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We report here results of spectropolarimetric observations of the classical TTauri star DN Tau carried out (at 2 epochs) with ESPaDOnS at theCanada-France-Hawaii Telescope within the `Magnetic Protostars and Planets'programme. We infer that DN Tau, with a photospheric temperature of 3,950+-50K, a luminosity of 0.8+-0.2 Lsun and a rotation period of 6.32 d, is a~2Myr-old fully-convective 0.65+-0.05 Msun star with a radius of 1.9+-0.2 Dsun,viewed at an inclination of 35+-10degr.  Clear circularly-polarized Zeeman signatures are detected in bothphotospheric and accretion-powered emission lines, probing longitudinal fieldsof up to 1.8 kG (in the He1 D3 accretion proxy). Rotational modulation ofZeeman signatures, detected both in photospheric and accretion lines, isdifferent between our 2 runs, providing further evidence that fields of cTTSsare generated by non-stationary dynamos.  Using tomographic imaging, we reconstruct maps of the large-scale field, ofthe photospheric brightness and of the accretion-powered emission at thesurface of DN Tau at both epochs. We find that the magnetic topology is mostlypoloidal, and largely axisymmetric, with an octupolar component (of polarstrength 0.6-0.8 kG) 1.5-2.0x larger than the dipolar component (of polarstrength 0.3-0.5 kG).  DN Tau features dominantly poleward accretion at both epochs. The large-scaledipole component of DN Tau is however too weak to disrupt the surroundingaccretion disc further than 65-90% of the corotation radius (at which the discKeplerian period matches the stellar rotation period), suggesting that DN Tauis already spinning up despite being fully convective.

Magnetospheric accretion on the fully-convective classical T Tauri star DN Tau