[en] We numerically and analytically work out the first-order post-Newtonian (1pN) orbital effects induced on the semimajor axis a, the eccentricity e, the inclination I, the longitude of the ascending node Ω, the longitude of perihelion ϖ, and the mean longitude at epoch ϵ of a test particle orbiting its primary, assumed static and spherically symmetric, by a distant massive third body X. For Mercury, the rates of change of the linear trends found are ${\stackrel{\dot{}<!--\; ??\; -->}{I}}_{1pN}^X$=-4.3 microarcseconds per century (μas cty${}^{-<!--\; ???\; -->1}$), ${\stackrel{\dot{}<!--\; ??\; -->}{\mathrm{\Omega <!--\; ??\; -->}}}_{1pN}^X$=18.2 μas cty${}^{-<!--\; ???\; -->1}$, ${\stackrel{\dot{}<!--\; ??\; -->}{\mathrm{\varpi <!--\; ??\; -->}}}_{1pN}^X$=30.4 μas cty${}^{-<!--\; ???\; -->1}$, ${\stackrel{\dot{}<!--\; ??\; -->}{\mathrm{ϵ<!--\; ??\; -->}}}_{1pN}^X$=271.4 μas cty${}^{-<!--\; ???\; -->1}$, respectively. Such values, which are due to the added actions of the other planets from Venus to Saturn, are essentially at the same level of, or larger by one order of magnitude than, the latest formal errors in the Hermean orbital precessions calculated with the EPM2017 ephemerides. The perihelion precession ${\stackrel{\dot{}<!--\; ??\; -->}{\mathrm{\varpi <!--\; ??\; -->}}}_{1pN}^X$ turns out to be smaller than some values recently appeared in the literature in view of a possible measurement with the ongoing BepiColombo mission. Linear combinations of the supplementary advances of the Keplerian orbital elements for several planets, if determined experimentally by the astronomers, could be set up in order to disentangle the 1pN N-body effects of interest from the competing larger precessions like those due to the Sun’s quadrupole moment J${}_2$ and angular momentum S.