  Solar spicules are plasma jets observed in the interface region between the
visible solar surface and the corona. At any given time, there are millions of
spicules present all over the Sun. While various models attempt to elucidate
their origin and characteristics, here, we consider the one driven by the
magneto-convection undulations. The radiative magneto-hydrodynamical (rMHD)
equations are solved using PENCIL CODE with a spatial resolution of 16 km using
various magnetic field strengths. The obtained rMHD simulation data are
investigated to unveil the various trends in spicular properties as function of
the applied magnetic fields. The important outcome of this study is the finding
of a consistent reduction in both the number density and the maximum height
reached by spicules as magnetic field strength increases. We also use parabolic
fitting on time-distance curves of spicules that are taller than
$75^\mathrm{th}$ percentile in the distribution, in order to find a relation
between deceleration of the spicule tip and the magnetic field strength. Our
results offer insights into the response of solar spicules to magnetic field
strength.
