Solving Friedmann Equation for Cosmology

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Homework Help Overview

The discussion revolves around deriving an integral relating the scale factor to time using the Friedmann equation in the context of a flat universe. The original poster expresses confusion regarding the mathematical aspects of the problem, specifically in manipulating the equation and understanding the implications of density components.

Discussion Character

  • Exploratory, Conceptual clarification, Mathematical reasoning

Approaches and Questions Raised

  • Participants discuss the correct formulation of the Friedmann equation and the implications of a flat universe. There are attempts to express the relationship between scale factor and time, with questions about the functional forms of matter and vacuum energy densities as they relate to the scale factor.

Discussion Status

Some participants have offered guidance on writing the Friedmann equation correctly and suggested considering the dependencies of density on the scale factor. There is ongoing exploration of how to express these densities and their changes as the universe expands, indicating a productive direction in the discussion.

Contextual Notes

There is mention of the need for explicit functional forms of density to perform the integral, and participants are questioning how the densities of matter and vacuum energy change with the expansion of the universe.

foranlogan5
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:confused: could anyone please help me with this coursework,i am soo confused with maths,thanks
1)

Start with friedmann equation for case for flat universe k=0 with mass density total p =p(m) + p(cosmo constant). how can i derive integral relating scale factor to time in form

$f(a)da = $(8piG/3)^(1/2) where $=integral
then by using change of variable a to s
s = {(p(cos)/p(mo))x(a/a(o))^3}^(1/2)

and

Then another change of variable s to (THETA) = sinh^-1(s) should be able to calculate integral in A to obtain a relation for t = G(A) WHERE G(A) YOU DERIVE


where p(mo) is density matter at t =0 and a(o) is scale factor at time t=0
x=times
^3= to power of three
sinh(s)^-1 does not equal 1 /sinh(s)
 
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Well, first you should write down the correct Friedmann equation.

Note that you need to show some work before we can help you here. Also, if you intend writing long mathematical expressions, it may be worth learning to use the board's \LaTeX feature.
 
thanks cristo, friedmann H^2 = (8piG/3)p + (kc^2)/(a^2)
and i'll consider learning latex
 
Now, you are told that the space is flat, so that should make a change to your Friedmann equation. Write H in terms of the scale factor and its time derivative. You should be able to write rho_m and rho_lambda in terms of the scale factor also.
 
da/{ax(rho_m +rho_lamb)^1/2} = dt(8piG/3)^1/2
is that the answer to first part?
i think that's correct
 
foranlogan5 said:
da/{ax(rho_m +rho_lamb)^1/2} = dt(8piG/3)^1/2
is that the answer to first part?
i think that's correct

I s either \rho_m or \rho_\Lambda a function of a? In order to do the integral, explicit functional forms must be used.
 
could you further that point george,i don't quite understand what you are saying?
 
foranlogan5 said:
could you further that point george,i don't quite understand what you are saying?

As the universe expands, does the density of matter change? What about the energy density of the vacuum? If they do change, in what way? If they do change, you might want to write them in terms of their values now (look at your first post) and a.
 

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