Where did Earth’s water come from? A team of Arizona State University geoscientists led by Peter Buseck, Regents’ Professor in ASU’s School of Earth and Space Exploration (SESE) and School of Molecular Sciences, has found an answer in a previously neglected source.
The team has also discovered that our planet contains considerably more hydrogen, a proxy for water, than scientists previously thought. So where is it? Mostly down in our planet’s core, but more about that in a minute. The bigger question is where did all this come from in the first place? Steven Desch, professor of astrophysics in SESE and one of the team scientists said in a statement:
“Comets contain a lot of ices, and in theory could have supplied some water. Asteroids are a source as well, not as water-rich, yet still plentiful.
“But there’s another way to think about sources of water in the solar system’s formative days. Because water is hydrogen plus oxygen, and oxygen is abundant, any source of hydrogen could have served as the origin of Earth’s water.”
In the beginning, what served as the source of Earth’s water?
Hydrogen gas was the major ingredient in the solar nebula — the gases and dust out of which the Sun and planets formed. If the abundant hydrogen in the nebula could combine with Earth’s rocky material as it formed, that could be the ultimate origin of Earth’s global ocean.
How Earth accumulated water, Step 1: Dust and gas collect into embryo bodies with a water content similar to asteroids today. (Image: J. Wu, S Desch via ASU)
Jun Wu, lead author of the paper that was published in the Journal of Geophysical Research, and is an assistant research professor in both SESE and the School of Molecular Sciences, said:
“The solar nebula has been given the least attention among existing theories, although it was the predominant reservoir of hydrogen in our early solar system.”
But first, some geochemical detective work. To distinguish between sources of water, scientists turn to isotope chemistry, measuring the ratio between two kinds of hydrogen. Nearly all hydrogen atoms have a nucleus that’s a single proton. But in about 1 in 7,000 hydrogen atoms, the nucleus has a neutron in addition to the proton. This isotope is called “heavy hydrogen,” or deuterium, symbolized as D.
Step 2: Embryos heat up, develop cores and mantles; most of the hydrogen lies in the cores, with the mantles being richer in deuterium (D). (Image: J. Wu, S Desch via ASU)
The ratio of the number of D atoms to ordinary H atoms is called the D/H ratio, and it serves as a fingerprint for where that hydrogen came from. For example, asteroidal water has a D/H of about 140 parts per million (ppm), while cometary water runs higher, ranging from 150 ppm to as much as 300 ppm.
Scientists know that Earth has one global ocean of water on its surface and about two more oceans of water dissolved in its mantle rocks. That water has a D/H ratio of about 150 ppm, making an asteroidal source a good match. Comets? With their higher D/H ratios, comets are mostly not good sources.
Step 3: The largest embryo develops a molten magma ocean on its surface from impacts and radioactive decay; iron in the molten layer grabs some hydrogen from the embryo’s primitive hydrogen-rich atmosphere. (Image: J. Wu, S Desch via ASU)
And what’s worse, the D/H of hydrogen gas in the solar nebula was only 21 ppm, far too low to supply large quantities of Earth’s water. In fact, asteroidal material is such a good match that previous researchers have discounted the other sources. But, said Wu and co-workers, other factors and processes have changed the D/H of Earth’s hydrogen, starting back when the planet was first beginning to form. Wu said:
“This means we shouldn’t ignore the dissolved solar nebula gas.”
Concentrating hydrogen
The key lies in a process combining physics and geochemistry, which the team found acted to concentrate hydrogen in the core while raising the relative amount of deuterium in Earth’s mantle. The process began quite early as the Sun’s planets were starting to form and grow through the merger of primitive building blocks called planetary embryos.
These moon-to-Mars-size objects grew very quickly in the early solar system, colliding and accreting material from the solar nebula. Within the embryos, decaying radioactive elements melted iron, which grabbed asteroidal hydrogen and sank to form a core. The largest embryo experienced collisional energy that melted its entire surface, making what scientists call a magma ocean.
Step 4: The magma ocean sinks to just above the embryo’s core, carrying its low D/H material down, where it gradually mixes into the mantle. (Image: J. Wu, S Desch via ASU)
Molten iron in the magma snatched hydrogen out of the developing primitive atmosphere, which derived from the solar nebula. The iron carried this hydrogen, along with hydrogen from other sources, down into the embryo’s mantle. Eventually, the hydrogen became concentrated in the embryo’s core.
Meanwhile, another important process was going on between molten iron and hydrogen. Deuterium atoms do not like iron as much as their H counterparts, thus causing a slight enrichment of H in the molten iron and leaving relatively more D behind in the magma. In this way, the core gradually developed a lower D/H ratio than the silicate mantle, which formed after the magma ocean cooled.
All this was stage one.
Step 5: Embryos of varying sizes and D/H ratios collide, merge, and mix, producing an Earth with a mantle rich in hydrogen as a proxy for water. (Image: J. Wu, S Desch via ASU)
Stage two followed as embryos collided and merged to become the proto-Earth. Once again a magma ocean developed on the surface, and once more, leftover iron and hydrogen may have undergone similar processes as in stage one, thus completing the delivery of the two elements to the core of the proto-Earth. Wu added:
“Besides the hydrogen that the embryos captured, we expect they also caught some carbon, nitrogen, and noble gases from the early solar nebula. These should have left some isotope traces in the chemistry of the deepest rocks, which we can look for.”
The team modeled the process and checked its predictions against samples of mantle rocks, which are rare today at Earth’s surface. Desch said:
“We calculated how much hydrogen dissolved in these bodies’ mantles could have ended up in their cores.
“Then we compared this to recent measurements of the D/H ratio in samples from Earth’s deep mantle.” This let the team set limits on how much hydrogen is in Earth’s core and mantle.
“The end result is that Earth likely formed with seven or eight global oceans’ worth of hydrogen. The majority of this indeed came from asteroidal sources. But a few tenths of an ocean’s worth of hydrogen came from the solar nebula gas.”
Adding up the quantities cached in several places, Wu said:
“Our planet hides the majority of its hydrogen inside, with roughly two global oceans’ worth in the mantle, four to five in the core, and of course, one global ocean at the surface.”
Step 6: As Earth continues to evolve, plumes of molten rock rise from the mantle, triggering volcanic activity at the surface — and bringing up rock with a lower D/H ratio than surface rocks have. The result is an Earth with multiple oceans’ worth of hydrogen stored at different depths. (Image: J. Wu, S Desch via ASU)
Not just for our solar system
The new finding, the team said, fits neatly into current theories for how the Sun and planets formed. It also has implications for habitable planets beyond the solar system. Astronomers have discovered more than 3,800 planets orbiting other stars, and many appear to be rocky bodies not greatly different from our own.
Many of these exoplanets might have formed far from the zones where water-rich asteroids and other building blocks might have arisen. Yet, they still could have collected hydrogen gas from their own stars’ solar nebulas in the way that Earth did. The team concluded:
“Our results suggest that forming water is likely inevitable on sufficiently large rocky planets in extrasolar systems.”
The authors of the paper are Jun Wu, Steven Desch, Laura Schaefer, Linda Elkins-Tanton, Kaveh Pahlevan, and Peter Buseck, all affiliated with SESE; Wu and Buseck are also affiliated with ASU’s School of Molecular Sciences. The research was funded by the Keck Foundation.
Provided by: Arizona State University [Note: Materials may be edited for content and length.]
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