  Wood et al suggested that mass-loss rate is a function of X-ray flux
($\dot{M} \propto F_x^{1.34}$) for dwarf stars with $F_x \lesssim F_{x,6}
\equiv 10^6$ erg cm$^{-2}$ s$^{-1}$. However, more active stars do not obey
this relation. These authors suggested that the break at $F_{x,6}$ could be
caused by significant changes in magnetic field topology that would inhibit
stellar wind generation. Here, we investigate this hypothesis by analysing the
stars in Wood et al's sample that had their surface magnetic fields
reconstructed through Zeeman-Doppler Imaging (ZDI). Although the solar-like
outliers in the $\dot{M}$ -- $F_x$ relation have higher fractional toroidal
magnetic energy, we do not find evidence of a sharp transition in magnetic
topology at $F_{x,6}$. To confirm this, further wind measurements and ZDI
observations at both sides of the break are required. As active stars can jump
between states with highly toroidal to highly poloidal fields, we expect
significant scatter in magnetic field topology to exist for stars with $F_x
\gtrsim F_{x,6}$. This strengthens the importance of multi-epoch ZDI
observations. Finally, we show that there is a correlation between $F_x$ and
magnetic energy, which implies that $\dot{M}$ -- magnetic energy relation has
the same qualitative behaviour as the original $\dot{M}$ -- $F_x$ relation. No
break is seen in any of the $F_x$ -- magnetic energy
