Difference between revisions of "Schwarzschild black hole"
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=== Problem 2. === | === Problem 2. === | ||
− | + | What is the physical distance between two points with coordinates $(r_{1},\theta,\varphi)$ and $(r_{2},\theta,\varphi)$? Between $(r,\theta,\varphi_{1})$ and $(r,\theta,\varphi_{2})$? How do these distances behave in the limit $r_{1},r\to r_{g}$? | |
<div class="NavFrame collapsed"> | <div class="NavFrame collapsed"> | ||
<div class="NavHead">solution</div> | <div class="NavHead">solution</div> | ||
<div style="width:100%;" class="NavContent"> | <div style="width:100%;" class="NavContent"> | ||
<p style="text-align: left;"> | <p style="text-align: left;"> | ||
− | + | \[l_{r1-r2}=\int\limits_{r_1}^{r_2} | |
+ | \frac{dr}{\sqrt{1-\frac{r_g}{r}}};\quad | ||
+ | l_{\varphi1-\varphi_2}=2\pi r|\varphi_1-\varphi_2|; | ||
+ | \quad | ||
+ | l_{\theta1-\theta_2}=2\pi r|\theta_1-\theta_2|.\] </p> | ||
</div> | </div> | ||
</div> | </div> | ||
<div id="BlackHole17"></div> | <div id="BlackHole17"></div> | ||
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=== Problem 3. === | === Problem 3. === | ||
problem formulation | problem formulation |
Revision as of 15:14, 17 June 2012
The spherically symmetric solution of Einstein's equations in vacuum for the spacetime metric has the form \cite{Schw} \begin{align}\label{Schw} ds^{2}=h(r)\,dt^2-h^{-1}(r)\,dr^2-r^2 d\Omega^{2}, &\qquad\mbox{where}\quad h(r)=1-\frac{r_g}{r};\quad r_{g}=\frac{2GM}{c^{2}};\\ d\Omega^{2}=d\theta^{2}+\sin^{2}\theta\, d\varphi^{2}&\;\text{-- metric of unit sphere.}\nonumber \end{align} The Birkhoff's theorem (1923) \cite{Birkhoff,Jebsen} states, that this solution is unique up to coordinate transformations. The quantity $r_g$ is called the Schwarzschild radius, or gravitational radius, $M$ is the mass of the central body or black hole.
Contents
Simple problems
Problem 1.
Find the interval of local time (proper time of stationary observer) at a point $(r,\theta,\varphi)$ in terms of coordinate time $t$, and show that $t$ is the proper time of an observer at infinity. What happens when $r\to r_{g}$?
The proper time of the stationary observer is $d\tau=ds|_{dr=d\theta=d\varphi=0}$: \[d\tau=\sqrt{g_{00}}dt=\sqrt{1-\frac{r_{g}}{r}}dt.\] At $r\to \infty$ it coincides with $dt$, so the coordinate time $t$ can be interpreted as the proper time of a "remote" observer. At $r\to r_g$ the local time flows slower and asymptotically stops. If one of two twins were to live some time at $r\approx r_g$, he will return to his remote twin having aged less (thought he might have acquired some grey hair due to constant fear of tumbling over the horizon).
Problem 2.
What is the physical distance between two points with coordinates $(r_{1},\theta,\varphi)$ and $(r_{2},\theta,\varphi)$? Between $(r,\theta,\varphi_{1})$ and $(r,\theta,\varphi_{2})$? How do these distances behave in the limit $r_{1},r\to r_{g}$?
\[l_{r1-r2}=\int\limits_{r_1}^{r_2} \frac{dr}{\sqrt{1-\frac{r_g}{r}}};\quad l_{\varphi1-\varphi_2}=2\pi r|\varphi_1-\varphi_2|; \quad l_{\theta1-\theta_2}=2\pi r|\theta_1-\theta_2|.\]
Problem 3.
problem formulation
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Problem 4.
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Problem 5.
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Symmetries and integrals of motion
Problem 6.
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Problem 7.
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Problem 8.
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Problem 9.
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Problem 10.
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Problem 11.
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Problem 12.
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Radial motion
Consider a particle's radial motion: $\dot{\varphi}=\dot{\theta}=0$. In this problem one is especially interested in asymptotes of all functions as $r\to r_{g}$.
Problem 13.
problem formulation
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Problem 14.
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Problem 15.
problem formulation
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Problem 16.
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Problem 17.
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Blackness of black holes
A source radiates photons of frequency $\omega_i$, its radial coordinate at the time of emission is $r=r_{em}$. Find the frequency of photons registered by a detector situated at $r=r_{det}$ on the same radial line in different situations described below. By stationary observers here, we mean stationary in the static Schwarzschild metric; "radius" is the radial coordinate $r$.
Problem 18.
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Problem 19.
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Problem 20.
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Problem 21.
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Orbital motion, effective potential
Due to high symmetry of the Schwarzschild metric, a particle's worldline is completely determined by the normalizing condition $u^{\mu}u_{\mu}=\epsilon$, where $\epsilon=1$ for a massive particle and $\epsilon=0$ for a massless one, plus two conservation laws---of energy and angular momentum.
Problem 22.
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Problem 23.
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Problem 24.
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Problem 25.
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Problem 26.
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Miscellaneous problems
Problem 27.
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Problem 28.
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Problem 29.
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Problem 30.
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Solving Einstein's equations for a spherically symmetric metric of general form in vacuum (energy-momentum tensor equals to zero), one can reduce the metric to \[ds^2=f(t)\Big(1-\frac{C}{r}\Big)dt^2 -\Big(1-\frac{C}{r}\Big)^{-1}dr^2-r^2 d\Omega^2,\] where $C$ is some integration constant, and $f(t)$ an arbitrary function of time $t$.
Problem 31.
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Problem 32.
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Problem 33.
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Different coordinates, maximal extension
We saw that a particle's proper time of reaching the singularity is finite. However, the Schwarzschild metric has a (removable) coordinate singularity at $r=r_{g}$. In order to eliminate it and analyze the casual structure of the full solution, it is convenient to use other coordinate frames. Everywhere below we transform the coordinates $r$ and $t$, while leaving the angular part unchanged.
Problem 34.
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Problem 35.
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Problem 36.
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Problem 37.
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Problem 38.
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Problem 39.
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