et l’on trouvera d’abord
![{\displaystyle {\begin{alignedat}{2}r^{\scriptscriptstyle {\text{V}}}[r^{\scriptscriptstyle {\text{IV}}},r^{\scriptscriptstyle {\text{V}}}]_{0}=&0{,}581231\qquad \qquad &\log .\quad &9{,}7643490,\\r^{\scriptscriptstyle {\text{V}}}[r^{\scriptscriptstyle {\text{IV}}},r^{\scriptscriptstyle {\text{V}}}]_{1}=&0{,}324152&&9{,}5107483,\\r^{\scriptscriptstyle {\text{V}}}[r^{\scriptscriptstyle {\text{IV}}},r^{\scriptscriptstyle {\text{V}}}]_{2}=&0{,}131965&&9{,}1204599,\\r^{\scriptscriptstyle {\text{V}}}[r^{\scriptscriptstyle {\text{IV}}},r^{\scriptscriptstyle {\text{V}}}]_{3}=&0{,}059278&&8{,}7728965,\\r^{\scriptscriptstyle {\text{V}}}[r^{\scriptscriptstyle {\text{IV}}},r^{\scriptscriptstyle {\text{V}}}]_{4}=&0{,}027873&&8{,}4451930,\\\ldots \ldots \ldots \ldots &\ldots \ldots \ldots &&\ldots \ldots \ldots ,\end{alignedat}}}](https://wikimedia.org/api/rest_v1/media/math/render/svg/9eb38394788e075bb560f3cce7ed2ff9666066a1)
ensuite
![{\displaystyle {\begin{alignedat}{2}2r^{\scriptscriptstyle {\text{V2}}}{\frac {[r^{\scriptscriptstyle {\text{IV}}},r^{\scriptscriptstyle {\text{V}}}]_{0}}{r^{\scriptscriptstyle {\text{V}}}}}=&0{,}223454\qquad \qquad &\log .\quad &9{,}3491882,\\2r^{\scriptscriptstyle {\text{V2}}}{\frac {[r^{\scriptscriptstyle {\text{IV}}},r^{\scriptscriptstyle {\text{V}}}]_{1}}{r^{\scriptscriptstyle {\text{V}}}}}=&0{,}835079&&9{,}9217276,\\2r^{\scriptscriptstyle {\text{V2}}}{\frac {[r^{\scriptscriptstyle {\text{IV}}},r^{\scriptscriptstyle {\text{V}}}]_{2}}{r^{\scriptscriptstyle {\text{V}}}}}=&0{,}612944&&9{,}7874209,\\2r^{\scriptscriptstyle {\text{V2}}}{\frac {[r^{\scriptscriptstyle {\text{IV}}},r^{\scriptscriptstyle {\text{V}}}]_{3}}{r^{\scriptscriptstyle {\text{V}}}}}=&0{,}396095&&9{,}5977994,\\2r^{\scriptscriptstyle {\text{V2}}}{\frac {[r^{\scriptscriptstyle {\text{IV}}},r^{\scriptscriptstyle {\text{V}}}]_{4}}{r^{\scriptscriptstyle {\text{V}}}}}=&0{,}242776&&9{,}3851950,\\\ldots \ldots \ldots \ldots \ldots &\ldots \ldots \ldots &&\ldots \ldots \ldots ,\end{alignedat}}}](https://wikimedia.org/api/rest_v1/media/math/render/svg/ad88275cb5f83eb536526592cb0ad14955657fd0)
11. Or
donc la formule des variations dont il s’agit deviendra
![{\displaystyle {\begin{aligned}-\mathrm {T} ^{\scriptscriptstyle {\text{IV}}}&\left[+1{,}339359\sin(p^{\scriptscriptstyle {\text{V}}}-p^{\scriptscriptstyle {\text{IV}}})-2{,}706669\sin 2(p^{\scriptscriptstyle {\text{V}}}-p^{\scriptscriptstyle {\text{IV}}})\right.\\&\ \ \qquad \qquad \qquad \qquad \qquad \left.-0{,}237901\sin 3(p^{\scriptscriptstyle {\text{V}}}-p^{\scriptscriptstyle {\text{IV}}})-\ldots \right].\end{aligned}}}](https://wikimedia.org/api/rest_v1/media/math/render/svg/42bd8b403f8b1f7a1816828e8fc4b7776ad0acf1)
De sorte qu’en substituant pour 
masse de Vénus, sa valeur en secondes 
on aura
Correction de la longitude de Mercure due et l’action de Vénus et dépendante de la distance héliocentrique entre ces Planètes
