In the beginning....

Well, what we're calling the beginning here is the universe when it had a temperature of 100,000,000,000 K. The universe had already existed for a very small fraction of a second. The universe was dominated by radiation. There was some matter present, but it was minuscule compared to the amount of radiation. The radiation was in the form of photons, neutrinos (and anti-neutrinos). The matter present was in the form of electrons, positrons, and a very small concentration of protons and neutrons (about 1 part per billion). As a result of the extremely high temperature and density present, all of these items acted like particles. This means that they were constantly colliding into each other, just like a sample of tightly-packed marbles in a container. In the early universe there were no physical "walls" to contain these objects, but there were so many collisions happening so quickly that the collisions themselves acted like the "walls" of the universe. But, these "walls" were not static. With the collisions, the size of the universe was increasing. This expansion caused the density of energy to go down as it was spread out over a larger volume. This resulted in a decrease in the temperature of the universe. This process continues to happen today.

These collisions had three major results. The first was that the universe reached a condition called thermal equilibrium. To give you an idea about what this is we'll look at a glass of water at 40 degrees. The temperature of an object is a reflection of the amount of energy present in that sample of matter. But, not every molecule has the energy that corresponds to 40 degrees. The total energy is actually spread out over a range of energies, so that there are some that have more energy than the corresponding temperature, and others that have less.

These molecules are constantly colliding with the surrounding molecues. This results in exchanges in energy. This causes the number of molecules at certain energies to change. If something is in thermal equilibrium, for every molecule that changes its energy level , there will be another molecule changing its energy level to replace it (not necessarily in the same collision). In a way, this means that the energy present in a system is spread out among particles in such a way that the population of molecules at different energies doesn't change, even though the molecules themselves are constantly changing energy levels. In the early universe, as a result of the rapid collisions between particles, there was a state of thermal equilibrium. The reason this is so important is that things in thermal equilibrium can be quantified. This means that the system can be described by mathematical formulas, and that predictions can be made as to how the system would would change with time. Therefore, we can follow the evolution of the early universe through these formulas, even though we weren't there.

The other two consequences of these collisions involve interactions between particles as they collided.

The first interaction to be considered was the constant annihilation and re-creation of electrons and positrons. One of the most famous scientific discoveries of this century is the equivalence of matter and energy. The basic concept is that under the proper conditions, energy can be turned into matter, or vice versa. This is not something common to our experience because of the conditions in which we now live (it's too cold and there's not enough pressure). But in the early universe, with its high temperature and density, this was a way of life. Photons were converted into electrons and positrons. (Known as PAIR PRODUCTION) They could not be converted into heavier particles (protons and neutrons) because they didn't have enough energy. These electrons and positrons would eventually collide with their respective anti-particle, and then be changed back into radiation. (Referred to as ANNIHILATION)

The second interaction was the conversion between protons and neutrons. These heavier atomic particles were already present "In the Beginning". They were continually changing back and forth by means of the following two reactions:

"In the beginning", because of the high energy density, the collisions between particles happened so rapidly that the proton- and neutron-creating reactions balanced each other out, and the relative number of protons and neutrons, though small, were equal. But, the equality between protons and neutrons was broken almost immediately. A neutron is slightly heavier than a proton. Therefore, it requires a little more energy to change a proton into a neutron than vice versa. Initially this didn't matter because there was plenty of energy to go around. But, because the energy density was decreasing as the universe expanded, there was less energy available for each collision. This started to tip the balance in favor of the proton-forming reactions. This lead to an increase in the number of protons compared to neutrons, and as the temperature dropped more, this effect became more exaggerated. (The final numbers will be mentioned later on.)

According to the formulas, at 13.82 seconds after "the Beginning", the temperature had dropped to 3,000,000,000 K. At this point there was a drastic reduction in the population of electrons and positrons. The reason for this was once again the expansion of the universe. As electrons and positrons annihilated, the radiation formed was being stretched (specifically its wavelength) by the growing universe. This reduced the energy carried by the photons below the level which would allow them to be converted back into electrons and positrons.

Up to this time (just over three minutes past "The Beginning") there had been no nucleosynthesis. This was a result of the high energy density. In order to form atomic nuclei, the nucleons (a science word for protons and neutrons) must be able to collide and stick together. In the early universe the key reaction was the collision of a proton and a neutron to form a deuterium nucleus (an isotope of hydrogen). Collisions between protons and neutrons had been happening continuously since "The Beginning", but their energies were too high to allow them to stick together to form deuterium nuclei.

This prevented further nuclear reactions leading to heavier nuclei. This type of situation where an intermediate product is the weak link in the overall synthesis is sometimes called a "bottleneck". This concept also applies in nucleosynthesis of heavier elements. Once the "bottleneck" is overcome, the remaining reactions are able to be completed. In the early universe, once the deuterium bottleneck was cleared, the newly formed deuterium could undergo further nuclear reactions to form Helium.

This could happen by means of two different reaction pathways described below.

Pathway #1

The deuterium nucleus collides with a proton to form He-3, then a neutron to form He-4.

Pathway #2

The deuterium collides first with a neutron to form H-3 (more commonly called tritium), then with a proton to form He-4.

He nuclei were the heaviest to form. This was the result of the energy density being too low to allow heavier nuclei to collide with enough energy to stick. At the time that nucleosynthesis began, the relative abundance of protons to neutrons was: 13% neutrons and 87% protons. When nucleosynthesis began, all the neutrons present were incorporated into He nuclei. When all the neutrons were used up, the remaining protons remained as hydrogen nuclei. So, when this first wave of nucleosynthesis was completed, the universe consisted of roughly 25% He and 75% H (by weight).

The final step in the formation of elements was capture of the proper number of free electrons to form neutral atoms. But, the remaining electrons still had plenty of energy, so it took about 700,000 years of cooling until this was able to occur. The capture of electrons to form atoms resulted in an important change in the universe. At that moment, without free electrons to interact with the photons present, the universe became transparent to radiation. This means that the photons were freely able to expand with the universe. These photons had high energies, which means that they had short wavelengths. But the expansion of the universe caused the wavelengths to get stretched out as the universe grew. These stretched out photon wavelengths are what we now refer to as the Cosmic Microwave Background (CMB). They are a leftover from the Big Bang. We have been able to measure the intensity of this background radiation, and it has closely matched that which is predicted from theoretical calculations. This has been a atrong evidence in support of the "Big Bang" theory of the universe's creation.

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