Exploring the General Form of FLRW Metric

In summary, the "generic" form of the FLRW metric is ds^2=(cdt)^2-dl^2 and the three-dimensional spatial metric can be found by plugging in the curvature parameter K into the formula dl^2=a^2(\frac{dr^2}{1-Kr^2})+r^2d\Omega^2).
  • #1
Fleet
8
0
Hi all,

I have found the "generic" form of the FLRW metric:
[tex]ds^2=(cdt)^2-dl^2[/tex]

And I have found the three-dimension spatial metric for euclidian space (K=0, spherical space K=1 and hyperboloid space (K=-1):

[tex]dl^2=a^2(dr^2+r^2d\Omega^2)[/tex]

[tex]dl^2=a^2(\frac{dr^2}{1-r^2})+r^2d\Omega^2)[/tex]

[tex]dl^2=a^2(\frac{dr^2}{1+r^2})+r^2d\Omega^2)[/tex]

BUT how do I find the "general" form of the FLRW metric, how can I include the curvature parameter K?

Please help, I really need it!

Best regards.
 
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  • #2
What happens if you just stick a K into the formula, with the understanding that it can take on just those 3 values: -1,0,and 1? Don't you get the three cases you want?

[tex]dl^2=a^2(\frac{dr^2}{1-Kr^2})+r^2d\Omega^2)[/tex]

Fleet said:
Hi all,

I have found the "generic" form of the FLRW metric:
[tex]ds^2=(cdt)^2-dl^2[/tex]

And I have found the three-dimension spatial metric for euclidian space (K=0, spherical space K=1 and hyperboloid space (K=-1):

[tex]dl^2=a^2(dr^2+r^2d\Omega^2)[/tex]

[tex]dl^2=a^2(\frac{dr^2}{1-r^2})+r^2d\Omega^2)[/tex]

[tex]dl^2=a^2(\frac{dr^2}{1+r^2})+r^2d\Omega^2)[/tex]

BUT how do I find the "general" form of the FLRW metric, how can I include the curvature parameter K?
...
 
  • #3
Thank you very much for you answer, I really appreciate it!

Yes, you are right I get the cases I want. But are you questioning to be ironical or are you sure it the correct way? :)

Love this forum, I'm going to contribute

Best regards
 
  • #4
Fleet said:
Yes, you are right I get the cases I want. But are you questioning to be ironical or are you sure it the correct way? :)

It is the correct way. The general form for the line element is the one that marcus gives. Plugging in values for k gives you the three specific line elements.
 

FAQ: Exploring the General Form of FLRW Metric

What is the FLRW metric and why is it important in cosmology?

The FLRW metric is a mathematical model used to describe the large-scale structure of the universe. It is a solution to Einstein's field equations in general relativity and describes a homogeneous and isotropic universe. It is important in cosmology because it serves as the basis for many theories and models used to understand the evolution and structure of the universe.

How does the FLRW metric relate to the Big Bang theory?

The FLRW metric is an essential component of the Big Bang theory. It describes the expanding universe and allows us to calculate the cosmic scale factor, which represents the change in size of the universe over time. By plugging the scale factor into the FLRW metric, we can determine the age and expansion rate of the universe, providing evidence for the Big Bang theory.

What are the four types of FLRW metrics and how do they differ?

The four types of FLRW metrics are named after the mathematicians who first derived them: Friedmann, Lemaître, Robertson, and Walker. They differ in their assumptions about the geometry and expansion of the universe. Friedmann and Lemaître assume a flat geometry and no cosmological constant, while Robertson and Walker allow for a non-zero cosmological constant and different curvatures.

How are the FLRW metric and the Hubble law related?

The FLRW metric and the Hubble law are closely related as they both describe the expansion of the universe. The Hubble law states that the recession velocity of galaxies is proportional to their distance from Earth. This can be derived from the FLRW metric by solving for the scale factor and taking the derivative with respect to time. Therefore, the FLRW metric provides a mathematical explanation for the Hubble law.

What are the implications of the FLRW metric for the fate of the universe?

The FLRW metric has important implications for the fate of the universe. By using the FLRW metric and plugging in different values for the density and cosmological constant, we can determine the ultimate fate of the universe. If the density is high enough, the universe will eventually stop expanding and collapse in a Big Crunch. If the density is too low, the universe will continue to expand forever in a state of heat death. The FLRW metric helps us understand and predict these possible outcomes.

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