Fawzy, D. E.Cuntz, M.2023-06-162023-06-1620111432-07460004-6361https://doi.org/10.1051/0004-6361/201015250https://hdl.handle.net/20.500.14365/1524Aims. We compute the wave energy fluxes carried by longitudinal tube waves along vertically oriented thin magnetic fluxes tubes embedded in the atmospheres of theoretical main-sequence stars based on stellar parameters deduced by Kurucz and Gray. In addition, we present a fitting formula for the wave energy flux based on the governing stellar and magnetic parameters. Methods. A modified theory of turbulence generation based on the mixing-length concept is combined with the magnetohydrodynamic equations to numerically account for the wave energies generated at the base of magnetic flux tubes. Results. The results indicate a stiff dependence of the generated wave energy on the stellar and magnetic parameters in principal agreement with previous studies. The wave energy flux F-LTW decreases by about a factor of 1.7 between G0 V and K0 V stars, but drops by almost two orders of magnitude between K0 V and M0 V stars. In addition, the values for F-LTW are significantly higher for lower in-tube magnetic field strengths. Both results are consistent with the findings from previous studies. Conclusions. Our study complements existing descriptions of magnetic energy generation in late-type main-sequence stars. Our results will be helpful for calculating theoretical atmospheric models for stars of different levels of magnetic activity.eninfo:eu-repo/semantics/openAccessmethods: numericalmagnetohydrodynamics (MHD)stars: chromospherestars: magnetic fieldstars: solar-typewavesStellar Convection ZonesMagnetic-FluxEnergy FluxesChromosphere ModelsTimeGranulationSunPropagationEvolutionNetworkArticle10.1051/0004-6361/2010152502-s2.0-78650868292