George Jones said:
...
clock A is thrown straight up from the surface and returns to the surface;
clock B is dropped from rest through a tunnel that goes through the centre of the planet;
Clock C remains on the surface;
clock D remains at the centre of the planet;
clock E orbits the body right at the surface.
Assume A is thrown up as E passes C so that A returns to C at the same time as E returns.
These are the results of some calculations I have done for the proper times of the clocks where R is the Radius of the planet and H is the Height that clock A reaches at its apogee when thrown upwards. F is the coordinate time according to a clock at infinity. I have not calculated the proper time for clock B oscillating inside the tunnel as that will require a real expert to figure out ;)
\begin{tabular}{l l l l l l l}<br />
R : 2.13m & 2.80m & 3.21m & 4.93m & 45.23m & 448.85m & 44,847.79m\\<br />
H : 3m & 5m & 6m &10m & 100m & 1,000m & 100,000m\\<br />
\hline<br />
A : 7.52 & 19.32 & 25.95 & 57.79 & 1882.18 & 59658.94 & 59673959.04<br />
\\<br />
C : 4.81 & 15.71 & 22.11 & 53.07 & 1868.45 & 59615.90 & 59673528.99<br />
\\<br />
D : -2.52 & 8.87 & 12.82 & 45.19 & 1847.07 & 59549.27 & 59672863.68<br />
\\<br />
E : (12.48) & (7.90) & 9.13 & 43.08 & 1846.72 & 59549.16 & 59672863.67<br />
\\<br />
F : 19.52 & 29.41 & 36.06 & 68.83 & 1911.19 & 59749.16 & 59674859.61\\<br />
\end{tabular}
Note that tossed clock A consistently records the longest proper time period than any of the other clocks, (except for the coordinate clock at infinity of course.) Orbiting clock E consistently records the least proper time. (The figures in brackets for clock E should not be compared as they are virtual periods because there are no real circular orbits at radii less than the photon orbit radius at 3m.). Centre clock D always records less proper time than stationary clock C at the surface as would be expected but it is somewhat surprising to me that also generally records more proper time than orbiting clock E. The proper time for clock D is calculated using the interior Schwarzschild solution. Generally the interior solution requires knowledge of the density distribution of the mass of the planet but in the case of a stationary clock exactly at the centre, the enclosed mass is zero and the density distribution becomes irrelevant.
The next table compares the coordinate spatial distances for the paths of the various clocks. Clocks C, D and F have not been included as they are always stationary.
\begin{tabular}{l l l l l l l}<br />
R : 2.13m & 2.80m & 3.21m & 4.93m & 45.23m & 448.85m & 44,847.79m\\<br />
H : 3m & 5m & 6m &10m & 100m & 1,000m & 100,000m\\<br />
\hline<br />
A : 1.74 & 4.40 & 5.59 & 10.14 & 109.54 & 1102.30 & 110304.42\\<br />
B : 8.52 &11.19 & 12.82 & 19.73 & 180.92 & 1795.40 & 179391.15\\<br />
E : 13.38 & 17.58 & 20.14 & 30.99 & 284.18 & 2820.21 & 281786.96\\<br />
\end{tabular}
Now it can be seen that clock A not only consistently has the greatest proper time but it also has the shortest spatial path distance and orbiting clock E that always has the least proper time also always has the longest path distance.
The geodesics of clocks A and E are the only ones that are directly comparable as they are the only geodesics that pass directly through the same point C. The clock at C is not on a geodesic as it is not inertial. The path of clock B is a geodesic that passes through point C but it remains to be determined what its proper time period is and whether there is a density distribution that allows it to return to point C at an interval that coincides with clocks A and E. An experiment could be set up to send clock A up to an altitude such that it returns to point C at the same time as clock B and clock E could be sent on an approximately elliptical orbit that has its short axis of the same length of the tunnel, but the maths would be very complicated and the fact that orbit of clock E would be precessing would add further complication.
Note: The negative proper time for clock D when R=2.13 is not a typo. The proper time of a clock at the centre of a gravitational mass is negative always negative for radii less than 2.25m or less than \frac{9}{8} R_{s}