Well, I want to get C_{l}, right? That is why I apply P_{l} on the correlation function (1) and integrate - it removes P_{l} and the sum leaving C_{l} * some factor in l. Where do you see a mistake?
Thanks.
Hello.
I don't know what to do with one integral. I am sure it is something very simple, but I just don't see it...
For some reason I am not able to post the equations, so I am attaching them as a separatre file.
Many thanks for help.
Hi all.
I have been applying for graduate (research) studies in Astrophysics (I am interested in cosmology - CMB, SNIa, models...) at some UK universities - Imperial College, Durham, Glasgow, Manchester.
All of them have research groups in the field of cosmology.
So far I have received an...
Thanks a lot, you opened my eyes... For some reason I didn't see the simple solution of plotting it as a parametric equation where x = t[\Theta] and y = R[\Theta]...
I was probably expecting something more complicated...
I doubt the result could be solved explicitly for R...
Right now I've got three books in Astrophysics/Cosmology here, every of them provides the parametric solutions (above) and clearly explains how to get the age of the universe from it (expressing parameters in terms of...
Simply, say, I want to make a plot of evolution of the scale factor R vs. t. Such plots are probably in every book which has something to do with cosmology.
To do this I need R as a function of t, unfortunatelly have no idea how to get it.
When k = 0, it's a simple differential equation...
Hello everybody,
could somebody tell me how to get the scale factor as a function of time [R(t)] from the Friedmann Equations for a simple dust, pressureless universe when k != 0, \Lambda = 0.
Mathematica 5.2 doesn't want to give me any solution and wherever I searched the best thing I got...
Mistake in the equation
It is probably too late, but I am quite sure that the equation should look like this:
]S=Nk\left[ \ln \left(\frac{A}{N}\right) + \ln \left(\frac{2\pi mU}{\hbar^2 N}\right) +2\right]