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We investigate whether pure deflagration models of Chandrasekhar-masscarbon-oxygen white dwarf stars can account for one or more subclass of theobserved population of Type Ia supernova (SN Ia) explosions. We compute a setof 3D full-star hydrodynamic explosion models, in which the deflagrationstrength is parametrized using the multispot ignition approach. For each model,we calculate detailed nucleosynthesis yields in a post-processing step with a384 nuclide nuclear network. We also compute synthetic observables with our 3DMonte Carlo radiative transfer code for comparison with observations. For weakand intermediate deflagration strengths (energy release E_nuc <~ 1.1 x 10^51erg), we find that the explosion leaves behind a bound remnant enriched with 3to 10 per cent (by mass) of deflagration ashes. However, we do not obtain thelarge kick velocities recently reported in the literature. We find that weakdeflagrations with E_nuc ~ 0.5 x 10^51 erg fit well both the light curves andspectra of 2002cx-like SNe Ia, and models with even lower explosion energiescould explain some of the fainter members of this subclass. By comparing oursynthetic observables with the properties of SNe Ia, we can exclude thebrightest, most vigorously ignited models as candidates for any observed classof SN Ia: their B - V colours deviate significantly from both normal and2002cx-like SNe Ia and they are too bright to be candidates for othersubclasses.

Three-dimensional pure deflagration models with nucleosynthesis and synthetic observables for Type Ia supernovae