Time Travel Research Center © 1998 Cetin BAL  GSM:+90 05366063183  Turkey / Denizli General Relativity:Note: The Feynman Lectures covers
most of the material from this lecture. I'm just adding a bit extra information
and a couple of comments... Einstein's General Theory of Relativity can be summed up in two key concepts:
. General Relativity represents a new view of particle motion, different in character than Newton's Laws:
General Relativity is all about (nonEuclidean) geometry. Aside  Geometry in Terms of "Intervals:"
Aside: Why the Minus Sign?
Aside  Why the Differentials?
Experimental Proof for GR:The book discusses several observations which support General Relativity. These are the “classic” experiments. However, I'd like to add my own two cents' worth... Gravitational Radiation:From classical electromagnetism, you know that an oscillating electric charge produces electromagnetic radiation (light!):
In the same way, the theory of General Relativity predicts that a timevarying distribution of mass should produce gravitational radiation  gravity waves. It would be very exciting to observe gravitational radiation. The problem is that gravity is so much weaker than electromagnetism  recall that even a tiny charge imbalance on, say, an electroscope or your socks when they come out of the dryer can counteract the force of gravity.
Nonetheless, there is some indirect proof of the existence of gravitational radiation. In 1974, Hulse and Taylor (Nobel, 1993) discovered a binary pulsar. A pulsar is a periodic stellar source of radio radiation  it is believed that a pulsar is a rotating neutron star, which channels charged particles out along magnetic field lines. As these particles move and accelerate in the magnetic field, they emit intense radiation  preferentially along the directions of the magnetic field lines. In a neutron star, these field lines are concentrated at the poles of the star  if the magnetic pole is offaxis (similar to the way the Earth's magnetic North pole does not lie on the “real” North pole), then as the star rotates, the magnetic field precesses about the rotational axis. From the point of view of observers on the Earth, the beam of radiation sweeps by us once every rotation  rather like the beam of light from a lighthouse (see Sec. 15.7 of the book). In any case, a pulsar is a periodic source of detectable radiation. In the case of the binary pulsar, the usual “searchlight” periodicity is modulated  the repitition rate of the observed beam first increases, then decreases. This is due to the Doppler effect as the pulsar orbits its companion star in the binary star system. What Hulse and Taylor noticed was that the period of this orbit was decreasing with time! This can be explained by the gravitational radiation which must be emitted by the system as the two objects orbit each other. As they radiate gravity waves, the energy of the system decreases. This means the radius of the orbit and its period decrease. When one calculates the expected change in period using General Relativity, the agreement is phenomenal! So the binary pulsar provides indirect evidence for the existence of gravity waves. It would be satisfying, however, to directly observe gravitational radiation, similar to the way we observe electromagnetic radiation. As I mentioned above, this is difficult because gravity is so much weaker than electromagnetism. It is also difficult because the period of gravity waves is given by the oscillation frequency of the source, and for the astronomical sources which would radiate enough gravitational radiation for us to observe, the orbital periods are relatively long (on the order of Hertz to hundreds of Hertz). It is very difficult to eliminate extraneous noise at these frequencies (noise generically decreases with increasing frequencies  note to budding experimentalists: perform your measurements at the highest frequency you can!). Nonetheless, there are gravitational wave observatories currently taking data or being commissioned. These include VIRGO (France/Italy), GEO 600. (Germany/Great Britain), TAMA 300 (Japan), ACIGA (Australia), and LIGO (US). By way of example, LIGO is a very large Michelson interferometer (what else!).
Each arm of the interferometer contains a resonant cavity. The mirrors of these cavities serve as reference masses  a passing gravity wave will warp spacetime in the vicinity of the interferometer, shortening one arm and lengthening the other. The effect is not large, but LIGO should be able to detect it, nonetheless. To give you some idea of the sensitivity required, each of LIGO's arms is 4 km long, but the instrument can sense changes in arm length of on the order of the diameter of an atomic nucleus! LIGO is just beginning to take data... Gravitational Lensing:Warped spacetime causes even light to deflect from what we would normally consider a geometric straight line. The deflection of starlight by the Sun, first observed during the 1919 solar eclipse, was the dramatic first experimental confirmation of the theory of General Relativity. In such effects, concentrations of mass serve as “lenses” to redirect the path of light. If a star lies behind a massive object, then rays of light which normally would not reach our eyes can be redirected towards us, allowing us to observe the normally obscured objetct:
Of course, the real situation can be much more complex  if the star isn't directly behind the lensing object, the image of the star can suffer various distortions. With the power of modern telescopes and observational techniques, gravitational lenses are routinely observed. See, for example, Pete Newbury's web site at UBC (click on “Examples.”). I pulled the following picture from the online archives of Hubble Space Telescope's pictures:
Black Holes:The book discusses black holes in Sec. 15.8. Laplace, reasoning only using Newtonian gravity, posited the possible existence of an object whose escape velocity exceeded the speed of light. However, what we normally think of when we hear the phrase “black hole” is the offspring of General Relativity. Einstein wrote down his differential equations for General Relativity, but he didn't find any solutions to the equations! The first person to do so was Karl Schwarzschild, in 1916. He worked out the solution and wrote it up while serving in the German army on the Russian Front! (Unfortunately for us all, he became ill whilst on the Front, and died soon thereafter...) I'll write out his solution to the Einstein field equations just so that you can see what a result in General Relativity looks like (to remind you, the math  which involves differential geometry  can get pretty heinous pretty quickly). The solution gives the spacetime interval in sphericalpolar coordinates in the presence of a spherically symmetric, nonrotating mass distribution as: . One can then use this quantity to calculate other physical observables. For instance, if is the time between two events as measured by someone a distance r from the centre of the massive object, then an observer at a point P very far from the massive object would measure a time interval of
between the same two events. Notice what happens to the spacetime interval and to as , known as the Schwarzchild radius. A divergence occurs! This divergence leads to the many bizarre effects of black holes. But note (as the book does on pg. 512) that this is a very “gentle” divergence. Nothing spectacular happens as an object passes the event horizon at r_{S}. However, from the point of view of outside observers, the object appears frozen in time. From the point of view of the object, the rest of the universe blinks by in an instant! If you haven't already, have a cruise through the event horizon at Andrew Hamilton's home page You can see a catalogue of possible black holes at the Hubble Space Telescope home page. A “Teaser”  the “Alcubierre Warp Drive:”So nothing can travel faster than the speed of light in a vacuum. This is a fundamental principle of modern physics, and it is correct. However, if one phrases it more accurately, “nothing can travel faster than the local speed of light in a vacuum.” Note the word local  what that means is that it is not inconsistent with the equations of General Relativity for an object at one point in space to move faster than the speed of light elsewhere, as long as it doesn't move faster than the speed of light where it is. Note that I said “not inconsistent!” Just because something is “allowed” by General Relativity, doesn't mean that it necessarily is possible, or even that it is consistent with the rest of physics! Keeping that caveat in mind, however, let me share a cool theoretical result from 1994 with you  just to give you some idea of the fun you can have with GR if you're willing to wade through the differential geometry. In 1994, Miguel Alcubierre found the following solutions to the Einstein field equations:
where , , and f(r) goes to zero for large r. Given these properties, ds becomes the usual spacetime interval of Special Relativity (flat spacetime) for large r. This spacetime interval describes a localized region of spacetime which moves with velocity v. This velocity v may be arbitrarily large (i.e. v > c is allowed)! Also, time flows at the same rate inside the spacetime “bubble” as it does outside, so that no relativistic timedilation is experienced between observers inside/outside the bubble.
So this solution looks like a possible “warp drive!” However, it is unclear whether it is possible to actually create such a region of spacetime. The spacetime it describes has a very particular curvature, which requires a very particular distribution of mass/energy. Indeed, it has been proven that the only way to obtain the required curvature is if one can create regions of negative mass/energy density! While it is true that negative mass/energy can occur for short periods of time on very small length scales (this is a result from quantum field theory), it seems unlikely at present that one could find a way to realize such a beast on a macroscopic and nontransitory scale. The “Alcubierre warp drive” also raises the threat of strange causality paradoxes. But it's a tantalizing thought...
Next time: We start in on quantum mechanics!
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