The Amazing Space Odyssey of a Hydrogen Atom

Author: Ryan Farber

Editors: Alex Taylor, Jessica Cote, and Sarah Kearns

Where do you come from? Somewhere on Earth, you say. But how did life begin? How did the Earth begin? How did the Sun begin? … How did the universe begin? These questions of origins have fascinated humanity for millennia. And though we can answer neither the first question nor the last, nor many in between, modern astronomical theory places a handle on the origins of one structure of particular importance for our existence: the Sun.

In this origin story, we will begin in the dark, sparse, altogether quite inhospitable, domain of interstellar space. In fact, if we consider a cubic centimeter of space, we would find only one lonely hydrogen atom, the hero of our story.

Our hero is not a hydrogen atom by lucky chance either. About 92% of all the matter in the universe is hydrogen1. Another 7% of the universe is made up of helium, leaving less than 1% for all the heavier elements. These heavier elements are generated in stars, bestowing upon them the lovely name of stardust. Life on Earth relies on them: from the oxygen atmosphere we breathe, to the silicon-based computers we use to read this delightful article, our daily lives depend on a teeny-tiny fraction of the stuff comprising the universe. Moreover, stardust will play a profound role in the origin story we are unraveling.

But for now, let us recall our lonely hydrogen atom, sitting in its spacious cubic centimeter of space. Now, one may be thinking, “Big deal! A cubic centimeter is tiny so of course there’s only one atom there. It’s about the same size as a sugar cube-” Exactly! A sugar cube of one cubic centimeter contains a whopping 1021 molecules. That’s a billion trillion molecules. There are only a thousand times more stars in the universe than molecules of sugar in that one cubic centimeter which is home to only one hydrogen atom. That’s just how sparse space is.

On the other hand, space is vast. Consider a cubical region of interstellar space, with each side spanning 300 light-years2. With one hydrogen atom per cubic centimeter, we expect there to be a mind-boggling 1061 hydrogen atoms in our imaginary cube of space (see Figure 1). That’s about as many atoms of sand as there would be in the entire universe if every star in the universe hosted an Earth-like planet (…and we’re still searching for the second Earth-like planet in the universe).

Farber-Hydrogen-Fig1.png
Figure 1. One is the loneliest number that you’ll ever do… We have herein anthropomorphized our lonely hydrogen atom to consist of a frowning (lonely) proton and an electron. Why is the proton yellow? Because protons are a-maize-ing!

As our lonely hydrogen atom whizzes about space amongst its 10 trillion trillion trillion trillion trillion neighbors, each with its own random trajectory, it is perhaps unsurprising that our hero will occasionally encounter another hydrogen atom. If they happen to approach close enough, their constituent protons will repulse one another, and the two atoms will whizz back apart. No harm, no foul? Not quite. Similar to how billiard balls lose energy during a collision (as evidenced by the sound of the collision), the two hydrogen atoms lose energy during the encounter (emitting light rather than sound; see Figure 2). In typical interstellar space conditions, such a process of encounter and loss of energy proceeds for about 200,000 years, an astrophysical blink of the eye.

Farber-Hydrogen-Fig2.png
Figure 2.  Two can be as bad as one… Left: Another hydrogen atom approaches our hero close enough that the protons repulse them apart from their collision course. Right: The two hydrogen atoms are about to whizz away from each other but as a result of the interaction, their electrons are collisionally excited and take some of the energy from the interaction to enter an excited state. A fraction of a second later, the electrons spontaneously emit photons to return to their ground states.

As the hydrogen atoms lose energy, the gas they comprise also drops in temperature. The cooling gas contracts, increasing its density. In a higher density environment, it is more likely that atoms will collide, accelerating the cooling process. When the density has increased about one thousand times and the temperature has simultaneously reached a frigid 5 K (-450 °F; for comparison, the coldest Antarctica has ever been was a balmy -128 °F), the stardust enters the picture.

Molecular hydrogen (H2) cannot form simply by sticking two hydrogen atoms together in free space like Velcro and hoping that they stay joined together. As mentioned previously, the protons will repulse one another. Instead, the hydrogen atoms first bind to particles of stardust. The close quarters enforced by the dust enables the hydrogen atoms to overcome their mutual repulsion and enter a bound state. The formation of molecular hydrogen releases some energy, unbinding the molecular hydrogen from the dust (see Figure 3). When the majority of our 1061 hydrogen atoms have formed molecular hydrogen, they form a new structure called a giant molecular cloud (see Figure 4).

Farber-Hydrogen-Fig3
Figure 3. Brrrr, 5K! Better huddle for warmth.
Farber-Hydrogen-Fig4.jpg
Figure 4. Taurus molecular cloud. In this image, dark red clouds can be seen thanks to their obscuration of background stars. The predominance of hydrogen in these clouds is what causes them to glow red, much like the effect in neon signs. These space clouds, reminiscent in shape to cirrus clouds in the Earth’s atmosphere, are actually several hundred light-years long. They are nothing like the perfect cube described in the article, but alas we astrophysicists adore our spherical cows. Mooooo!  Credit: NASA. 

At such a low temperature, there is essentially no pressure to halt the gravitational collapse. Piece by piece, the giant molecular cloud fragments into separately collapsing cloudlets, each attaining yet higher densities. Hurtling faster than a rocker re-entering the Earth’s atmosphere, millions upon millions of molecules of hydrogen are all squished into the once cozy cubic centimeter of space. When collisions occur at such breakneck speeds, the interaction is nothing like the tranquil cooling process of Figure 2. Instead, the temperature furiously increases, disintegrating the molecular hydrogen back into atoms. The hydrogen atoms are rapidly ionized (stripped of their electrons). The free-floating electrons speed through the cloud, disintegrating more molecular hydrogen back into atomic form. The cloudlet’s collapse is halted when the temperature has increased sufficiently that the resulting pressure counteracts the inexorable force of gravity. The temperature now vastly exceeds the typical interstellar value. As the very core of the cloud is crushed by the billion trillion trillions of hydrogen nuclei above, the temperature attains a scorching ten million Kelvin. The hydrogen nuclei are packed so densely and are racing so quickly that a fortunate pair collide and fuse, transforming a hydrogen nucleus into a helium nucleus (see Figure 5). Fusion releases a prodigious amount of energy, marking the birth of a new star.

Farber-Hydrogen-Fig5.png
Figure 5. Fusion of two hydrogen nuclei to form a helium nucleus. In particular, we show the fusion of protium (hydrogen nucleus composed of one proton and zero neutrons) and deuterium (hydrogen nucleus composed of one proton and one neutron) to form He-3 (helium nucleus with only one neutron; garden variety helium is He-4).

The stellar nursery of a giant molecular cloud host hundreds of newly formed stars. And once upon a time, from its own stellar nursery, a dull yellow star began fusing hydrogen. 93 million miles from the star, a coalescence of astronomically minuscule traces of stardust, all but forgotten by the universe, gave birth to our Earth (see Figure 6). So weigh heavy in your hearts that space is not empty, for without the scores of light-years of lonely hydrogen atoms, dragging with them strands of stardust, we would not be here to ponder the magnificence of space.

NASA-earth
Figure 6. The Earth. Photo credit: NASA.

1 Note that I am citing the number abundances of the elements, whereas the oft-quoted ~¾ hydrogen, ¼ helium, and 2% heavier elements utilize the mass abundances.

2 A light-year is the distance light travels in one year. Light travels at blazingly fast speeds that put Comcast to shame; for example, light takes only 8 minutes to travel the 93 million miles from the Sun to the Earth. 300 light-years is the size of a giant molecular cloud, which will be described subsequently.

ryan-headshotRyan Farber is a third-year PhD student at the University of Michigan, studying Astronomy & Astrophysics. Ryan researches the efficiency with which high energy charged particles (unfortunately named cosmic “rays”) can accelerate galactic outflows. Beyond research, Ryan enjoys cheering on his home and local sports teams, weightlifting, running, and learning languages.

Read all posts by Ryan here.

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