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Vortex-flows exist across a broad range of spatial and temporal scales in thesolar atmosphere. Small-scale vortices have been proposed to play an importantrole in energy transport in the solar atmosphere. However, their physicalproperties remain poorly understood due to the limited spatial resolution ofthe observations. We aim to explore and analyze the physical properties ofsmall-scale vortices inside magnetic flux tubes using numerical simulations,and to investigate whether they contribute to heating the chromosphere in aplage region. Using the three-dimensional (3D) radiative magnetohydrodynamic(MHD) simulation code 'MURaM', we perform numerical simulations of a unipolarsolar plage region. To detect and isolate vortices, we use the SwirlingStrength criterion and select the locations where the fluid is rotating with anangular velocity greater than a certain threshold. We concentrate onsmall-scale as they are the strongest and carry most of the energy. We explorethe spatial profiles of physical quantities viz. density, horizontal velocity,etc. inside these vortices. Moreover, to apprehend their generalcharacteristics, a statistical investigation is performed. Magnetic flux tubeshave a complex filamentary substructure harbouring an abundance of small-scalevortices. At the interfaces between vortices strong current sheets are formedthat may dissipate and heat the solar chromosphere. Statistically, vorticeshave higher densities and higher temperatures than the average values at thesame geometrical height in the chromosphere. We conclude that small-scalevortices are ubiquitous in solar plage regions, and they are denser and hotterstructures that contribute to chromospheric heating, possibly by dissipation ofthe current sheets formed at their interfaces.

Vortex Flow Properties in Simulations of Solar Plage Region: Evidence for their role in chromospheric heating