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We carry out non-rotating high-resolution calculations of the solar globalconvection, which resolve convective scales of less than 10 Mm. To cope withthe low Mach number conditions in the lower convection zone, we use the reducedspeed of sound technique (RSST), which is simple to implement and requires onlylocal communication in the parallel computation. In addition, the RSST allowsus to expand the computational domain upward to about $0.99 R_{\odot}$ as itcan also handle compressible flows. Using this approach, we study the solarconvection zone on the global scale, including small-scale near-surfaceconvection. In particular, we investigate the influence of the top boundarycondition on the convective structure throughout the convection zone as well ason small-scale dynamo action. Our main conclusions are: 1. The small-scaledownflows generated in the near-surface layer penetrate into deeper layers tosome extent and excite small-scale turbulence in the region $>0.9R_\odot$,where $R_\odot$ is the solar radius. 2. In the deeper convection zone($<0.9R_\odot$), the convection is not influenced by the location of the upperboundary. 3. Using an LES approach, we can achieve small-scale dynamo actionand maintain a field of about $0.15-0.25 B_\mathrm{eq}$ throughout theconvection zone, where $B_\mathrm{eq}$ is the equipartition magnetic field tothe kinetic energy. 4. The overall dynamo efficiency varies significantly inthe convection zone as a consequence of the downward directed Poynting flux andthe depth variation of the intrinsic convective scales.

astrophysical journal/the astrophysical journal

High-resolution calculations of the solar global convection with the  reduced speed of sound technique: I. The structure of the convection and the  magnetic field without the rotation