A simulation of solar convection at supergranulation scale

Abstract

We present here numerical simulations of surface solar convection which cover a box of 30$\times 30\times$3.2 Mm${}^3$ with a resolution of 315$\times 315\times$82, which is used to investigate the dynamics of scales larger than granulation. No structure resembling supergranulation is present; possibly higher Reynolds numbers (i.e. higher numerical resolution), or magnetic fields, or greater depth are necessary. The results also show interesting aspects of granular dynamics which are briefly presented, like extensive p-mode ridges in the k-$\omega$ diagram and a ringlike distribution of horizontal vorticity around granules. At large scales, the horizontal velocity is much larger than the vertical velocity and the vertical motion is dominated by p-mode oscillations.

Contribution to the proceedings of the workshop entitled "THEMIS and the new frontiers of solar atmosphere dynamics" (March 2001), 6 pages, to appear in Nuovo Cimento C

Cited by in corpus (3)

• The Sun's Supergranulation
• The Impact of Stellar Surface Magnetoconvection and Oscillations on the Detection of Temperate, Earth-Mass Planets Around Sun-Like Stars
• Space-time segmentation method for study of the vertical structure and evolution of solar supergranulation from data provided by local helioseismology