lake Erie.
While one wouldn't expect a freshly laid lake to survive many sun-baked lunar days at 200 degrees, any comet that happened to crash in the bottom of a deep crater near the poles (or happened to make a deep polar crater itself), would remain in darkness because deep craters near the poles are the only places on the Moon where the
Sun don't shine. (If you otherwise thought the Moon had a perpetual dark side then you have been badly misled by many sources, no doubt including Pink Floyd's 1973 best-selling rock album Dark Side of the Moon.) As light-starved Arctic and Antarctic dwellers know, the Sun never gets very high in the sky at any time of day or year. Now imagine living in the bottom of a crater whose rim was higher than the highest level the Sun ever reached. In such a crater on the Moon, where there is no air to scatter sunlight into shadows, you would live in eternal darkness.
But ice evaporates even in cold darkness. Just look at cubes in your freezer's ice tray after you've come back from a long vacation: they'll be distinctly smaller than when you last looked. But if the ice is well mixed with solid particles (as in a comet), it can survive for thousands and millions of years at the bottom of the Moon's deep polar craters. No doubt about it, if we were ever to establish an outpost on the Moon it would benefit greatly from being located near this lake. Apart from the obvious advantages of having ice to melt, filter, then drink, you can also dissociate the water's hydrogen from its oxygen. Use the hydrogen and some of the oxygen as active ingredients in rocket fuel and keep the rest of the oxygen for breathing. And in your spare time between space missions, you can always go ice skating on the frozen lake.
Knowing that the Moon has been hit by impactors, as its pristine record of craters tells us, then one might expect Earth to have been hit too. Given Earth's larger size and stronger gravity, one might even expect us to have been hit many more times. It has been—from birth, all the way to present day. In the beginning, Earth didn't just hatch from an interstellar void as a preformed spherical blob. It grew from the condensing protosolar gas cloud from which the other planets and the Sun were formed. Earth continued to grow by accreting small solid particles and eventually through incessant impacts with mineral-rich asteroids and water-rich comets. How incessant? The early impact rate of comets is suspected of being high enough to have delivered Earth's entire oceanic supply of water. But uncertainties (and controversies) remain. When compared with the water in Earth's oceans, the water in comets observed today is anomalously high in deuterium, a form of hydrogen that packs one extra neutron in its nucleus. If the oceans were delivered by comets, then the comets available to hit Earth during the early solar system must have had a somewhat different chemical profile.
And just when you thought it was safe to go outside, a recent study on the water level in Earth's upper atmosphere suggests that Earth regularly gets slammed by house-sized chunks of ice. These interplanetary snowballs swiftly vaporize on impact with the air, but they too contribute to Earth's water budget. If the observed rate has been constant over the 4.6 billion-year history of Earth, then these snowballs may also account for the world's oceans. When added to the water vapor that we know is out-gassed from volcanic eruptions, we have no shortage of ways that Earth could have acquired its supply of surface water.
Our mighty oceans now comprise over two thirds of Earth's surface area, but only about one five thousandth of Earth's total mass. While a small fraction of the total, the oceans weigh in at a hefty 1.5 quintillion tons, two percent of which is frozen at any given time. If Earth ever suffers a runaway greenhouse effect (like what has happened on Venus), then our atmosphere would trap excess amounts of solar energy, the air temperature would rise, and the oceans would swiftly evaporate into the atmosphere as they sustained a rolling boil. This would be bad. Apart from the obvious ways that Earth's flora and fauna will die, an especially pressing cause of death would result from Earth's atmosphere becoming 300 times more massive as it thickens with water vapor. We would all be crushed.
Many features distinguish Venus from the other planets in the solar system, including its thick, dense, heavy atmosphere of carbon dioxide that imparts 100 times the pressure of Earth's atmosphere. We would all get crushed there too. But my vote for Venus's most peculiar feature is the presence of craters that are all relatively young and uniformly distributed over its surface. This innocuous-sounding feature implicate a single planetwide catastrophe that reset the cratering clock by wiping out all evidence of previous impacts. A major erosive weather phenomenon such as a planet-wide flood could do it. But so could widespread geologic (Venusiologic?) activity, such as lava flows, turning Venus's entire surface into the American automotive dream—a totally paved planet. Whatever reset the clock, it must have ceased abruptly. But questions remain. If indeed there was a planet-wide flood on Venus, where is all the water now? Did it sink below the surface? Did it evaporate into the atmosphere? Or was the flood composed of a common substance other than water?
Our planetary fascination (and ignorance) is not limited to Venus. With meandering river beds, floodplains, river deltas, networks of tributaries, and river-eroded canyons, Mars was once a watering hole. The evidence is strong enough to declare that if anyplace in the solar system other than Earth ever boasted a flourishing water supply, it was Mars. For reasons unknown, Mars's surface is today bone dry. Whenever I look at both Venus and Mars, our sister and brother planets, I look at Earth anew and wonder how fragile our surface supply of liquid water just might be.
Imaginative observations of the planet by the noted American astronomer Percival Lowell led him to suppose that colonies of resourceful Martians had built an elaborate network of canals to redistribute water from Mars' polar ice caps to the more populated middle latitudes. To explain what he thought he saw, Lowell imagined a dying civilization that was somehow running out of water. In his thorough, yet curiously misguided treatise Mars as the Abode of Life, published in 1909, Lowell laments the imminent end of the Martian civilization he imagined he saw.
The drying up of the planet is certain to proceed until its surface can support no life at all. Slowly but surely time will snuff it out. When the last ember is thus extinguished, the planet will roll a dead world through space, its evolutionary career forever ended.
Lowell happened to get one thing right. If there were ever a civilization (or any kind of life at all) that required water on the Martian surface, then at some unknown time in Martian history, and for some unknown reason, all the surface water did dry up, leading to the exact fate for life that Lowell describes. Mars's missing water may be underground, trapped in the planet's permafrost. The evidence? Large craters on the Martian surface are more likely than small craters to exhibit dried mud-spills over their rims. Assuming the permafrost to be quite deep, reaching it would require a large collision. The deposit of energy from such an impact would melt this subsurface ice on contact, enabling it to splash upward. Craters with this signature are more common in the cold, polar latitudes- just where one might expect the permafrost layer to be closer to the Martian surface. By some estimates, if all the water suspected of hiding in the Martian permafrost and known to be locked in the polar ice caps were melted and spread evenly over its surface, Mars would don a planetwide ocean tens of meters deep. A thorough search for contemporary (or fossil) life on Mars must include a plan to look many places, especially below the Martian surface.
When thinking about where liquid water might be found (and by association, life), astronomers were originally inclined to consider planets that orbited the right distance from their host star to keep water in liquid form—not too close and not too far. This Goldilocks-inspired
habitable zone, as it came to be known, was a good start. But it neglected the possibility of life in places where other sources of energy may be responsible for keeping water as a liquid when it might have otherwise turned to ice. A mild greenhouse effect would do it. So would an internal source of energy such as leftover heat from the formation of the planet or the radioactive decay of unstable heavy elements, each of which contributes to Earth's residual heat and consequent geologic activity.
Another source of energy is planetary tides, which is a more general concept than simply the dance between a moon and a sloshing ocean. Jupiter's moon Io gets continually stressed by changing tides as it ambles slightly closer and then slightly farther from Jupiter during its near-circular orbit. At all times, the side of Io closest to Jupiter feels a stronger force of gravity than the side that is farthest. This difference serves to slightly elongate the solid moon in the direction of Jupiter. But as Io's distance to Jupiter changes during its orbit, Jupiter's tidal force across the moon also changes, thus pulsing Io's already oblong shape. And like a squash ball or racquet ball under high-use, if a system suffers structural stress then its temperature will rise. With a distance from the Sun that would otherwise guarantee a forever-frozen world, Io's stress level earns it the title of the most geologically active place in the entire solar system—complete with belching volcanoes, surface fissures, and plate tectonics. Some have analogized modern day Io to the early Earth, when our planet was still piping hot from its episode of formation.
An equally intriguing moon of Jupiter is Europa, which also happens to be tidally heated. As had been suspected for some time, Europa was recently confirmed (from images taken by the Galileo planetary probe) to be a world covered with thick, migrating ice sheets, afloat on a subsurface ocean of slush or liquid water. An ocean of water! Imagine going ice-fishing there. Indeed, engineers and scientists at the Jet Propulsion Laboratories are beginning to think about a mission where a space probe lands, finds (or cuts) a hole in the ice, and extends a submersible camera to have a peek. Since oceans were the likely place of origin for life on Earth, the existence of life in Europa's oceans becomes a plausible fantasy.
In my opinion, the most remarkable feature of water is not the well-earned badge of
universal solvent that we all learned in chemistry class; nor is it the unusually wide temperature range over which it remains liquid. Water's most remarkable feature is that, while most things—water included—shrink and become denser as they cool, when water cools below 4 degrees celsius it expands, becoming less and less dense. When water freezes at 0 degrees, it becomes even less dense than at any temperature when it was liquid, which is very good news to fish. In the winter, as the outside air drops below freezing, 4-degree water sinks to the bottom and stays there while a floating layer of ice builds extremely slowly on the surface, insulating the warmer water below.
Without this density inversion below 4 degrees, whenever the outside air temperature fell below freezing, the upper surface of a bed of water would cool and sink to the bottom as warmer water rose from below. This forced convection would rapidly drop the water's temperature to zero degrees as the surface begins to freeze. The denser, solid, ice would sink to the bottom and force the entire bed of water to freeze solid from the bottom up. In such a world, there would be no ice fishing because all the fish would be dead—fresh frozen. And ice anglers would find themselves sitting on a layer of ice that was either submerged below all remaining liquid water or was atop a completely frozen body of water. No longer would you need icebreakers to traverse the frozen Arctic—either the entire Arctic ocean would be frozen solid, or the frozen parts would all have sunk to the bottom and you could just sail your ship without incident. You could ice skate on lakes and ponds fearless of falling through. In this altered world, ice cubes and icebergs would sink, and in 1912, the Titanic would have steamed safely into its port of call in New York City.
The existence of water in the galaxy is not limited to planets and their moons. Water molecules, along with several other household chemicals such as ammonia and methane and ethyl alcohol, are found routinely in cool interstellar gas clouds. Under special conditions of low temperature and high density, an ensemble of water molecules can be induced to transform and funnel energy from a nearby star into an amplified, high-intensity beam of microwaves. The atomic physics of this phenomenon greatly resembles what goes on with visible light inside a laser. But in this case, the relevant acronym is M-A-S-E-R, for microwave amplification by the stimulated emission of radiation. Not only is water practically everywhere in the galaxy, it occasionally beams at you, too.
While we know water to be essential for life on Earth, we can only presume it to be a prerequisite for life elsewhere in the galaxy. Among the chemically illiterate, however, water is a deadly substance to be avoided. A now-famous science fair experiment that tested anti-technology sentiments and associated chemical-phobia was conducted in 1997 by Nathan Zohner, a 14-year-old student at Eagle Rock Junior High School in Idaho. He invited people to sign a petition that demanded either strict control of, or a total ban on, dihydrogen monoxide. He listed some of the odious properties of this colorless and odorless substance:
- It is a major component in acid rain
- It eventually dissolves almost anything it comes in contact with
- It can kill if accidentally inhaled
- It can cause severe burns in its gaseous state
- It has been found in tumors of terminal cancer patients
Forty-three out of fifty people approached by Zohner signed the petition, six were undecided, and one was a great supporter of dihydrogen monoxide and refused to sign. Yes, eighty-six percent of the passersby voted to ban water (H2O) from the environment.
Maybe that's what really happened to the water on Mars.
Neil deGrasse Tyson, an astrophysicist, is the Frederick P. Rose Director of New York City’s Hayden Planetarium and a visiting research scientist at Princeton University.
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