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Some of the small-scale solar magnetic flux can be attributed to asmall-scale dynamo (SSD) operating in the near-surface convection. The SSDfields have consequences for solar granular convection, basal flux, as well aschromospheric heating. A similar SSD mechanism is expected to be active in thenear-surface convection of other cool main-sequence stars, but this has neverbeen investigated. We aim to investigate changes in stratification andconvection due to inclusion of SSD fields for F3V, G2V, K0V and M0V spectraltypes in the near-surface convection. 3D magnetohydrodynamic (MHD) models ofthe four stellar boxes, covering the subsurface convection zone up to the lowerphotosphere in a small cartesian box, are studied using the \textit{MURaM}radiative-MHD simulation code. The SSD runs are compared against referencehydrodynamic runs. An SSD is found to efficiently produce magnetic field withenergies ranging between 5\% to 80\% of the plasma kinetic energy at differentdepths. This ratio tends to be larger for larger $T_{\mathrm{eff}}$. Therelative change in density and gas pressure stratification for the deeperconvective layers due to SSD magnetic fields is negligible, except for theF-star. For the F-star, there is a substantial reduction in convectivevelocities due to Lorentz force feedback from magnetic fields, which, in turn,reduces the turbulent pressure. SSD in near-surface convection for coolmain-sequence stars introduces small but significant changes in thermodynamicstratification (especially for the F-star) due to reduction in convectivevelocities.

Small-scale Dynamo in Cool Stars: I. Changes in stratification and near-surface convection for main-sequence spectral types