Nope, the Universe wasn’t born “ready for life”

Here on Earth, our planet practically overflows with life. After upwards of 4 billion years of unbroken biological activity on our world, life has spread to practically every niche of our planet’s surface, from the deepest depths of the ocean trenches to interiors of volcanic craters to nearly boiling, acidic geothermal springs to the highest snow-capped mountain peaks. Living organisms are literally everywhere, well-adapted to their ecological niches and capable of extracting energy and/or nutrients from their environments to survive, thrive, and reproduce.

Despite the tremendous differences between an anaerobic single-celled organism and a human being, their similarities are striking. All organisms rely on the same biochemical precursor molecules, which in turn are built out of the same atoms: primarily carbon, nitrogen, oxygen, hydrogen, and phosphorus, with a number of less-abundant elements also being essential to life processes. Given that everything in the Universe arose from the same cosmic beginning — the hot Big Bang — you might think that the building blocks necessary for life were present from the start.

But that couldn’t be further from the truth. The Big Bang, spectacular though it was, failed to put the proper ingredients in place for life to arise. Here’s how, for all its successes, the Big Bang failed to set the Universe up for the emergence of life.

There is a large suite of scientific evidence that supports the expanding Universe and the Big Bang. At every moment throughout our cosmic history for the first several billion years, the expansion rate and the total energy density balanced precisely, enabling our Universe to persist and form complex structures. Today, dark energy dominates the Universe, while early on, prior to the onset of the hot Big Bang, a phase of cosmological inflation occurred, preceding it and setting it up.

The biggest takeaway from the hot Big Bang is this: the Universe, as it exists today, is cold, expanding, sparse, and clumpy, having emerged from a hotter, more rapidly expanding, denser, and more uniform past. If this sounds like a wild idea to you, don’t be alarmed; in many ways, it is. The first hint we had that the Big Bang — or something very much like it — might describe our Universe didn’t come from any observable fact, but rather from a theoretical consideration.

If you begin with General Relativity, our best theory of gravity, and you consider a Universe that’s filled with roughly equal amounts of matter everywhere, you’ll discover something fascinating: this Universe is unstable. If you simply started with this matter at rest, the entire Universe would collapse until it created an event horizon and formed a black hole. At this point, the Universe as we know it would end in a singularity. As first realized by Alexander Friedmann way back in 1922, a Universe filled with equal amounts of “stuff” everywhere could not be both stable and static; it must either be expanding or contracting.

In a Universe that isn’t expanding, you can fill it with stationary matter in any configuration you like, but it will always collapse down to a black hole. Such a Universe is unstable in the context of Einstein’s gravity, and must be expanding to be stable, or we must accept its inevitable fate.

Observationally, the 1920s became a revolutionary decade for our understanding of the Universe. Newer, larger, more powerful telescopes enabled us to measure, for the first time, the properties of individual stars in galaxies other than the Milky Way, revealing their distances. Combined with the fact that the light we observed from them was not only systematically shifted toward longer, redder wavelengths, but that the farther a galaxy was from us, the greater the redshift was, this helped seal the deal: the Universe was expanding.

If the Universe is expanding today, and the light traveling through it is getting stretched to longer, redder wavelengths, then that teaches us that our Universe will continue to get:

• larger in volume,
• less dense in terms of the matter-and-energy per unit volume,
• clumpier as gravitation continues to draw nearby masses toward one another,
• and colder, as the light traveling through it becomes continuously lower in temperature.

If we know what the Universe is made out of, we can even figure out how that expansion rate will evolve into the far future.

Possible fates of the expanding Universe. Notice the differences between models in the past; only a Universe with dark energy matches our observations, and the dark energy-dominated solution came from de Sitter all the way back in 1917. By observing the expansion rate today and measuring the components present in the Universe, we can determine both its future and past histories.

But something remarkable comes along for the ride: if we can figure out what the Universe is made out of and how it’s expanding today, we can not only extrapolate the far future of the Universe, but also the distant past as well. The same equations — the Friedmann equations — that tell us how the Universe will evolve into the future also tell us what the Universe must have been like in the past; remember that in General Relativity, spacetime tells matter and energy how to move, while matter and energy tell spacetime how to curve and evolve.

If you know where all the matter and energy is and what it’s doing at any moment in time, you can determine how the Universe expanded and what its properties were at any point in either the past or the future. If we step backward in time, then, instead of forward, we’ll find that the young Universe should be:

• less clumpy and more uniform,
• smaller in volume and greater in matter-and-energy density,
• and hotter, as the radiation within it has had less time to be shifted to lower energies.

This last part extends not only to the light and radiation created by stars, but to any radiation that’s been present throughout all of our cosmic history, including even the very beginning.

How matter (top), radiation (middle), and dark energy (bottom) all evolve with time in an expanding Universe. As the Universe expands, the matter density dilutes, but the radiation also becomes cooler as its wavelengths get stretched to longer, less energetic states. Dark energy’s density, on the other hand, will truly remain constant if it behaves as is currently thought: as a form of energy intrinsic to space itself. These three components, together, dictate how the Universe expands at all times from the Big Bang until the present day and beyond.

If you imagine starting off the Universe in a very hot, dense, and uniform state, but one that’s expanding very rapidly, the laws of physics themselves will paint a remarkable picture of what’s to come.

• In the initial stages, every quantum of energy that exists will be so hot that it will be traveling at speeds indistinguishable from the speed of light, smashing into other quanta countless times per second due to the overwhelming densities.
• When a collision occurs, there’s a substantial chance that any particle-antiparticle pair that can get created — restricted only by the quantum mechanical conservation laws that govern the Universe and the amount of energy available for particle creation from Einstein’s famous E = mc² relation — will come into existence.
• Similarly, whenever a particle-antiparticle pair happens to collide, there’s a substantial chance that they’ll annihilate back into photons.

So long as you have an initially hot, dense, expanding Universe filled with interacting quanta of energy, those quanta will populate the Universe with all the various types of particles and antiparticles that are permitted to exist.

At the high temperatures achieved in the very young Universe, not only can particles and photons be spontaneously created, given enough energy, but also antiparticles and unstable particles as well, resulting in a primordial particle-and-antiparticle soup. Yet even with these conditions, only a few specific states, or particles, can emerge, and by the time a few seconds have passed, the Universe is much larger than it was in the earliest stages. As the Universe begins expanding, the density, temperature, and expansion rate of the Universe all rapidly drop as well.

But what happens next? As the Universe expands, everything cools: massive particles lose kinetic energy while massless particles get redshifted to longer wavelengths. Early on, at very high energies, everything was in equilibrium: particles and antiparticles got created at the same rate they got annihilated. But as the Universe cools, the “forward” reaction rates, where you create new particles-and-antiparticles based on collisions, begin to occur less rapidly than the “backward” reaction rates, where particles-and-antiparticles annihilate away back into massless particles, such as photons.

At very high energies, all of the known particles and antiparticles of the Standard Model are easy to create in large quantities. As the Universe cools, however, the more massive particles and antiparticles become more difficult to create, and they eventually annihilate away until there’s a negligible amount left. This winds up leading to a Universe filled with radiation, with just a tiny bit of leftover matter: protons, neutrons, and electrons, which somehow came to exist slightly more abundantly — about 1 extra matter particle per 1.4 billion photons — than antimatter. (How, exactly, that occurred is still an open area of research and is known as the baryogenesis problem.)

In the very early Universe, there were tremendous numbers of quarks, leptons, antiquarks, and antileptons of all species. After only a tiny fraction-of-a-second has elapsed since the hot Big Bang, most of these matter-antimatter pairs annihilate away, leaving a very tiny excess of matter over antimatter. How that excess came about is a puzzle known as baryogenesis, and it is one of the greatest unsolved problems in modern physics.

When the Universe becomes a few microseconds old, the excess of quarks (over antiquarks) combines with gluons to form hadrons: the first stable protons and neutrons. As it ages, it continues to expand and cool. Then, about 1 second later, while the Universe is still very hot and has a little bit of antimatter left (positrons, the antimatter counterpart of electrons, and antineutrinos, the antimatter counterpart of neutrinos), the remaining protons and neutrons attempt to fuse together under the hot, dense conditions of this early Universe. With temperatures about ~1000 times hotter than the ones we find at the center of the Sun, conditions seem right for nuclear fusion, where elements can build their way up the periodic table in rapid succession.

If the Universe could do precisely this, then as soon as the Universe becomes cool enough to form neutral atoms and enough time passes so that the gravitational imperfections can attract enough matter to form stars and star systems, we’d have chances for life. The atoms necessary for life — the raw ingredients — can bind together into all sorts of molecular configurations all on their own, through natural, abiotic processes, just like we find today all throughout interstellar space.

If we could begin building elements in these early stages of the hot Big Bang, the high temperatures and densities could permit not just fusion of hydrogen into helium, but helium into carbon, and so on into nitrogen, oxygen, and many of the heavier elements found all throughout the modern cosmos.

But that’s a big “if,” and one that doesn’t turn out to be true.

In a Universe loaded with neutrons and protons, it seems like building elements would be a cinch. All you have to do is start off with that first step: building deuterium, and the rest will follow from there. But while making deuterium is easy, not destroying it is particularly hard. During the first 3-4 minutes after the Big Bang, the Universe experiences a “deuterium bottleneck,” where no further nuclear reactions can proceed until deuterium is stably formed. So long as there are enough photons of sufficient energy to spontaneously blast a deuterium nucleus apart, no heavy elements can form.

This is the problem: deuterium. The Universe is full of protons and neutrons, and it’s hot and dense. Whenever a proton and neutron find one another, they’ll fuse into a deuteron, which is a heavy isotope of hydrogen, and is also more stable than a free proton and neutron separately; each time you form a deuteron from a proton and neutron, you liberate 2.2 million electron-volts of energy. (You can also form deuterium from nuclear reactions involving two protons, but the reaction rate is much lower than from a proton and a neutron.)

So why, then, can’t you add protons or neutrons to each deuteron, building your way up to heavier isotopes and elements?

The same hot, dense conditions lead to a “backward” reaction that swamps the “forward” creation of deuterium by fusing protons with neutrons: the fact that enough photons, which outnumber protons and neutrons by more than a billion-to-one, have more than 2.2 million electron-volts of energy themselves. When they collide with a deuteron, which occurs far more frequently than a deuteron colliding with anything else made out of protons-and-neutrons, they immediately blast it apart.

The inability of the cosmos to maintain deuterium in the early Universe for long enough periods to build up to heavier elements is the primary reason that the Big Bang can’t create the ingredients for life on its own.

From beginning with just protons and neutrons, the Universe builds up helium-4 rapidly, with small but calculable amounts of deuterium, helium-3, and lithium-7 left over as well. Until the latest results from the LUNA collaboration, step 2a, where deuterium and a proton fuse into helium-3, had the largest uncertainty. That uncertainty has now dropped to just 1.6%, allowing for incredibly strong conclusions.

So, what can the Universe do? It’s compelled to wait until it’s expanded and cooled enough so that deuterium isn’t immediately blasted apart. But in the meanwhile, a whole slew of other things happen while we wait for the Universe to cool sufficiently. They include:

• neutrinos and antineutrinos stop efficiently participating in interactions with other particles, also known as the freeze-out of the weak interactions,
• electrons and positrons, like other species of matter and antimatter, annihilate away, leaving only the excess electrons,
• and the free neutrons, being unable to bind themselves up in heavier nuclei, begin to decay away into protons, electrons, and anti-electron neutrinos.

Finally, after a little more than about ~200 seconds, we can finally form deuterium without immediately blasting it apart. But at this point, it’s too late. The Universe has cooled but become much less dense: only about one-billionth the density found in the central core of our Sun. The deuterons can fuse with other protons, neutrons, and deuterons to build up copious amounts of helium, but that’s where the chain reaction ends.

With less energy per particle, with strong repulsive forces between the helium nuclei, and with every combination of:

• helium-4 and a proton,
• helium-4 and a neutron,
• and helium-4 and helium-4,

being unstable, that’s pretty much the end of the line. The Universe, in the immediate aftermath of the Big Bang, is made of 99.99999%+ hydrogen and helium, exclusively.

The most current, up-to-date image showing the primary origin of each of the elements that occur naturally in the periodic table. Neutron star mergers, white dwarf collisions, and core-collapse supernovae may allow us to climb even higher than this table shows. The Big Bang gives us almost all of the hydrogen and helium in the Universe, and almost none of everything else combined. Most elements, in some form or another, are forged in stars.

Even though we’re talking about cosmic scales, it’s actually the laws that govern subatomic particles — nuclear and particle physics — that prevent the Universe from forming the heavy elements required for life in the early stages of the Big Bang. If the rules were a little bit different, like deuterium was more stable, there were much greater numbers of protons and neutrons, or there were fewer photons at high energies, nuclear fusion could have built up large quantities of heavy elements in the first few seconds of the Universe.

But the easily-destroyed nature of deuterium, combined with the enormous numbers of photons present in the early Universe, kills our dreams of having the necessary raw ingredients right at the beginning.

Instead, it only produces hydrogen and helium nuclei, which will form neutral atoms a few hundred thousand years later, and which will become the raw ingredients for the first star after tens to hundreds of millions of years. That’s the key step: we need to wait for stars to form before we build up any substantial quantities of any heavier elements, such as carbon, oxygen, and the other elements essential for life. The Big Bang was a great start to our Universe, but it couldn’t set us up for life all on its own. For that, we needed generations of stars to live, die, and enrich the interstellar medium with the heavier elements that all biochemical processes require. When it comes to your existence, the Big Bang absolutely isn’t enough to give rise to you. For that to occur, you can literally thank your lucky stars: the ones that lived, died, and created the essential elements still inside of you today.