Water in space – a 'Goldilocks' star reveals previously hidden step in how water gets to planets like Earth
- Written by John Tobin, Scientist, National Radio Astronomy Observatory
Without water, life on Earth could not exist as it does today. Understanding the history of water in the universe is critical to understanding how planets like Earth come to be.
Astronomers typically refer to the journey water takes from its formation as individual molecules in space to its resting place on the surfaces of planets as “the water trail.” The trail starts in the interstellar medium with hydrogen and oxygen gas and ends with oceans and ice caps on planets, with icy moons orbiting gas giants and icy comets and asteroids that orbit stars. The beginnings and ends of this trail are easy to see, but the middle has remained a mystery.
I am an astronomer[1] who studies the formation of stars and planets using observations from radio and infrared telescopes. In a new paper, my colleagues and I describe the first measurements ever made[2] of this previously hidden middle part of the water trail and what these findings mean for the water found on planets like Earth.
How planets are formed
The formation of stars and planets is intertwined. The so-called “emptiness of space” – or the interstellar medium – in fact contains large amounts of gaseous hydrogen[5], smaller amounts of other gasses and grains of dust[6]. Due to gravity, some pockets of the interstellar medium will become more dense as particles attract each other[7] and form clouds. As the density of these clouds increases, atoms begin to collide more frequently and form larger molecules[8], including water that forms on dust grains and coats the dust in ice[9].
Stars begin to form when parts of the collapsing cloud reach a certain density and heat up enough to start fusing hydrogen atoms together. Since only a small fraction of the gas initially collapses into the newborn protostar, the rest of the gas and dust forms a flattened disk of material[10] circling around the spinning, newborn star. Astronomers call this a proto-planetary disk.
As icy dust particles collide with each other inside a proto-planetary disk, they begin to clump together[11]. The process continues and eventually forms the familiar objects of space like asteroids, comets, rocky planets like Earth and gas giants like Jupiter or Saturn.
Gas and dust can condense into clouds, like the Taurus Molecular Cloud, where collisions between hydrogen and oxygen can form water.
ESO/APEX (MPIfR/ESO/OSO)/A. Hacar et al./Digitized Sky Survey 2, CC BY[12][13]
Two theories for the source of water
There are two potential pathways that water in our solar system could have taken. The first, called chemical inheritance[14], is when the water molecules originally formed in the interstellar medium are delivered to proto-planetary disks and all the bodies they create without going through any changes.
The second theory is called chemical reset[15]. In this process, the heat from the formation of the proto-planetary disk and newborn star breaks apart water molecules, which then reform once the proto-planetary disk cools.
Normal hydrogen, or protium, does not contain a neutron in its nucleus, while deuterium contains one neutron, making it heavier.
Dirk Hünniger/Wikimedia Commons, CC BY-SA[16][17]
To test these theories, astronomers like me look at the ratio between normal water and a special kind of water called semi-heavy water. Water is normally made of two hydrogen atoms and one oxygen atom. Semi-heavy water is made of one oxygen atom, one hydrogen atom and one atom of deuterium – a heavier isotope of hydrogen with an extra neutron in its nucleus.
The ratio of semi-heavy to normal water is a guiding light on the water trail – measuring the ratio can tell astronomers a lot about the source of water. Chemical models[18] and experiments[19] have shown that about 1,000 times more semi-heavy water will be produced in the cold interstellar medium than in the conditions of a protoplanetary disk[20].
This difference means that by measuring the ratio of semi-heavy to normal water in a place, astronomers can tell whether that water went through the chemical inheritance or chemical reset pathway.
V883 Orionis is a young star system with a rare star at its center that makes measuring water in the proto-planetary cloud, shown in the cutaway, possible.
ALMA (ESO/NAOJ/NRAO), B. Saxton (NRAO/AUI/NSF), CC BY[21][22]
Measuring water during the formation of a planet
Comets have a ratio of semi-heavy to normal water almost perfectly in line with chemical inheritance[23], meaning the water hasn’t undergone a major chemical change since it was first created in space. Earth’s ratio sits somewhere in between the inheritance and reset ratio, making it unclear where the water came from.
To truly determine where the water on planets comes from, astronomers needed to find a goldilocks proto-planetary disk – one that is just the right temperature and size to allow observations of water. Doing so has proved to be incredibly difficult[24]. It is possible to detect semi-heavy and normal water when water is a gas; unfortunately for astronomers, the vast majority of proto-plantary disks are very cold and contain mostly ice[25], and it is nearly impossible to measure water ratios[26] from ice at interstellar distances.
A breakthrough came in 2016, when my colleagues and I were studying proto-planetary disks around a rare type of young star called FU Orionis stars. Most young stars consume matter from the proto-planetary disks around them. FU Orionis stars are unique because they consume matter about 100 times faster than typical young stars and, as a result, emit hundreds of times more energy[27]. Due to this higher energy output, the proto-planetary disks around FU Orionis stars are heated to much higher temperatures, turning ice into water vapor out to large distances from the star.
Using the Atacama Large Millimeter/submillimeter Array[28], a powerful radio telescope in northern Chile, we discovered[29] a large, warm proto-planetary disk around the Sunlike young star V883 Ori, about 1,300 light years from Earth in the constellation Orion.
V883 Ori emits 200 times more energy than the Sun, and my colleagues and I recognized that it was an ideal candidate to observe the semi-heavy to normal water ratio.
The proto-planetary disk around V883 Ori contains gaseous water, shown in the orange layer, allowing astronomers to measure the ratio of semi-heavy to normal water.
ALMA (ESO/NAOJ/NRAO), J. Tobin, B. Saxton (NRAO/AUI/NSF), CC BY[30][31]
Completing the water trail
In 2021, the Atacama Large Millimeter/submillimeter Array took measurements of V883 Ori for six hours. The data revealed a strong signature of semi-heavy and normal water[32] coming from V883 Ori’s proto-planetary disk. We measured the ratio of semi-heavy to normal water and found that the ratio was very similar to ratios found in comets[33] as well as the ratios found in younger protostar systems[34].
These results fill in the gap of the water trail forging a direct link between water in the interstellar medium, protostars, proto-planetary disks and planets like Earth through the process of inheritance, not chemical reset.
The new results show definitively that a substantial portion of the water on Earth most likely formed billions of years ago, before the Sun had even ignited. Confirming this missing piece of water’s path through the universe offers clues to origins of water on Earth. Scientists have previously suggested that most water on Earth came from comets impacting the planet[35]. The fact that Earth has less semi-heavy water than comets and V883 Ori, but more than chemical reset theory would produce, means that water on Earth likely came from more than one source.
References
- ^ I am an astronomer (www.cv.nrao.edu)
- ^ first measurements ever made (www.nature.com)
- ^ Bill Saxton, NRAO/AUI/NSF (www.nrao.edu)
- ^ CC BY (creativecommons.org)
- ^ large amounts of gaseous hydrogen (doi.org)
- ^ grains of dust (doi.org)
- ^ more dense as particles attract each other (doi.org)
- ^ form larger molecules (doi.org)
- ^ on dust grains and coats the dust in ice (doi.org)
- ^ forms a flattened disk of material (doi.org)
- ^ they begin to clump together (doi.org)
- ^ ESO/APEX (MPIfR/ESO/OSO)/A. Hacar et al./Digitized Sky Survey 2 (www.eso.org)
- ^ CC BY (creativecommons.org)
- ^ chemical inheritance (doi.org)
- ^ chemical reset (doi.org)
- ^ Dirk Hünniger/Wikimedia Commons (commons.wikimedia.org)
- ^ CC BY-SA (creativecommons.org)
- ^ Chemical models (doi.org)
- ^ experiments (doi.org)
- ^ than in the conditions of a protoplanetary disk (doi.org)
- ^ ALMA (ESO/NAOJ/NRAO), B. Saxton (NRAO/AUI/NSF) (public.nrao.edu)
- ^ CC BY (creativecommons.org)
- ^ chemical inheritance (doi.org)
- ^ proved to be incredibly difficult (doi.org)
- ^ contain mostly ice (doi.org)
- ^ impossible to measure water ratios (doi.org)
- ^ emit hundreds of times more energy (doi.org)
- ^ Atacama Large Millimeter/submillimeter Array (public.nrao.edu)
- ^ we discovered (ui.adsabs.harvard.edu)
- ^ ALMA (ESO/NAOJ/NRAO), J. Tobin, B. Saxton (NRAO/AUI/NSF) (public.nrao.edu)
- ^ CC BY (creativecommons.org)
- ^ strong signature of semi-heavy and normal water (doi.org)
- ^ similar to ratios found in comets (doi.org)
- ^ in younger protostar systems (doi.org)
- ^ came from comets impacting the planet (doi.org)
Authors: John Tobin, Scientist, National Radio Astronomy Observatory
