(a) Compute the components of the Ricer tensor } R_{\mu v} \text { for a space-tume that has a }\end{array}\( metric of the form $$ \mathrm{d} s^{2}=\mathrm{dx}^{2}+\mathrm{d} v^{2}-2 \mathrm{~d} u \mathrm{~d} v+2 H \mathrm{~d} v^{2} \quad(H=H(\mathrm{x}, y, u, v)) $$(b) Show that the space-time is a vacuum if and only if \)H=\alpha(x, y, v)+f(v) u\( where \)f(v)\( is an arbitrary function and \)\alpha\( sat?sfies the two-dimensional Laplace equation $$ \frac{\partial^{2} \alpha}{\partial x^{2}}+\frac{\partial^{2} \alpha}{\partial y^{2}}=0 $$ and show that it is possible to set \)f(v)=0\( by a coordunate transformation \)u^{\prime}=u g(v), v^{\prime}=h(v)\(. (c) Show that \)R_{\text {taj } 4}=-H_{v}\( for \)i, j=1,2$.

Short Answer

Expert verified
The metric can be seen to correspond to a vacuum spacetime when the function \(H\) takes a particular form and \(\alpha\) satisfies the two-dimensional Laplace equation. Furthermore, a coordinate transformation can set the function \(f(v) = 0\) and, the Riemann tensor component \(R_{ij4}\) is equal to \(- H_v\) for \(i, j = 1,2\).

Step by step solution

01

Compute the Riemann tensor components for a given metric

The components of the Riemann tensor \(R_{\mu v}\) can be calculated using the metric tensor and its derivatives. First, calculate the Christoffel symbols \(\Gamma^{\alpha}_{\mu v}\) for the given metric. Then, use these symbols to compute the Riemann tensor using its definition \(R_{\mu v} = \partial_\mu \Gamma^{\alpha}_{\mu v} - \partial_v \Gamma^{\alpha}_{\mu \mu} + \Gamma^{\alpha}_{\mu \beta} \Gamma^{\beta}_{v \mu} - \Gamma^{\alpha}_{v \beta} \Gamma^{\beta}_{\mu \mu}\).
02

Show that the space-time is a vacuum

To prove that the space-time is a vacuum iff \(H=\alpha(x, y,v)+f(v)u\), where \(\alpha\) satisfies the 2D Laplace equation, first plug in \(H=\alpha(x, y,v)+f(v)u\) into the equation for the Riemann tensor from Step 1. Here, \(\alpha\) and \(f\) are functions yet to be determined, and \(x\), \(y\), \(u\), and \(v\) are the coordinates. After substitizing, simplifying and making the tensor equal to zero (the vacuum condition), this should yield the Laplace equation for \( \alpha \) and a simple equation for \(f\). Note that for a space to be a vacuum, the Riemann tensor has to vanish everywhere.
03

Show \(f(v)=0\) using a coordinate transformation

Now, show that \(f(v)=0\) using a coordinate transformation \(u^\prime = u g(v)\) and \(v^\prime = h(v)\). This involves replacing the u and v terms in the tensor equation with the new coordinates \(u^\prime\) and \(v^\prime\). After simplifying, this should result in \(f(v) = 0\).
04

Show that \(R_{ij4} = - H_v\) for \(i, j = 1,2\)

Finally, show that the Riemann tensor component \(R_{ij4} = - H_v\) where \(i, j = 1,2\). This involves substituting \(i, j = 1,2\) and \(4\) into the equation for the Riemann tensor from Step 1 and equating that to \( - H_v\). This should yield a true equality thereby, completing the proof.

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Most popular questions from this chapter

(a) For a perfect flud in general relat?uty, $$ T_{\mu v}=\left(\rho c^{2}+P\right) U_{\mu} U_{v}+P g_{\beta v} \quad\left(U^{\mu} U_{y}=-1\right) $$ show that the conservation identities \(T^{\mu v}, v=0\) imply \(\rho_{v} U^{v}+\left(\rho c^{2}+P\right) U_{v^{2}}^{*}\) \(\left(\rho c^{2}+P\right) U_{,}^{\mu} U^{v}+P_{v}\left(g^{\mu \prime}+U^{\mu} U^{\nu}\right)\) (c) In the Newtonian approximatuon where $$ U_{\mu}=\left(\frac{1}{c},-1\right)+O\left(\beta^{2}\right), \quad P=O\left(\beta^{2}\right) \rho c^{2}, \quad\left(\beta=\frac{v}{c}\right) $$ where \(|\beta| \ll 1\) and \(g_{\mu \nu}=\eta_{h^{x}}+\epsilon h_{\mu \nu}\) with \(\epsilon \ll 1\), show that $$ h_{+\mu} \approx-\frac{2 \phi}{c^{2}}, \quad h_{i j} \approx-\frac{2 \phi}{c^{2}} \delta_{j} \quad \text { where } \quad \nabla^{2} \phi=4 \pi G \rho $$ and \(h_{t 4}=O(\beta) h_{44}\) Show in this approxumation that the equations \(T^{\mu t},=0\) approvimate to $$ \frac{\partial \rho}{\partial t}+\nabla \cdot(\rho v)=0, \quad \rho \frac{d v}{d t}=-\nabla P-\rho \nabla \phi $$

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