There is a law in this universe that states: Energy may be transformed from one kind to another, but it cannot be created or destroyed. Einstein's formula E=mc2 shows that mass and energy are the same thing. Particles like electrons and protons have rest energy.
The classical big bang (BB) theory starts the universe with all the matter present today at the start (in some form). The inflationary version (Alan Guth, 1980) has a brief period of extraordinarily rapid expansion (inflation) which lasted for maybe 10-30 seconds, and expanded the universe by at least a factor of 1025. This expansion was faster than the speed of light. The initial 'seed' weighed about an ounce (25 grams), and had a diameter more that a billion times smaller than a proton.
Edwin Hubble discovered that most galaxies are receding from us because of red-shifted light (see Doppler effect). A galaxy twice as far away is receding about twice as fast (proportional to distance). The Hubble constant is between 15 and 30 kilometers per second per million light years. Hubble's law is interpreted as evidence that the universe is undergoing homogeneous expansion. It is also assumed that there is no center and no edge to the distribution of galaxies.
The ultimate fate of the universe (according to BB theory) depends on the average mass density of the universe. If the mass density exceeds a critical value (that can be calculated from the expansion rate) then gravity will win out and the expansion will reverse and we will have the 'big crunch.' This is called a closed universe. A closed universe is finite in volume, but has no edge or boundary. If a rocket ship were to travel for a sufficiently long time in what would appear to be a straight line, it would come back to the starting point. If the mass density is less than the critical value the universe will go on expanding forever (open universe). If the mass density is precisely at the critical value then the universe is called flat. It would continue to expand without limit, but the rate of expansion would become closer and closer to zero as time goes on. The slowing of the expansion due to gravity is described by the equations of Friedmann and Lemaitre, based on Einstein's theory of general relativity. The critical density is believed to be between 4.5 x 10-30 and 1.8 x 10-29 grams per cubic centimeter. This is between 2 and 8 hydrogen atoms per cubic yard (more than 10 million times lower than the best vacuum than can be achieved in a laboratory)! The Greek letter omega (W) is used to denote the ratio of the actual mass density to the critical density. If it is >1 then the universe is closed.
The inflationary version of the BB theory explains the flatness problem. Robert Dicke at Princeton University concluded that 1 second after the BB that W had to be between 0.999999999999999 and 1.0000000000000001 (1 to 15 decimal places) or the universe would not resemble our own. The classical BB theory offers no explanation for this value. With inflation, omega is driven toward 1 with incredible swiftness. Before inflation W could have been 0.000001 or 1 million. As long as exponential expansion continues long enough, W will be driven toward 1 with extreme precision. In doubling 100 times, the difference between W and 1 decreases by a factor of 1060.
The inflationary version also explains the horizon problem. At 300,000 years after the BB, the universe was transparent to light, allowing the Cosmic Background Explorer (COBE) to look around. The photons of the cosmic background radiation have been traveling in a straight line since that time. The horizon distance (the maximum distance that light could have traveled since the beginning of time) was 900,000 light-years. Two photons coming at us from opposite directions 90 million light-years apart are 100 times the horizon distance. The zeroth law of thermodynamics can't operate outside the horizon distance, so there was no way to get everything at the same temperature. The only way the classical BB theory can explain it is to assume that the universe began in a state of uniformity. With inflation, the size of the universe before inflation was incredibly small, and the speed of light imposed no barrier. There was plenty of time before inflation for cosmic uniformity to be established.
A big boon to the BB theory is the cosmic background radiation (CMB). It was discovered by Arno Penzias and Robert Wilson in 1964 at Crawford Hill, New Jersey, as a hiss in a microwave communications receiver. That is what is expected when the 'fabric of space' is stretched out which contained very high energy light in a small space. The expansion stretches the wavelength of light to microwave radio frequencies. By early 1965 Jim Peebles had a prediction of the spectrum of the radiation – the way in which the energy density varies with the frequency or wavelength. It would be a blackbody spectrum at a temperature of 10 degrees centigrade above absolute zero (10 Kelvin). The cooling caused by the expansion is understood by using conventional thermal physics. The cooling robs the particles of most of their energy, transferring that energy to the gravitational field.
The measurements by Penzias and Wilson on their horn antenna (at 1 frequency) was about 3.5°K. This was considered quite close to the prediction. In November 1989, NASA launched COBE. This was after several other failed and inconclusive attempts. Measurements of the cosmic background radiation were at 67 wavelengths from far below the blackbody peak to far above it. The data fell on the theoretical blackbody curve to a high precision. The temperature measurement is 2.726°K with an uncertainty of less than 0.01°K. The temperature of the radiation is found to be the same in all directions to an accuracy of about 1 part in 100,000. The COBE team announced that the steady state theory is ruled out.
(Most of the above adapted from The Inflationary Universe by Alan Guth, copyright 1997)
I will talk about magnetic monopoles and Higgs fields in part 2. Let's discuss the horizon and flatness 'problems'. Are they really problems, or only in someone's mind?