Friedmann's equation for a^3 with Λ, ρm

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SUMMARY

The discussion centers on proving the equation a3(t) = ρo/2Λ [cosh(sqrt(24πGΛ)*t) - 1] using the variable substitution u = 2Λa3o. The participants analyze Friedmann's equations, particularly focusing on the relationship between Λ and ρm, concluding that the assumption of a direct proportionality between them is incorrect. The second attempt at deriving the equation reveals that the integration process consistently fails to yield the cosh function, indicating a fundamental misunderstanding of the relationship between Λ and ρm as the universe expands.

PREREQUISITES
  • Understanding of Friedmann's equations in cosmology
  • Familiarity with variable substitution in differential equations
  • Knowledge of hyperbolic functions, specifically cosh
  • Basic principles of cosmological parameters, including Λ (cosmological constant) and ρm (matter density)
NEXT STEPS
  • Study the derivation of Friedmann's equations in detail
  • Learn about the implications of the cosmological constant Λ in an expanding universe
  • Explore the relationship between matter density ρm and the scale factor a(t)
  • Investigate hyperbolic functions and their applications in cosmological models
USEFUL FOR

Astronomers, cosmologists, and physics students interested in the mathematical foundations of cosmological models and the dynamics of the universe's expansion.

QuarkDecay
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Homework Statement
We have a flat Universe with a positive Λ, density matter ρ[SUB]m[/SUB]. Need to prove the formula for a[SUP]3[/SUP](t) below from the first Friedmann equation and changing the variable from the u=(...) given below
Relevant Equations
- Friedmann's first equation; H[SUP]2[/SUP]= 8πGρ[SUB]total[/SUB]/3 - k/a[SUP]2[/SUP]
- New variable; u=2Λa[SUP]3[/SUP]/ρ[SUB]o[/SUB]
We need to prove that a3(t)= ρo/2Λ [cosh(sqrt(24πGΛ)*t) -1] by changing into a variable of u, where
u=2Λa3o

From Friedmann's second equation we know that Λ= ρm/ 2
Also ρm= ρo/ a3

[First attempt]
I begin from Friedmann's equation where (for here), ρtotal= ρm + Λ and k=0;

a'2/a2 = 8πG(ρm + Λ)/3 , (a'=da/dt)

⇒ a'/a = sqrt ((8πG/3) * (3ρo/2a3) )

⇒∫ da/a = ∫sqrt((8πG/3) * (3ρo/2a3))dt

⇒ lna = sqrt((8πG) * (ρo/2a3)) t

⇒ a= exp [sqrt((8πG) * (ρo/2a3))t ]

which is not close with what we're trying to prove, and I didn't use the variable u I was supposed to. The solution is the correct for a flat universe, but when we're looking for the a(t). Seems like I have to change the a into u completely inside friedmann's equation.

So I tried this too; (second attempt)

a'2/a2 = 8πG(ρm + Λ)/3

⇒ a'/a = sqrt ((8πG/3) * (3ρo/2a3)) = sqrt(4πGρo/a3) ⇒

⇒ da/dt = a*sqrt(4πGρo/a3) = sqrt(a24πGρo/a3)=

= sqrt(4πGρo/a) (a)

and now changing the variable from a to u;

u=2Λa3o ⇒ a3 = uρo/2Λ ⇒

a= [uρo/2Λ] 3/2 (1)

So,
da= (ρo/2Λ) 3/2 u1/2du (2) (a),(1),(2) → ... du/u1/2= sqrt(8πGΛ)dt = sqrt(8πGΛ)t

Where the cosh() is still missing...
In the first attempt I had the exact same problem too. The first integral was always da/sqrt(a) that doesn't give a cosh for a solution
 
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QuarkDecay said:
From Friedmann's second equation we know that Λ= ρm/ 2
This is not true. You have not been given the relation between ##\Lambda## and ##\rho_m## and the proportion between them is arbitrary. Furthermore, ##\rho_m## is going to change as the universe expands, which ##\Lambda## will not.

QuarkDecay said:
8πG(ρm + Λ)/3 , (a'=da/dt)

⇒ a'/a = sqrt ((8πG/3) * (3ρo/2a3) )
Which means that this is wrong. As stated above ##\Lambda## will depend on ##a## in a different way from ##\rho_m##.
 

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