\delta {\bf F} \vert
\simeq 2.92 \times 10^{-4}$ mm$/$s$^2$, which it is very small in comparison perturbing accelerations we have found in the previous section. However, a disregarded zonal coefficient with order $J_n \simeq 10^{-4}$ could explain the anomalies in the integration of our model. So, further research into the structure of Jupiter is necessary and this can be achieved in future analysis of the data provided by the Juno mission. Anyway, it seems unlikely that zonal coefficients of order eight and higher could be so large. As it happens in the case of the Earth, we expect that these coefficients would diminish with the order and from Eq. (\[Jcoeff\]) an upper bound $J_8 < 10^{-5}$ seems reasonable for the first ignored coefficient in our calculation. The Eqs. (\[Fgeor\]) and (\[Fgeot\]) then gives us an estimation of $1$ mm/s$^2$ for the magnitude of the component of the acceleration at perijove but this is only $10^{-3}$ mm/s$^2$ an hour before or after the perijove. So, a better modelling of the gravitational model of Jupiter is necessary for studying the orbit of Juno near the perigee but we cannot discard the anomaly because it persists even an hour after crossing the perigee 