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pi.rootpi
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Hey! I'd like to see an easy way to arrive to Friedmann equation by using Newton's Mechanics. I've seen many ways but they skip many steps so I don't understand the whole.
THANKS!
THANKS!
Wikipedia said:The Friedmann equations are a set of equations in cosmology that govern the expansion of space in homogeneous and isotropic models of the universe within the context of general relativity. They were first derived by Alexander Friedmann in 1922[1] from Einstein's field equations of gravitation for the Friedmann-Lemaître-Robertson-Walker metric and a fluid with a given mass density ρ and pressure p. The equations for negative spatial curvature were given by Friedmann in 1924.
Orion1 said:
As stated by Wikipedia, the Friedmann equations are derived from General Relativity, not from Newtonian Mechanics. If you are interested in how these equations were derived, I recommend reading Friedmann's actual papers themselves, they are listed in reference 1 below, at the end of page in Reference as well as most of the important equations.
Reference:
http://en.wikipedia.org/wiki/Friedmann_equations" [Broken]
Affirmative, the units have changed in the relativistic harmonic oscillator potential energy well.but in the final Friedmann equation, the units have switched...
Negative.If you were to model a classical circular orbit, which accounted for the Lambda force, would the following form be correct?
The Friedmann Equation is a mathematical equation that describes the expansion of the universe in the context of general relativity. It was derived by Alexander Friedmann in 1922 and is a key component in understanding the evolution and dynamics of the universe.
The Friedmann Equation is derived by incorporating Newton's laws of motion into the equations of general relativity. This allows us to describe the expansion of the universe using the principles of classical mechanics, which are more intuitive and easier to understand than the complex mathematics of general relativity.
The Friedmann Equation is based on a few key assumptions, including the cosmological principle (the universe is homogeneous and isotropic on large scales), the principle of energy conservation, and the presence of matter and energy in the universe. These assumptions allow us to simplify the equations and make them more manageable.
The Friedmann Equation is used to study the evolution and dynamics of the universe, including its expansion rate, density, and curvature. It is also used to make predictions about the future of the universe, such as whether it will continue to expand or eventually collapse.
The Friedmann Equation has several important implications for our understanding of the universe. It supports the idea of a constantly expanding universe, which is a key concept in the Big Bang theory. It also helps us understand the role of dark matter and dark energy in the universe, and how they contribute to its overall expansion and structure.