  The main aim of this paper is to obtain analytic relativistic anisotropic
spherical solutions in f(R,$\mathcal{T}$) scenario. To do so we use modified
Durgapal-Fuloria metric potential and the isotropic condition is imposed in
order to obtain the effective anisotropic factor $\tilde{\Delta}$. Besides, a
notable and viable election on f(R,$\mathcal{T}$) gravity formulation is taken.
Specifically $f(R,\mathcal{T})=R+2\chi\mathcal{T}$, where $R$ is the Ricci
scalar, $\mathcal{T}$ the trace of the energy-momentum tensor and $\chi$ a
dimensionless parameter. This choice of $f(R,\mathcal{T})$ function modifies
the matter sector only, including new ingredients to the physical parameters
that characterize the model such as density, radial, and tangential pressure.
Moreover, other important quantities are affected such as subliminal speeds of
the pressure waves in both radial and transverse direction, observational
parameters, for example, the surface redshift which is related with the total
mass $M$ and the radius $r_{s}$ of the compact object. Also, a transcendent
mechanism like equilibrium through generalized Tolman-Oppenheimer-Volkoff
equation and stability of the system are upset. We analyze all the physical and
mathematical general requirements of the configuration taking $M=1.04
M_{\odot}$ and varying $\chi$ from $-0.1$ to $0.1$. It is shown by the
graphical procedure that $\chi<0$ yields to a more compact object in comparison
when $\chi\geq0$ (where $\chi=0.0$ corresponds to general relativity theory)
and increases the value of the surface redshift. However, negative values of
$\chi$ introduce in the system an attractive anisotropic force (inward) and the
configuration is completely unstable (corroborated employing Abreu's
criterion). Furthermore, the model in Einstein gravity theory presents cracking
while for $\chi>0$ the system is fully stable.
