Low-latitude magnetic flux emergence on rapidly rotating solar-type stars

TL;DR

This study investigates how magnetic flux tubes emerge at low latitudes on rapidly rotating solar-type stars, suggesting that intense magnetic fields and steeper temperature gradients enable flux emergence contrary to previous poleward deflection predictions.

Contribution

It proposes a model where strong magnetic fields and enhanced temperature gradients allow low-latitude flux emergence in rapidly rotating stars, resolving a discrepancy with earlier flux emergence models.

Findings

Flux emergence at 1-20 degrees latitude requires fields up to 500 kG.

Explosions of 100-kG tubes are compatible with the star's convection zone conditions.

Steeper temperature gradients are necessary for flux emergence in rapid rotators.

Abstract

Besides a dense coverage of their high latitudes by starspots, rapidly rotating cool stars also display low-latitude spots in Doppler images, although generally with a lower coverage. In contrast, flux emergence models of fast-rotating stars predict strong poleward deflection of radially rising magnetic flux as the Coriolis effect dominates over buoyancy, leaving a spot-free band around the equator. To resolve this discrepancy, we consider a flux tube near the base of the convection zone in a solar-type star rotating eight times faster than the Sun, assuming field intensification by weak-tube explosions. For the intensification to continue into to the buoyancy-dominated regime, the upper convection zone must have a significantly steeper temperature gradient than in the Sun, by a factor that is comparable with that found in 3D simulations of rotating convection. Within the hypothesis that stellar active regions stem from the base of the convection zone, flux emergence between 1-20 degree latitudes requires highly supercritical field strengths of up to 500 kG in rapidly rotating stars. These field strengths require explosions of 100-kG tubes within the convection zone, compatible with reasonable values of the superadiabatic temperature gradient associated with the more rapid rotation.