Inflation set up the hot Big Bang and gave rise to the observable Universe we have access to, but we can only measure the last tiny fraction of a second of inflation’s impact on our Universe. This is enough, however, to give us a large slew of predictions to go out an look for, many of which have already been observationally confirmed.(E. Siegel, with images derived from ESA/Planck and the DoE/NASA/ NSF interagency task force on CMB research)

What Was It Like When The Universe Was Inflating?

Cosmic inflation is what happened before, and set up, the Big Bang. Here’s what it’s like to live in an inflating Universe.


Our Universe today is full of matter and radiation, and can be observed by us through a variety of means. Atoms have clumped and clustered together due to billions of years of gravitation. This has formed a great cosmic web on the largest scales, with clusters of galaxies, individual galaxies, clouds of gas, stars, planets, and more on smaller scales. Through it all, the Universe has been expanding and cooling, something it’s been doing since the earliest moments of the hot Big Bang.

But the Big Bang wasn’t the very beginning of the Universe. Before that, there was a period known as cosmic inflation, which came earlier and set up the hot Big Bang. While living in an expanding, cooling Universe is difficult to intuit, inflation paints an entirely different picture. Here’s what it would be like to live in an inflating Universe.

We often visualize space as a 3D grid, even though this is a frame-dependent oversimplification when we consider the concept of spacetime. If you place a particle on this grid and allow the Universe to expand, the particle will appear to recede from you. (ReunMedia / Storyblocks)

Imagine that you were a particle, located somewhere in the fabric of spacetime. A short distance away, another particle also exists. Imagine that the only thing that impacts them is the expansion of the Universe. How, then, will this particle move relative to you?

If your Universe were filled with radiation, it would expand like the square root of time: the distance between you and this particle scales as ~t^(1/2).

If your Universe were filled with matter, it would expand like time to the two-thirds power: the distance between you and this particle scales as ~t^(2/3).

But when your Universe inflates, space expands exponentially: like ~e^(Ht), where H is the expansion rate of the Universe.

This diagram shows, to scale, how spacetime evolves/expands in equal time increments if your Universe is dominated by matter, radiation, or the energy inherent to space itself, with the latter corresponding to an inflating, energy-inherent-to-space-dominated Universe. (E. Siegel)

This means that after a certain amount of time, this particle would double its distance from you. Because inflation is not only exponential but also rapid — the expansion rate is very large during inflation — that doubling only requires somewhere in the neighborhood of 10^-35 seconds. But the defining trait of inflation isn’t its rapidity, since, after all, the early stages of the hot Big Bang may be just as rapid. Instead, the defining trait of inflation is its relentlessness.

  • After 10^-35 seconds, this nearby particle would be twice as far away as it initially was.
  • After 2 × 10^-35 seconds, it would be 4 times its initial distance.
  • After 3 × 10^-35 seconds, it would be 8 times its initial distance.
  • After 4 × 10^-35 seconds, it would be 16 times its initial distance.

And we can continue this as long as we want. After 10^-34 seconds of inflation, the nearby particle would be 10²⁴ times as far away as it was initially. After 10^-33 seconds, it would be 10³⁰ times as far as its initial distance. And after 10^-30 seconds of inflation, this particle would be about 10³⁰⁰⁰⁰ times as distant as it was initially. If your Universe began full of particles of any type, they would in extraordinarily short order be driven away from one another so that no two ever saw each other again.

Particles that are extremely close together in a pre-inflationary Universe will be driven apart at an exponential rate in an expanding spacetime. By time around 10^-32 seconds have passed in an inflating Universe, there is no way to have two particles in the same volume of space that correspond to our entire visible Universe today. (E. Siegel / Beyond The Galaxy)

Space itself may have begun with an interesting intrinsic curvature to it. It could have been balled-up, knotted, twisted-and-turned, or even spherical. It could have been full of topological defects, with holes throughout it. It could have been connected in multiple places in bizarre ways. It could have even contained the entirety of space within a volume as minuscule as a subatomic particle.

But during inflation, this rapid-and-relentless expansion will increase the size of the Universe many, many times over: by the same amount that it would push any other particle away. It will take any initial geometry and stretch it to such a large scale that any region you look at — even something as large as our entire observable Universe today — would be indistinguishable from spatially flat.

Inflation causes space to expand exponentially, which can very quickly result in any pre-existing curved or non-smooth space appearing flat. If the Universe is curved, it has a radius of curvature that is at minimum hundreds of times larger than what we can observe. (E. Siegel (L); Ned Wright’s cosmology tutorial (R))

The reason inflation works this way is because there’s a large amount of energy that’s intrinsic to space itself. As the fabric of the Universe expands, new space gets created, also with that same amount of energy inherent to it. This is why the expansion is relentless. If you look at an inflating Universe, it continues to inflate in an ongoing fashion, never decreasing in its rapidity.

But on the very smallest scales, under these conditions, there are also quantum fluctuations occurring.

Visualization of a quantum field theory calculation showing virtual particles in the quantum vacuum. Even in empty space, this vacuum energy is non-zero. (Derek Leinweber)

These fluctuations happen in our Universe today, only they occur both on very low energy scales and on timescales that are extremely short compared to anything we observe. If you visualize these fluctuations as virtual particle-antiparticle pairs popping in-and-out of existence, they do so on timescales that are far too short to result in anything interesting happening; they simply add a small amount of extra energy to the fabric of space itself.

An illustration of the early Universe as consisting of quantum foam, where quantum fluctuations are large, varied, and important on the smallest of scales. (NASA/CXC/M.Weiss)

But during inflation, these fluctuations are much, much larger in energy: about 100 orders of magnitude larger than they are today. On average, the value of the energy inherent to space jumps up-and-down by about 0.003% randomly, due to these quantum fluctuations.

Unlike today, though, when the Universe is inflating, these fluctuations get stretched across the Universe. As a result, the value of the energy inherent to space varies, with the older, more-stretched fluctuations showing up on larger scales, and the younger, less-stretched ones appearing on smaller scales.

The quantum fluctuations that occur during inflation do indeed get stretched across the Universe, but they also cause fluctuations in the total energy density, leaving us with some non-zero amount of spatial curvature left over in the Universe today. These field fluctuations cause density imperfections in the early Universe, which then lead to the temperature fluctuations we experience in the cosmic microwave background. (E. Siegel / Beyond the Galaxy)

Every 10^-33 to 10^-32 seconds, the smallest subatomic scale we can describe with our physical laws known today — the Planck scale — gets stretched to the size of our presently observable Universe. On longer timescales than that, what was previously created would then become unobservable. Inflation, remember, is relentless, and what happened just a tiny fraction of a second ago is now more than an entire visible Universe away. On all scales, from the very small to the very large, there should be these quantum fluctuations not only imprinted, but continuously newly imprinting on the Universe.

A representation of flat, empty space with no matter, energy or curvature of any type. With the exception of small quantum fluctuations, space in an inflationary Universe becomes incredibly flat like this, except in a 3D grid rather than a 2D sheet. Space is stretched flat, and particles are rapidly driven away, with a small, 1-part-in-30,000 fluctuation (not visible here) remaining as the only deviation from uniformity. (Amber Stuver / Living Ligo)

Yet inflation doesn’t last forever everywhere in the Universe. Every time new space is created, there’s a small-but-finite probability that inflation will be brought closer to its inevitable end. One way to visualize whether inflation ends or not is to picture a ball that rolls very, very slowly atop a plateau. Below the plateau is a valley that lies below; if the ball rolls into the valley, inflation ends.

When you create new space, there’s again a random distribution of probabilities: whether the ball rolls closer to the plateau’s center or closer to the edge. For the places where the ball reaches the edge and rolls into the valley, inflation ends and the energy transforms into the energy of the hot Big Bang.

Inflation ends (top) when a ball rolls into the valley. But the inflationary field is a quantum one (middle), spreading out over time, and taking on different values in different regions of inflating space. While many regions of space (purple, red and cyan) will see inflation end, many more (green, blue) will see inflation continue, potentially for an eternity (bottom). (E. Siegel / Beyond The Galaxy)

It was very likely that the first regions to undergo this transition weren’t the ones that became our observable Universe, but that we survived while these other Big Bangs occurred elsewhere in our inflating Universe. Most of them were incredibly distant, but some of them may have occurred very close to the region that eventually became our Universe. As long as inflation goes on, space continues to be filled with these energy fluctuations on all scales, creating a fabric of space that appears like a continuously vibrating grid. Not just on one scale, like we imagine a passing gravitational wave would induce, but on all scales.

As ripples through space arising from distant gravitational waves pass through our Solar System, including Earth, they ever-so-slightly compress and expand the space around them. During inflation, ripples and fluctuations in space also exist, but on all scales.(European Gravitational Observatory, Lionel BRET/EUROLIOS)

Finally, inflation comes to an end where we are. It’s as though all of this energy inherent to space, with slightly different values at different locations, all comes tumbling down. It transforms into matter, antimatter, and radiation, and creates a Universe that is now hot, dense, and uniform in temperature, rather than cold and empty. This transition is known as cosmic reheating, and it marks the transition from an inflationary spacetime into the beginning of our hot Big Bang. The energy fluctuations become density fluctuations, which gives rise to the large-scale structure in our Universe today.

When inflation comes to an end, our Universe as-we-know-it begins.

The analogy of a ball sliding over a high surface is when inflation persists, while the structure crumbling and releasing energy represents the conversion of energy into particles. (E. Siegel)

In theory, what lies beyond the observable Universe will forever remain unobservable to us, but there are very likely large regions of space that are still inflating even today. Once your Universe begins inflating, it’s very difficult to get it to stop everywhere. For every location where it comes to an end, there’s a new, equal-or-larger-sized location getting created as the inflating regions continue to grow. Even though most regions will see inflation end after just a tiny fraction of a second, there’s enough new space getting created that inflation should be eternal to the future.

This illustration shows regions where inflation continues into the future (blue), and where it ends, giving rise to a Big Bang and a Universe like ours (red X). Note that this could go back indefinitely, and we’d never know, but once it ends in our region, we cannot see the places beyond our horizon where it still inflates. (E. Siegel / Beyond The Galaxy)

Inflation set up and created the entire observable Universe, and gave the hot Big Bang the conditions we need it to have to be consistent with what we observe. But the inflationary Universe was dramatically different than the Universe we observe today. In order to understand and visualize it, we have to put our intuition aside, and embrace a reality where the only energy that matters is the energy intrinsic to the fabric of space itself.


Starts With A Bang is now on Forbes, and republished on Medium thanks to our Patreon supporters. Ethan has authored two books, Beyond The Galaxy, and Treknology: The Science of Star Trek from Tricorders to Warp Drive.