A Numerically solving Scalar field coupled to Friedman equation

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The discussion centers on numerically solving the Friedmann equation coupled to a scalar field, as detailed in the research paper by Sean Carroll and colleagues. The author, a physics graduate student, seeks assistance due to a lack of understanding and urgency to complete their degree. A response from one of the paper's authors clarifies that while the problem is standard, it requires careful rescaling of parameters and emphasizes that only equations 5 and 14 need to be solved together, as others are redundant. The author suggests using Mathematica for the numerical solution and provides a resource for further guidance. This exchange highlights the challenges of tackling complex equations in theoretical physics.
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I am a research student of MS PHYSICS. I have to numerically solve Friedman equation coupled to scalar field(phi). It is given in research paper of Sean Carroll, Mark Trodden and Hoffman entitled as ""can the dark energy equation of state parameter w be less than-1?"" http://dx.doi.org/10.1103/PhysRevD.68.023509
The equations, that can be used are equation 5 and 14.
Plz someone help me, since it took me two extra semesters and I am on a verge of losing my degree, as per university policy.
I am a research student of MS PHYSICS. I have to numerically solve Friedman equation coupled to scalar field(phi). It is given in research paper of Sean Carroll, Mark Trodden and Hoffman entitled as ""can the dark energy equation of state parameter w be less than-1?"" http://dx.doi.org/10.1103/PhysRevD.68.023509
The equations, that can be used are equation 5 and 14.
Plz someone help me, since it took me two extra semesters and I am on a verge of losing my degree, as per university policy.
 
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I know 0 about this topic, however, I’d start by listing all boundary conditions and all symmetries the problem is expected to have. Every symmetry should allow you to reduce the complexity of the resulting differential equation. Hopefully this will greatly improve your chances for a numerical solution.
 
Will be a kind act.. thanks
 
Following is the reply i received from one of the author of the paper, when I requested him to help me
""""
Hi,
I won’t be able to spend a lot of time on this but your question is not really about our paper. You’re asking about solving the Friedman equation coupled to a scalar field. This is a standard system that many authors have solved numerically It can be done in Mathematica, but one should rescale parameters so that one need not use large dimensionaful parameters like the Planck mass. Furthermore, you need not solve equation all three equations since they are redundant. Solving 5 and 14 together is sufficient.

Typically, the more difficult part of this is the Friedman equation, which is first order. You can find an example of how to approach solving it here
https://web.physics.ucsb.edu/~gravitybook/mathematica.html

You would need to include the scalar equation and solve them simultaneously.
""""
 
https://en.wikipedia.org/wiki/Recombination_(cosmology) Was a matter density right after the decoupling low enough to consider the vacuum as the actual vacuum, and not the medium through which the light propagates with the speed lower than ##({\epsilon_0\mu_0})^{-1/2}##? I'm asking this in context of the calculation of the observable universe radius, where the time integral of the inverse of the scale factor is multiplied by the constant speed of light ##c##.
Why was the Hubble constant assumed to be decreasing and slowing down (decelerating) the expansion rate of the Universe, while at the same time Dark Energy is presumably accelerating the expansion? And to thicken the plot. recent news from NASA indicates that the Hubble constant is now increasing. Can you clarify this enigma? Also., if the Hubble constant eventually decreases, why is there a lower limit to its value?
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