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The solar atmosphere is filled with clusters of hot small-scale loopscommonly known as Coronal Bright Points (CBPs). These ubiquitous structuresstand 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 thesolar coronal heating puzzle. In addition, they can be the source of coronaljets and small-scale filament eruptions. Here we present a novel 3D numericalmodel using the Bifrost code that explains the sustained CBP heating forseveral hours. We find that stochastic photospheric convective motions alonesignificantly stress the CBP magnetic field topology, leading to importantJoule and viscous heating concentrated around the CBP's inner spine at a fewmegameters above the solar surface. We also detect continuous upflows withfaint EUV signal resembling observational dark coronal jets and small-scaleeruptions when H$_{\alpha}$ fibrils interact with the reconnection site. Wevalidate our model by comparing simultaneous CBP observations from SDO and SSTwith observable diagnostics calculated from the numerical results for EUVwavelengths as well as for the H$_{\alpha}$ line using the Multi3D synthesiscode. Additionally, we provide synthetic observables to be compared withHinode, Solar Orbiter, and IRIS. Our results constitute a step forward in theunderstanding of the many different facets of the solar coronal heatingproblem.

Deciphering the solar coronal heating: Energizing small-scale loops through surface convection