General Relativity Physics Honours 2005

General RelativityPhysics Honours 2005

Dr Geraint F. LewisRm 557, A29

[email protected]

http://www.physics.usyd.edu.au/~gfl/

Lecture

Spin (a quick look)In flat space-time, the axis of spin of a gyroscope is a constant. If the spin is represented by a 4-vector of the form sa = (0,s) then this implies an equation of motion of

In non-flat space-time, we can generalize this expression to

In the local inertial frame u.s=0 (in general, this is something that holds in all frames).


Lecture

Geodetic PrecessionA gyroscope in classical physics retains its orientation wrt to distant stars as it orbits a massive body. What about GR?

Again, we consider an equatorial orbit ( =/2). The only spatial part of the 4-velocity is

For circular orbits, = m/r3, and the 4-velocity is

(check u.u=1)


Lecture

Geodetic Precession

and inserting the expression for u then (algebra….)


Lecture

Geodetic PrecessionThe geodetic precession per orbit is

For the Earth, this is ~8.4”/yr. While this is small, this should be measurable by Gravity Probe B.

With a rotating metric, there are additional precession effects.


Lecture

Gravitational WavesSo far, the solutions to the field equations we have examined are static, making problems easier to solve.

In reality, space-time should be dynamics, evolving as the distribution of matter/energy changes. Space-time can even be made to “wave” due to asymmetries in collapse or explosions (think of the electromagnetic waves produced as charges are accelerated).

Large disturbances are difficult to calculate, requiring numerical computation of the evolving field equations.


Lecture

Wave hitting a Black Hole

Harald Pfeiffer


Lecture

Gravitational WavesSmall disturbances can be tackled analytically, revealing waves traveling at the speed of light. To do this, we need to employ the linearized field equations

where is a small, dimensionless parameter and hab!0 as r!0.

Defining (ignoring higher order terms) then


Lecture

Gravitational WavesHence we can calculate the Christoffel symbols

and the Riemann tensor is given by

This satisfies the Bianchi identities Rab[cd,e] = 0


Lecture

Gravitational WavesFurthermore, the Ricci tensor and curvature scalar are

where cdhcd=hcc=h and the d’Alembertian is =abab

The resulting Einstein tensor is given by


Lecture

Gauge TransformationsAs in EM, we can make a gauge transformation without changing the predictions of the theory. As GR does not prefer any particular coordinate system, we are free to make a coordinate transformation

We can use this to transform gab (and hence hab) to the new coordinates and find


Lecture

Gauge TransformationsCalculating the curvature tensor and its contractions in the new coordinate system reveals that they are identical to those in the old coordinate system i.e. we have a gauge invariance.

Given this, we can chose an appropriate coordinate system to simplify the linearized field equations. Introducing a new variable

then


Lecture

Gauge TransformationsWe can impose the gauge condition that

results in a wave equation of the form

Hence the small perturbations on an otherwise flat metric can propagate as waves (See Hartle’s comparison of GR and EM on page 462 of his book).


Lecture

Plane Gravitational WavesIf we assume

substantial algebra (see textbook) reveals we can choose coordinates such that

and the perturbation depends only on two independent functions.


Lecture

Polarization StatesIf h23=0, the line element becomes

the wave travels in the x-direction. For h22>0 then distances in the y-direction are decreased and those in the z-direction are increased.If h22=0, the line element becomes

this is a rotation through 45o of the case where h23=0.


Lecture

Polarization States

Hence there are two polarization states, h+ and hx at 45o to one another. This is different from the EM case where polarization states are at 90o. This is because EM is represented by a vector potential (Aa, spin 1) whereas gravity is represented by a second rank tensor (hab, spin 2).


Lecture

Detecting Gravitational WavesGravitational waves should be formed in asymmetric core collapse supernova, or neutron star and black hole collisions.

The expected waves would have h~10-19 (or much less). Detecting these waves has a long history and in the 1960s Weber looked at the deformation of a large cylinder of aluminium although his results were inconclusive. More sensitive laser interferometers have been established, but to date, no waves have been seen!


Lecture

Pulsar Orbital DecayIndirect evidence for gravitational radiation comes from binary pulsar PSR1913+16 whose orbit is decreasing as energy is carried away by gravitational waves. The quadrupole luminosity is

where M is the mass of the stars in circular orbit, lo is their separation and is their angular velocity (monopole and dipole radiation are forbidden due to spin 2 nature). The change in the period of the orbit is


Lecture

Nobels & PulsarsTaylor & Hulse won the 1993 Nobel prize for their measurement of the orbital decay of PSR1913. Energy is radiated away in the form of gravitational waves.


Lecture

Do Waves Carry Energy?Remember, we have solved the equation

Where is the energy in the equation? Energy is used to form waves, and energy can be deposited by waves, but there is no localized energy identifiable in the waves.

(The entire question of energy conservation in GR is a big one which does not appear close to being solved).

General Relativity Physics Honours 2005

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