  The young and magnetically active K dwarf Epsilon Eridani exhibits a
chromospheric activity cycle of about 3 years. Previous reconstructions of its
large-scale magnetic field show strong variations at yearly epochs. To
understand how Epsilon Eridani's large-scale magnetic field geometry evolves
over its activity cycle we focus on high cadence observations spanning 5 months
at its activity minimum. Over this timespan we reconstruct 3 maps of Epsilon
Eridani's large-scale magnetic field using the tomographic technique of Zeeman
Doppler Imaging. The results show that at the minimum of its cycle, Epsilon
Eridani's large-scale field is more complex than the simple dipolar structure
of the Sun and 61 Cyg A at minimum. Additionally we observe a surprisingly
rapid regeneration of a strong axisymmetric toroidal field as Epsilon Eridani
emerges from its S-index activity minimum. Our results show that all stars do
not exhibit the same field geometry as the Sun and this will be an important
constraint for the dynamo models of active solar-type stars.
