How Do General Relativity Tensors and Their Indices Work?

In summary, the conversation discusses the definitions of the Hodge dual and exterior derivative of a p-form, and the relation between them involving the orientation of the manifold. The question is then posed about a specific calculation involving these definitions. Through a series of steps, it is shown that the desired result is obtained by applying the relation and using properties of antisymmetrization.
  • #1
vidi
6
0
This is a question on the nitty-gritty bits of general relativity.

Would anybody mind teaching me how to work these indices?

**Definitions**:

Throughout the following, repeated indices are to be summed over.

Hodge dual of a p-form [itex]X[/itex]:
[tex](*X)_{a_1...a_{n-p}}\equiv \frac{1}{p!}\epsilon_{a_1...a_{n-p}b_1...b_p}X^{b_1...b_p}[/tex]
Exterior derivative of p-form [itex]X[/itex]: [tex](dX)_{a_1...a_{p+1}}\equiv (p+1) \nabla_{[a_1}X_{a_2...a_{p+1}]}[/tex]

Given the relation
[tex]\epsilon^{a_1...a_p c_{p+1}...c_n}\epsilon_{b_1...b_pc_{p+1}...c_n}\equiv p!(n-p)! \delta^{a_1}_{[b_1}...\delta^{a_p}_{b_p]}\,\,\,\,\,\,\,\,\,(\dagger)[/tex]
where [itex]\epsilon_{a_1...a_n}[/itex] is an orientation of the manifold.

Why then is
[tex](*d*X)_{a_1...a_{p-1}}=(-1)^{p(n-p)}\nabla^b X_{a_1...a_{p-1}b}[/tex]?Firstly, I believe [itex](*d*X)[/itex] means [itex]*(d(*X))[/itex]?
[tex](d*X)_{c_1...c_{n-p+1}}=\frac{n-p+1}{p!}\nabla_{[c_1}\epsilon_{c_2...c_{n-p+1}]b_1...b_p}X^{b_1...b_p}[/tex]
Then [tex]*(d*X)_{d_1...d_{p-1}}=\frac{n-p+1}{(n-p+1)!p!}\epsilon_{d_1...d_{p-1}c_1...c_{n-p+1}}\nabla^{[c_1}\epsilon^{c_2...c_{n-p+1}]b_1...b_p}X_{b_1...b_p}[/tex]
[tex]=\frac{1}{(n-p)!p!}\epsilon_{d_1...d_{p-1}c_1...c_{n-p+1}}\nabla^{[c_1}\epsilon^{c_2...c_{n-p+1}]b_1...b_p}X_{b_1...b_p}[/tex]

Now I know that I should apply [itex](\dagger)[/itex] but I don't know how to given the antisymmetrisation brackets. Would someone mind explaining it to me please? Thank you!
 
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  • #2
Ok let's take it slow because you messed up in one of the steps. This is a bit messy (but not much). So we start off with ##d(*\alpha)_{c b_1...b_{n-p}} = (n - p + 1)\nabla_{[c}*\alpha_{b_1...b_{n-p}]}## hence ##*d(*\alpha)_{a_1...a_{p-1}} = \frac{n - p + 1}{(n-p + 1)!}\epsilon_{d_1...d_{n-p + 1}a_1...a_{p-1}}\nabla^{[d_1}*\alpha^{d_2...d_{n-p+1}]}##. Before proceeding, notice that ##\nabla^{[d_1}*\alpha^{d_2...d_{n-p+1}]} = \delta^{[d_1}_{e_1}...\delta^{d_{n-p +1}]}_{e_{{n-p+1}}}\nabla^{e_1}*\alpha^{e_2...e_{n-p+1}} =\\ \frac{1}{(p - 1)!(n - p +1)!}\epsilon^{f_1...f_{p-1}d_1...d_{n-p + 1}}\epsilon_{f_1...f_{p-1}e_{1}...e_{n-p+1}}\nabla^{e_1}*\alpha^{e_2...e_{n-p+1}}##

Now ##\epsilon^{f_1...f_{p-1}d_1...d_{n-p + 1}}\epsilon_{d_1...d_{n-p + 1}a_{1}...a_{p-1}} = (-1)^{(p-1)(n - p + 1)}(p - 1)!(n - p + 1)!\delta^{[f_1}_{a_1}...\delta^{f_{p-1}]}_{a_{p-1}}##
(the ##(-1)^{(p-1)(n - p + 1)}## comes from rearranging the indices on ##\epsilon^{f_1...f_{p-1}d_1...d_{n-p + 1}}## so that it takes the right form)
so ##*d(*\alpha)_{a_1...a_{p-1}} = \frac{(n - p + 1)(-1)^{(p -1)(n - p + 1)}}{(n - p +1)!}\epsilon_{a_1...a_{p-1}e_{1}...e_{n-p+1}}\nabla^{e_1}*\alpha^{e_2...e_{n-p+1}}##. Take it from there.
 
  • #3
Just to be on the safe side, let me know if you need more help and/or if the above isn't clear enough (thankfully there is very little you have to do beyond what I posted above). Also, I didn't mention this before because it isn't really important but for a Lorentzian space-time manifold, the relation you gave involving the orientation of the space-time has an overall negative sign. Finally, keep in mind that ##\nabla_{b}\epsilon_{a_1...a_n} = 0##.
 
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  • #4
I've been following this thread because I'm interested in the solution, but sadly the OP never came back. Can somebody give it anyway?
 
  • #5
Sure, there's very little to do beyond what was in post #2 anyways. So we left off at ##*d(*\alpha)_{a_1...a_{p-1}} = \frac{(n - p + 1)(-1)^{(p -1)(n - p + 1)}}{(n - p +1)!}\epsilon_{a_1...a_{p-1}e_{1}...e_{n-p+1}}\nabla^{e_1}*\alpha^{e_2...e_{n-p+1}}##.

Now ##(-1)^{(p -1)(n - p + 1)}\epsilon_{a_1...a_{p-1}e_{1}...e_{n-p+1}}\nabla^{e_1}*\alpha^{e_2...e_{n-p+1}} \\ = \frac{(-1)^{p(n - p)}}{p!}\epsilon_{e_2...e_{n-p+1}a_1...a_{p-1}e_{1}}\epsilon^{e_2...e_{n-p + 1}d_1...d_p }\nabla^{e_1}\alpha_{d_1...d_p} \\ =(-1)^{p(n - p)}(n - p)! \nabla^{e_1}\alpha_{[a_1...a_{p-1}e_1]} ##

hence ##*d(*\alpha)_{a_1...a_{p-1}} = \frac{(-1)^{p(n - p)}(n - p + 1)(n - p)!}{(n - p + 1)!} \nabla^{e_1}\alpha_{[a_1...a_{p-1}e_1]} = (-1)^{p(n - p)}\nabla^{e_1}\alpha_{a_1...a_{p-1}e_1} ##
where ##\alpha_{[a_1...a_{p-1}e_1]} = \alpha_{a_1...a_{p-1}e_1}## by definition of a differential form. Thus we have the desired result.
 

FAQ: How Do General Relativity Tensors and Their Indices Work?

1. What are tensors in general relativity?

Tensors in general relativity are mathematical objects that are used to describe the curvature of spacetime. They are used to represent physical quantities such as energy, momentum, and stress, and they allow us to make precise calculations and predictions about the behavior of matter and space in the presence of gravitational fields.

2. How are tensors used in general relativity?

In general relativity, tensors are used to describe the curvature of spacetime caused by the presence of matter and energy. They are also used to calculate how matter and radiation move in this curved spacetime. Tensors are an essential tool in understanding and predicting the behavior of the universe on a large scale.

3. What are the different types of tensors in general relativity?

There are several types of tensors used in general relativity, including the metric tensor, the stress-energy tensor, and the Ricci tensor. The metric tensor is used to describe the geometry of spacetime, while the stress-energy tensor represents the distribution of energy and momentum in spacetime. The Ricci tensor is used to calculate the curvature of spacetime.

4. How do tensors relate to Einstein's theory of general relativity?

Tensors play a crucial role in Einstein's theory of general relativity. In this theory, the curvature of spacetime is described by the Einstein field equations, which are based on the use of tensors. These equations relate the curvature of spacetime to the distribution of matter and energy, allowing us to understand how gravity works on a large scale.

5. Are tensors difficult to understand?

Tensors may seem complex and intimidating at first, but with some basic understanding of linear algebra and differential geometry, they can be grasped and applied effectively. It is important to have a solid understanding of the concepts and notation used in general relativity to fully comprehend the role of tensors in this theory.

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