Deceleration Parameter Computation

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Discussion Overview

The discussion focuses on the computation of the deceleration parameter (##q_0##) in the context of a radiation-dominated universe. Participants explore the relationships between the scale factor, its derivatives, and the density parameters involved in the calculation.

Discussion Character

  • Technical explanation
  • Mathematical reasoning
  • Debate/contested

Main Points Raised

  • One participant seeks guidance on computing ##q_0## for a radiation-dominated universe, referencing specific equations and values for density parameters.
  • Another participant points out that the value for ##\Omega_{rad}## provided may not be appropriate for a radiation-dominated scenario, as the current universe is not in that state.
  • A participant expresses confusion about the calculation process and shares their derivation of ##q_0## using the scale factor and its derivatives.
  • One participant notes that a radiation-dominated universe is characterized by ##\Omega_{rad}## being close to one, but does not verify the calculations presented.
  • Another participant reiterates the calculation of ##q_0## and highlights a potential oversight regarding the sign in the formula.

Areas of Agreement / Disagreement

Participants express uncertainty about the appropriateness of certain values and calculations, indicating that multiple views on the correct approach remain. The discussion does not reach a consensus on the computation of ##q_0##.

Contextual Notes

Participants reference various assumptions about the scale factor and density parameters, but there is no resolution on how to correctly compute ##\Omega_0## or the implications of using current values in a radiation-dominated context.

roam
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Hi everyone,

Can anyone point me into the right direction on how to compute the deceleration parameter (##q_0##) for a radiation dominated universe?

I know that q0 is given by

##q_0=-\frac{\ddot{a}(t_0)}{a(t_0) H^2 (t_0)} = - \frac{\ddot{a}(t_0) a(t_0)}{\dot{a}^2(t_0)}=\frac{\Omega_0}{2}##​

So for a radiation dominated universe, we have ##\omega = + \frac{1}{3}##. And ρ~1/a4, and a~t1/2. I'm not sure how to relate this to that equation.

My notes say ##\Omega _{rad} = 8.2 \times 10^-5## but I'm not sure how this was calculated. How do I compute Ω0=ρ/ρcrit in this case? I know that ρcrit=3H2/8πG, but what is the density ρ? :confused:

Using that value I get the following but I'm not sure if it's correct:

##q_0 = \frac{\Omega_0}{2} = \frac{8.2 \times 10^-5}{2} = 4.1 \times 10^{-5}##.

I couldn't find any info on this computation online. So any help is greatly appreciated.
 
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You have a(t), and since H(t) = \dot{a}(t)/a(t) and q(t) is fully determined by a(t), you should be good to go...

Your value for \Omega_{rad} is the current radiation density in the actual universe, which isn't radiation dominated and not appropriate for use with w=1/3, etc.
 
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Thank you for the clarification regarding ##\Omega##, it makes perfect sense now.

But I'm still not sure how the calculation goes (my book lacks any worked problems) :confused:

Since for a radiation dominated universe we had the scale factor a~t1/2, with its time derivatives ##\dot{a}=\frac{1}{2 t^{1/2}}##, and ##\ddot{a}=\frac{-1}{4t^{3/2}}##, then

##q_0 = \frac{\ddot{a}}{a \left( \dot{a}/a \right)} = \frac{-1}{16t^{6/2}}##

Is this correct?
 
A radiation-dominated universe is one where \Omega_{rad} is very close to one. I haven't checked your math at all, but hopefully that helps you get the right answer.
 
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A radiation-dominated universe has positive deceleration (negative acceleration).

roam said:
Since for a radiation dominated universe we had the scale factor a~t1/2, with its time derivatives ##\dot{a}=\frac{1}{2 t^{1/2}}##, and ##\ddot{a}=\frac{-1}{4t^{3/2}}##, then

##q_0 = \frac{\ddot{a}}{a \left( \dot{a}/a \right)} = \frac{-1}{16t^{6/2}}##

Is this correct?

You forgot the initial minus sign.
 
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Thank you very much. :)
 

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