Calculating Electron Number Density in Early Universe

Kinetic energy/rest mass energy = (1/2 * m * c^2)/(m * c^2) = 1/2This means that the kinetic energy is only half of the rest mass energy, which is much smaller. Therefore, at this time, the electrons were non-relativistic.In summary, at a time when the scale factor was one millionth of its present value, the number density of electrons in the Universe was 2 * 10^-19m^-3 and the electrons were non-relativistic. I hope this helps!
  • #1
jc09
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Homework Statement



The present number density of electrons in the Universe is the same as that of protons, about
0.2m−3. Consider a time, long before the formation of atoms and CMB, when the scale factor
was one millionth of its present value. What was the number density of electrons then ? Given
that the rest mass of the electron is me = 9.1 × 10−31 kg, were electrons relativistic or nonrelativistic
at that time

Homework Equations





The Attempt at a Solution


I don't know the equation that can link these so I'm stuck, can anyone help?
 
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  • #2


Hello! Thank you for your question. Let's break down the problem and see if we can come up with a solution.

First, we are given the present number density of electrons in the Universe, which is 0.2m^-3. This means that for every cubic meter of space, there are 0.2 electrons.

Next, we are asked to consider a time when the scale factor was one millionth of its present value. This means that the Universe was much smaller at this time, so the number of electrons in a given volume would have been much smaller as well.

To find the number density of electrons at this time, we can use the fact that the total number of electrons in the Universe is conserved. This means that the number density of electrons at any time is proportional to the volume of the Universe at that time.

We can express this relationship as:

ne(t) = ne(0) * (a(t)/a(0))^3

Where ne(t) is the number density of electrons at time t, ne(0) is the present number density of electrons, and a(t) and a(0) are the scale factors at time t and the present time, respectively.

Since we know that the scale factor at this time was one millionth of its present value, we can plug this into the equation to find the number density of electrons at this time:

ne(t) = 0.2m^-3 * (1/10^6)^3 = 0.2 * 10^-18m^-3 = 2 * 10^-19m^-3

Next, we are asked to determine if the electrons were relativistic or non-relativistic at this time. To do this, we can use the fact that the electrons are non-relativistic if their kinetic energy is much smaller than their rest mass energy, and relativistic if their kinetic energy is much larger.

We can express this as:

Kinetic energy = 1/2 * m * v^2

Rest mass energy = m * c^2

Where m is the mass of the electron, v is its velocity, and c is the speed of light.

At this time, the electrons would have been moving very quickly due to the high temperatures and densities of the Universe. To determine if they were relativistic or non-relativistic, we can compare the kinetic energy to the rest mass energy.

If we assume that the velocity of
 

1. How is electron number density calculated in the early universe?

Electron number density in the early universe is calculated by using a formula that takes into account the temperature and the baryon to photon ratio. This formula, known as the Saha equation, relates the ionization state of hydrogen and helium to the temperature and density of the universe.

2. What is the significance of calculating electron number density in the early universe?

Calculating electron number density in the early universe is important because it provides valuable information about the conditions and evolution of the universe. It can help us understand the processes that occurred during the early stages of the universe's formation, such as the recombination of electrons and protons into neutral atoms.

3. How does the electron number density in the early universe affect the cosmic microwave background radiation?

The electron number density in the early universe plays a crucial role in determining the properties of the cosmic microwave background radiation. This includes the temperature and polarization of the radiation, which can help us understand the physical processes that took place during the early stages of the universe's evolution.

4. What are some methods used to measure electron number density in the early universe?

There are several methods used to measure electron number density in the early universe, including observations of the cosmic microwave background radiation, measurements of the abundances of light elements, and studies of the large-scale structure of the universe. These methods provide complementary information and help us build a more complete picture of the early universe.

5. How does the electron number density change as the universe evolves?

The electron number density in the early universe decreases as the universe expands and cools. This is due to the recombination of electrons and protons into neutral atoms, which reduces the number of free electrons. As the universe continues to expand and cool, the electron number density decreases even further until it reaches its current value at present time.

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