**FULL TITLE** ASP Conference Series, Vol. **VOLUME**, **YEAR OF PUBLICATION** **NAMES OF EDITORS** Are Convective Dynamos Responsible for the Minimum X-ray Fluxes Observed in the Sun and Late-Type Main Sequence Stars?

Abstract. We extend the investigation of Bercik et al. (2005) to the case of a non-rotating solar-type reference star. Using three-dimensional numerical simulations of a turbulent dynamo driven by convection and the empirical re-lationship of Pevtsov et al. (2003), we predict the level of X-ray emission from such a convective turbulent dynamo, and ¯nd that our results are consistent with quiet Sun observations. This implies that it is plausible that the Sun may have a rotation-independent convective dynamo working together with the large-scale dynamo believed to be responsible for the solar cycle. 1. Background The large-scale magnetic ¯eld on the Sun is believed to originate via a global-scale dynamo, the ®{ dynamo (Durney & Latour 1978), powered mainly by velocity shear due to di®erential rotation. It is often assumed that the amount of di®erential rotation is proportional to the rotation rate itself (e.g., RÄudiger 1989). This dynamo mechanism is also applied to other cool stars, based on the observed connection between rotation rate and magnetic activity (Skumanic