  We scrutinize the red dwarf component in the eclipsing binary system V471 Tau
in order to unravel relations between different activity layers from the
stellar surface through the chromosphere up to the corona. We aim at studying
how the magnetic dynamo in the late-type component is affected by the close
white dwarf companion. We use space photometry, high resolution spectroscopy
and X-ray observations from different space instruments to explore the main
characteristics of magnetic activity. From K2 photomery we find that 5-10 per
cent of the apparent surface of the red dwarf is covered by cool starspots.
From seasonal photometric period changes we estimate a weak differential
rotation. From the flare activity we derive a cumulative flare frequency
diagram which suggests that frequent flaring could have a significant role in
heating the corona. Using high resolution spectroscopy we reconstruct four
Doppler images for different epochs which reveal an active longitude, that is,
a permanent dominant spot facing the white dwarf. From short term changes in
the consecutive Doppler images we derive a weak solar-type surface differential
rotation with 0.0026 shear coefficient, similar to that provided by photometry.
The long-term evolution of X-ray luminosity reveals a possible activity cycle
length of 12.7 ys, traces of which were discovered also in the H$\alpha$
spectra. We conclude that the magnetic activity of the red dwarf component in
V471 Tau is strongly influenced by the close white dwarf companion. We confirm
the presence of a permanent dominant spot (active longitude) on the red dwarf
facing the white dwarf. The weak differential rotation of the red dwarf is very
likely the result of tidal confinement by the companion. We find that the
periodic appearance of the inter-binary H$\alpha$ emission from the vicinity of
the inner Lagrangian point is correlated with the activity cycle.
