High-activity stellar-wind mass-loss behavior

Determine the behavior of the stellar-wind mass-loss rate at the high-activity end of the empirical mass-loss-rate–coronal-X-ray-flux relation, including the origin of the putative wind divide.

Background

The paper discusses an empirical power-law relation between stellar-wind mass-loss rate and coronal X-ray flux for low-mass main-sequence stars. Observationally, this relation may break down at high activity levels, but the physical behavior of stellar winds in that regime is not established. The authors identify this possible wind divide as an unresolved issue that complicates comparisons between observations and global wind models.

References

First, the behaviour at the high-activity end remains an unsolved puzzle \citep[the putative ``wind divide'', e.g.,][]{Wood2021}.

— High-Resolution Modelling of Coronae and Winds in Solar-type Stars with Varying Rotation Rates II. Stellar Winds  (2609.28067 - Chen et al., 23 Sep 2026) in Section 1, Introduction