  The solar atmosphere is filled with clusters of hot small-scale loops
commonly known as Coronal Bright Points (CBPs). These ubiquitous structures
stand out in the Sun by their strong X-ray and/or extreme-ultraviolet (EUV)
emission for hours to days, which makes them a crucial piece when solving the
solar coronal heating puzzle. In addition, they can be the source of coronal
jets and small-scale filament eruptions. Here we present a novel 3D numerical
model using the Bifrost code that explains the sustained CBP heating for
several hours. We find that stochastic photospheric convective motions alone
significantly stress the CBP magnetic field topology, leading to important
Joule and viscous heating concentrated around the CBP's inner spine at a few
megameters above the solar surface. We also detect continuous upflows with
faint EUV signal resembling observational dark coronal jets and small-scale
eruptions when H$_{\alpha}$ fibrils interact with the reconnection site. We
validate our model by comparing simultaneous CBP observations from SDO and SST
with observable diagnostics calculated from the numerical results for EUV
wavelengths as well as for the H$_{\alpha}$ line using the Multi3D synthesis
code. Additionally, we provide synthetic observables to be compared with
Hinode, Solar Orbiter, and IRIS. Our results constitute a step forward in the
understanding of the many different facets of the solar coronal heating
problem.
