  In this work, we investigated a most general isotropic charged fluid solution
for the Buchdahl model via a two-step method in $\mathscr{F}(Q)$-gravity
framework for the first time. In this context, a linear function of the form
$\mathscr{F}(Q)=\zeta_1 Q+\zeta_2$ and a particular transformation is used to
solve the Einstein-Maxwell Equations (EMEs) employing the Buchdahl ansatz: $
e^{\Upsilon(r)}=\frac{\mu(1+\lambda r^2)}{\mu+\lambda r^2}$, where $\zeta_1$,
$\zeta_2$, $\lambda$ and $\mu$ are constant parameters. The Schwarzschild de
Sitter~(AdS) exterior solution is joined to the interior solution at the
boundary to determine the constant parameters. It should be emphasized that,
for a given transformation, the Buchdahl ansatz only offers a mathematically
feasible solution in the context of electric charge, where pressure and density
are maximum at the center and decrease monotonically towards the boundary when
$0<\mu<1$. We taken into account the compact star EX01785-248 with $M=(1.3\pm
0.2)M_{\odot}$; Radius $=12.02^{+0.55}_{-0.55}$~km for graphical analysis. The
physical acceptability of the model in the context of $\mathscr{F}(Q)$ has been
evaluated by looking at the necessary physical properties, including energy
conditions, causality, hydrostatic equilibrium, pressure-density ratio, etc.
Additionally, we predicted the maximum mass limit of different compact objects
for various parameter values along with the mass-radius relation. The maximum
masses range (1.927 - 2.321)~$M_\odot$ are obtained for our solution. It can be
observed that when the coupling parameter $\zeta_1$ for $\mathscr{F}(Q)$
gravity is smaller, then our solution yields massive stars. The present
investigation provides novel insights and realistic implications regarding the
formation of compact astrophysical objects.
