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Figure 2: Difference $\mathrm{\Delta }r(t)$ between the radial distances obtained from the solutions of two numerical integrations with MATHEMATICA of the equations of motion over 3 years with and without $\dot{\mu }/\mu$; the initial conditions are the same. Just for illustrative purposes a mass loss rate of the order of $-10^{-1}$ yr${}^{-1}$ has been adopted for the Sun; for the planet initial conditions corresponding to $a=1$ AU, $e=0.01$ have been chosen. The cumulative increase of the Sun-planet distance induced by the mass loss is apparent.