Theoretical and Observational Evidence for Coriolis Effects in Coronal Magnetic Fields Via Direct Current Driven Flaring Events

TL;DR

This paper combines theoretical modeling and observational data to explore how Coriolis effects influence the distribution of stellar flare energies, suggesting faster rotation leads to shallower energy distributions.

Contribution

It introduces a topological model incorporating Coriolis effects to explain variations in stellar flare energy distributions based on rotation rates.

Findings

Coriolis effects produce shallower flare energy distributions in rapidly rotating stars.

Observational evidence supports the predicted correlation between stellar rotation and flare energy distribution slope.

The model links magnetic field braiding and reconnection to observed flare statistics.

Abstract

All stars produce explosive surface events such as flares and coronal mass ejections. These events are driven by the release of energy stored in coronal magnetic fields, generated by the stellar dynamo. However, it remains unclear if the energy deposition in the magnetic fields is driven by direct or alternating currents. Recently, we presented observational measurements of the flare intensity distributions for a sample of $\sim10^5$ stars across the main sequence observed by $\textit{TESS}$, all of which exhibited power-law distributions similar to those observed in the Sun, albeit with varying slopes. Here we investigate the mechanisms required to produce such a distribution of flaring events via direct current energy deposition, in which coronal magnetic fields braid, reconnect, and produce flares. We adopt a topological model for this process which produces a power-law distribution of energetic flaring events. We expand this model to include the Coriolis effect, which we demonstrate produces a shallower distribution of flare energies in stars that rotate more rapidly (corresponding to a weaker decline in occurrence rates toward increasing flare energies). We present tentative evidence for the predicted rotation-power-law index correlation in the observations. We advocate for future observations of stellar flares that would improve our measurements of the power-law exponents, and yield key insights into the underlying dynamo mechanisms that underpin the self-similar flare intensity distributions.