  Despite the lack of a shear-rich tachocline region low-mass fully convective
stars are capable of generating strong magnetic fields, indicating that a
dynamo mechanism fundamentally different from the solar dynamo is at work in
these objects. We present a self-consistent three dimensional model of magnetic
field generation in low-mass fully convective stars. The model utilizes the
anelastic magnetohydrodynamic equations to simulate compressible convection in
a rotating sphere. A distributed dynamo working in the model spontaneously
produces a dipole-dominated surface magnetic field of the observed strength.
The interaction of this field with the turbulent convection in outer layers
shreds it, producing small-scale fields that carry most of the magnetic flux.
The Zeeman-Doppler-Imaging technique applied to synthetic spectropolarimetric
data based on our model recovers most of the large-scale field. Our model
simultaneously reproduces the morphology and magnitude of the large-scale field
as well as the magnitude of the small-scale field observed on low-mass fully
convective stars.
