Abstract
In the previous chapters we have introduced a possible generalization of the space–time geometry based on the model of Riemann manifold.
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Notes
- 1.
R.V. Pound and G.A. Rebka, Phys. Rev. Lett. 4, 337 (1960).
- 2.
J. Hafele and R. Keating, Science 177, 166 (1972).
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Appendices
Exercises Chap. 5
5.1
Time-Dependent Spectral Shift A photon propagates along the (light-like) geodesics associated to the following line-element:
which describes a space–time with a time-dependent geometry. The photon is emitted at a time \(t_e\) and received at a time \(t_r\). Compute the frequency shift of the received photon with respect to the emitted one in terms of the geometric parameter a(t).
5.2
Hyperbolic Geodesic Motion Determine the time-like geodesic trajectories associated to a motion along the x axes, in the space–time manifold parametrized by the coordinates \(x^0=ct\), \(x^i=(x,y,z)\), and described by the following line-element:
where \(t_0\) is a constant.
Solutions
5.1
Solution In order to evaluate the frequency shift experienced by the photon along its geodesic path we shall use the condition of parallel transport of the four-momentum vector, given by Eq. (5.9).
We recall, first of all, that in the Minkowski space–time a photon of frequency \(\omega \) is characterized by an energy \(\mathcal{E}= \hbar \omega \) and a momentum \(p^i= (\hbar \omega /c) n^i\), where \(n^i\) is the unit vector pointing to the propagation direction. In the space–time described by the line-element (5.43) the four-momentum \(p^\mu \) of the photon has then the following components:
The factor \(a^{-1}\) appearing in the spatial part of the vector is prescribed by the minimal coupling principle, in order to satisfy the covariant version of the null normalization condition:
The non-vanishing components of the connection associated to the metric (5.43) are given by:
(we have used the definition (3.90)). By applying the geodesic equation (5.9) we then obtain
Let us now recall that a light-like geodesic is characterized by a null space–time interval, \(dx_\mu dx^\mu = ds^2=0\). A photon propagating along the spatial direction \(n^i\), across a space–time geometry specified by Eq. (5.43), must then follow a trajectory which satisfies the differential condition
Inserting this result into Eq. (5.48), using \(\delta _{ij}n^in^j=1\), and dividing by \(\hbar /c\), we obtain:
The integration of this equation immediately gives the time dependence of \(\omega \) as a function of the time dependence of the geometric parameter a(t):
where \(\omega _0\) is an integration constant, representing the corresponding frequency in the Minkowski space–time (where \(a=1\)). The spectral shift between the emitted frequency \(\omega _e\equiv \omega (t_e)\) and the received frequency \(\omega _r\equiv \omega (t_r)\) is then fixed by the ratio:
It may be noted, finally, that if \(a(t_r)>a(t_e)\) then we obtain \(\omega _r<\omega _e\), namely the received frequency is red-shifted with respect to the emitted one. This is a typical effect of the cosmological gravitational field which permeates our Universe on very large scales of distance, and which can be indeed described (in first approximation) by a geometry of the type (5.43) (see e.g. the books [12, 19, 24] quoted in the bibliography).
5.2
Solution The geometry of the manifold (5.44) is described by the metric
and the non-zero components of the associated connection (defined by Eq. (3.90)) are given by:
Let us explicitly write down the components of the geodesic equation (5.7), by setting \(x^0=ct\) and recalling that the dot denotes differentiation with respect to the parameter \(\tau \), which we can identify with the proper time along the particle trajectory:
We are considering, in particular, a one-dimensional motion along the x axes. Equation (5.56) can thus be easily integrated, and gives
where \(\alpha \) is an integration constant with the dimensions of an acceleration (the parameter \(t_0\) has been inserted for further convenience). Instead of integrating also Eq. (5.55) we now observe that a time-like geodesic must satisfy the normalization condition
which, combined with Eq. (5.59), gives
Combining this result with Eq. (5.59) we can eliminate the proper-time variable \(\tau \) (in terms of t), to obtain
Another simple integration finally gives us the equation of the trajectory,
where \(x_0\) is an integration constant depending on the initial conditions. Note that this solution also automatically satisfies Eq. (5.55), as can be explicitly checked by differentiating with respect to \(\tau \).
The above trajectory can be geometrically interpreted by squaring \(x -x_0\), and moving ct to the left-hand side:
In the plane (x, ct) this is an hyperbola with center at the point of coordinates \(x=x_0\) and \(t=0\), and asymptotes given by the light-cone \(x= x_0 \pm ct\). The time-like geodesics of the given geometry thus exactly reproduce the trajectories of a uniformly accelerated motion in Minkowski space, characterized by a four-acceleration vector with constant modulus \(a_\mu a^\mu = \alpha ^2\).
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Gasperini, M. (2017). Test Bodies and Signals in a Riemann Space–Time. In: Theory of Gravitational Interactions. UNITEXT for Physics. Springer, Cham. https://doi.org/10.1007/978-3-319-49682-5_5
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